{"title":"Shelyak Spectroscopes","description":"\u003cp\u003eShelyak Instruments is a French maker of astronomical spectroscopes used by amateurs, schools and pro-am observing campaigns. This collection covers the range: the compact Alpy 600 and Alpy 200, the modular UVEX, the high-resolution Lhires III and the LISA, plus calibration hardware for the eShel echelle spectrograph.\u003c\/p\u003e\u003cp\u003eSpare parts and upgrades include grating modules for the UVEX and Lhires III, slits and slit holders, guiding and calibration modules, fiber connector kits and a LISA near-infrared conversion kit.\u003c\/p\u003e","products":[{"product_id":"shelyak-alpy-600-spectroscope","title":"Shelyak Alpy 600 Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eResolution Power: R ~600\u003c\/li\u003e\n\u003cli\u003eFast F\/4 Optical Design\u003c\/li\u003e\n\u003cli\u003eWeight: 200g\u003c\/li\u003e\n\u003cli\u003eMulti-Position Interchangeable Slits: 25µm, 50µm, 100µm, 300µm\u003c\/li\u003e\n\u003cli\u003eMechanical Backfocus: 10.5-21mm\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eShelyak Alpy 600 Spectroscope\u003c\/h2\u003e\n      \u003cp\u003eThe Shelyak Alpy 600 Spectroscope packs a resolution power of R~600 into a compact body just 65mm long and weighing only 200g. Its fast F\/4 optical design and multi-position slit wheel, featuring a 25µm slit for ~1nm resolution, provide a versatile platform for scientific discovery. With a flexible mechanical backfocus range of 10.5-21mm, the Alpy 600 integrates easily into existing imaging trains to open the door to astrophysical analysis.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eR~600 Resolution: Capturing Stellar Spectra with 1nm Detail\u003c\/h3\u003e\n      \u003cp\u003eThe core of the Alpy 600 is a 600 lines\/mm grism (a combination grating and prism) that delivers a resolving power of R~600. When paired with the 25µm slit, you can achieve a spectral resolution of approximately 1nm across the visible spectrum. This level of detail is sufficient to clearly identify the spectral class of stars, observe prominent absorption and emission lines, and track the evolution of variable stars from one night to the next.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eMulti-Position Slit: 25µm to 300µm for Any Target\u003c\/h3\u003e\n      \u003cp\u003eA slit is what separates a spectroscope from a simple grating, and the Alpy 600 includes a multi-position wheel for maximum flexibility. The slit isolates your target from background skyglow and nearby stars, enabling high-contrast spectra and analysis of extended objects like nebulae and planets. This makes your data quality independent of seeing conditions or minor tracking errors.\u003c\/p\u003e\n      \u003cul\u003e\n        \u003cli\u003e\n\u003cstrong\u003e25µm \u0026amp; 50µm Slits:\u003c\/strong\u003e Use these for the highest resolution on bright stars to resolve fine spectral details.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003e100µm \u0026amp; 300µm Slits:\u003c\/strong\u003e Select these wider slits to allow more light through when targeting fainter objects like galaxies or nebulae, trading some resolution for stronger signal.\u003c\/li\u003e\n      \u003c\/ul\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n  \n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eFast F\/4 Optics in a Compact 200g Body\u003c\/h3\u003e\n      \u003cp\u003eEngineered for broad compatibility, the Alpy 600 features a fast F\/4 optical system that maximizes light throughput, allowing you to capture data on faint objects in minutes. Its remarkably low weight of 200g and compact 65mm x 45mm frame ensure it can be used with modest mounts and smaller telescopes down to 80mm in aperture without causing balance or stability issues.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eModular Integration: 10.5-21mm Backfocus and Optional Upgrades\u003c\/h3\u003e\n      \u003cp\u003eThe Alpy 600 connects to your camera via a standard M42x0.75mm T-mount thread and offers a versatile mechanical backfocus range of 10.5mm to 21mm, accommodating a wide variety of dedicated astronomy cameras. For a complete scientific workflow, the system is expandable with optional guiding and calibration modules. When fully configured with these modules, the required total backfocus is 64mm, a critical figure for planning your imaging train.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eAlpy 600 vs. Slitless Gratings: The Advantage of a Slit\u003c\/h3\u003e\n      \u003cp\u003eFor those starting in spectroscopy, a common choice is a simple slitless grating. While effective for basic stellar spectra, a slit-based instrument like the Alpy 600 represents a significant step up in scientific capability.\u003c\/p\u003e\n      \u003cul\u003e\n        \u003cli\u003e\n\u003cstrong\u003eSlitless Grating Advantage:\u003c\/strong\u003e They are simpler to use, as you don't need to precisely center a star on a narrow opening, and they have higher light throughput.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003eAlpy 600 Advantage:\u003c\/strong\u003e The slit isolates the target object, producing a clean, high-contrast spectrum free from contamination from nearby stars or background light pollution. This is essential for accurate wavelength calibration, studying extended objects, and producing data that is robust and independent of observing conditions.\u003c\/li\u003e\n      \u003c\/ul\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of scientific projects can I do with the Shelyak Alpy 600?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe Alpy 600's R~600 resolution opens the door to many projects. You can classify stars by their spectral type (O, B, A, F, G, K, M), detect the Doppler shift in binary star systems, measure the expansion of the universe by observing the redshift of quasars, or monitor the changing spectra of variable stars and comets.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I choose the right slit size (25µm, 50µm, 100µm, 300µm) for my target?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe choice is a trade-off between resolution and light throughput.\n    \u003c\/p\u003e\n\u003cul\u003e\n      \u003cli\u003eFor \u003cstrong\u003ebright stars\u003c\/strong\u003e where you want maximum detail, use the narrowest slits (\u003cstrong\u003e25µm or 50µm\u003c\/strong\u003e).\u003c\/li\u003e\n      \u003cli\u003eFor \u003cstrong\u003efaint, extended objects\u003c\/strong\u003e like nebulae or galaxies, use the wider slits (\u003cstrong\u003e100µm or 300µm\u003c\/strong\u003e) to capture more photons at the cost of lower resolution.\u003c\/li\u003e\n    \u003c\/ul\u003e\n    \n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use my DSLR with the Shelyak Alpy 600?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYes, you can use a DSLR. The Alpy 600 connects via a standard T-mount (M42x0.75mm), and you will need a T-ring for your specific camera model. However, for best results, a sensitive monochrome astronomy camera is recommended as it will capture faint spectral lines more efficiently than a color CMOS sensor.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the advantage of the Alpy 600's R~600 resolution for observing Be stars like Gamma Cassiopeiae?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eAn R~600 resolution is ideal for studying Be stars like Gamma Cassiopeiae (Navi). It allows you to clearly resolve the prominent Hydrogen-alpha emission line that characterizes these stars, which appears as a sharp spike \"filling in\" the normal absorption line. You can monitor the strength and shape of this emission line over time to track activity in the star's circumstellar disk.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Alpy 600 perform on a bright planet like Jupiter with an 8\" SCT?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe Alpy 600 is excellent for planetary spectroscopy with a telescope like an 8\" f\/10 SCT. You can orient the slit across Jupiter's disk to see the absorption bands of methane and ammonia in its atmosphere. By comparing the spectra of the belts and zones, you can detect differences in their chemical composition.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need the optional guiding and calibration modules for the Shelyak Alpy 600?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eWhile not strictly required to start, the optional modules significantly improve the workflow. The \u003cstrong\u003eguiding module\u003c\/strong\u003e lets you see the field of view to accurately place and keep your target on the narrow slit. The \u003cstrong\u003ecalibration module\u003c\/strong\u003e provides a reference lamp spectrum (Argon-Neon), which is essential for precise wavelength calibration, turning your data from a picture into a scientific measurement.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003ctable class=\"DAV-specifications\"\u003e\n    \u003ctbody\u003e\n      \u003ctr\u003e\n\u003ctd\u003eResolution Power\u003c\/td\u003e\n\u003ctd\u003eR ~600 (with 25µm slit)\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eSpectral Resolution\u003c\/td\u003e\n\u003ctd\u003e~1nm (with 25µm slit)\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eAperture\u003c\/td\u003e\n\u003ctd\u003eF\/4\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eSlit Options\u003c\/td\u003e\n\u003ctd\u003eMulti-position wheel with 25µm, 50µm, 100µm, 300µm slits (5µm tolerance); 25µm hole; 3mm hole\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eSlit Length\u003c\/td\u003e\n\u003ctd\u003e3mm\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e200g\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e65mm length, 45mm diameter\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eCamera Interface\u003c\/td\u003e\n\u003ctd\u003eT-mount thread (M42x0.75mm)\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eMechanical Backfocus\u003c\/td\u003e\n\u003ctd\u003e10.5mm to 21mm range\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eTotal Backfocus (with modules)\u003c\/td\u003e\n\u003ctd\u003e64mm\u003c\/td\u003e\n\u003c\/tr\u003e\n    \u003c\/tbody\u003e\n  \u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e \n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Backfocus_Diagram.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Backfocus Diagram\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":44968070545693,"sku":"SHK-PF0035","price":1349.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/products\/Shelyal-Alpy600-LowRes__29165.1671740990.1280.1280.jpg?v=1684348645"},{"product_id":"shelyak-alpy-guiding-module","title":"Shelyak Alpy Guiding Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eEssential guiding accessory for Alpy 600 \u0026amp; UVEX spectroscopes\u003c\/li\u003e\n\u003cli\u003eEnsures precise centering of the target star on the spectroscope slit\u003c\/li\u003e\n\u003cli\u003eUtilizes a reflective slit for off-axis guiding with a separate camera\u003c\/li\u003e\n\u003cli\u003eAdds 34mm of mechanical backfocus to the optical train\u003c\/li\u003e\n\u003cli\u003eLightweight 260g design minimizes impact on mount balance\u003c\/li\u003e\n\u003cli\u003eCompact 90x65x75mm body for easy integration\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Alpy Guiding Module\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Alpy Guiding Module solves the primary challenge of astronomical spectroscopy by adding only 260g and a compact 90x65x75mm profile to your imaging train. This essential accessory for the Alpy 600 and UVEX provides a critical 34mm of mechanical backfocus, using an innovative reflective slit to ensure your target star remains perfectly centered for accurate data acquisition.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eReflective Slit Guiding: Centering Your Star with the Alpy 600 \u0026amp; UVEX\u003c\/h3\u003e\n\u003cp\u003eWhen observing a star's spectrum, the target must be placed precisely on the spectroscope's slit and held there. The Alpy Guiding Module makes this possible by replacing the standard slit with a reflective, slightly inclined one. This surface reflects the entire telescope field of view to a separate guiding camera, allowing you to see both your target star and the slit simultaneously.\u003c\/p\u003e\n\u003cp\u003eThis system transforms pointing and guiding from a difficult guessing game into a straightforward, repeatable process. You can visually confirm the star is centered before an exposure and use autoguiding software to keep it locked in place for the duration of the observation. For any spectroscopic work lasting more than a few seconds, this module is an indispensable tool.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eOptical \u0026amp; Mechanical Integration: 34mm Backfocus in a 260g Package\u003c\/h3\u003e\n\u003cp\u003eDesigned for seamless integration, the Alpy Guiding Module is both compact and lightweight. At just 260g, it adds minimal load to your mount, preserving tracking accuracy and balance. Its 90x65x75mm dimensions ensure it fits easily into complex imaging trains without causing clearance issues.\u003c\/p\u003e\n\u003cp\u003eThe module introduces a fixed 34mm of mechanical backfocus, measured from the module's body to the reflective slit. This is a critical measurement for planning your optical train and ensuring you can achieve focus with both your guiding camera and the main spectroscope camera. This fixed, known distance simplifies the setup process for reliable, repeatable scientific measurements.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy is the Alpy Guiding Module essential for the Alpy 600 or UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWithout it, you have no way to visually confirm that your target star is on the spectroscope's slit. The \u003cstrong\u003eAlpy Guiding Module\u003c\/strong\u003e reflects the field of view to a guide camera, allowing you to see the star and the slit together. This is critical for both initial pointing and for autoguiding during long exposures to prevent the star from drifting off the slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Alpy Guiding Module's reflective slit work?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module contains a specially designed slit that is mirrored and slightly tilted. This surface allows a tiny fraction of the starlight to pass through to the spectroscope while reflecting the vast majority of the surrounding field of view at a 90-degree angle to a separate port. You connect a guiding camera to this port to see the field and guide the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the exact backfocus of the Alpy Guiding Module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe mechanical backfocus on the telescope side is \u003cstrong\u003e34mm\u003c\/strong\u003e. This is the precise distance from the main body of the guiding module to the surface of the reflective slit. You must account for this distance when calculating the spacing for your complete imaging train.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Alpy Guiding Module visually with an eyepiece?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWhile primarily designed for a guiding camera, visual use is possible with an optional eyepiece holder (sold separately). This allows you to look through an eyepiece to center the star on the slit manually. However, for any long-exposure work, a guiding camera is highly recommended for autoguiding.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Alpy Guiding Module help when taking a spectrum of Vega (Alpha Lyrae) with an 8\" SCT and a UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAn 8\" SCT has a long focal length, creating a very narrow field of view. Finding and centering a bright star like Vega on the invisible slit would be very difficult. With the \u003cstrong\u003eAlpy Guiding Module\u003c\/strong\u003e, you can use your guide camera to easily locate Vega in the field, place it perfectly on the slit, and then engage your mount's autoguiding to keep it there, ensuring all of the star's light enters the UVEX for a high-quality spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill the 260g weight of the Alpy Guiding Module affect my portable mount's balance?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAt only \u003cstrong\u003e260g\u003c\/strong\u003e (about half a pound), the module's weight is minimal. While you should always rebalance your telescope after adding any accessory, this small mass is unlikely to cause significant balance or tracking issues on most mounts capable of supporting a spectroscope and camera.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eMechanical Backfocus\u003c\/td\u003e\n\u003ctd\u003e34mm (from module body to slit)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e260g\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e90 x 65 x 75mm (without guiding camera)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Guiding Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Guiding_Module_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Guiding Module Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Autoguiding_Camera_Assembly_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Autoguiding Camera Assembly Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":44968070611229,"sku":"SHK-PF0036","price":1557.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/products\/PF0036-Alpy-guiding-module-T210x187_134__36715.1671741744.1280.1280.png?v=1684348649"},{"product_id":"shelyak-alpy-calibration-module","title":"Shelyak Alpy Calibration Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eArgon-Neon (Ar-Ne) calibration lamp for precise wavelength reference\u003c\/li\u003e\n\u003cli\u003eTungsten-halogen lamp for creating flat-field frames\u003c\/li\u003e\n\u003cli\u003eIntegrated dark frame mode with a servo-controlled shutter\u003c\/li\u003e\n\u003cli\u003eCompact dimensions of 100x95x30mm\u003c\/li\u003e\n\u003cli\u003eLightweight design at only 300g\u003c\/li\u003e\n\u003cli\u003eRemote control capability via 12V inputs\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Alpy Calibration Module\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Alpy Calibration Module automates essential reference frames for the Alpy 600 and UVEX spectrographs, integrating Argon-Neon and halogen lamps into a compact 100x95x30mm unit. Weighing just 300g, this module allows you to acquire wavelength calibration, flat-field, and dark frames remotely without altering your telescope setup, dramatically increasing observational productivity.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eDual Lamps for Full Calibration: Argon-Neon (Ar-Ne) and Halogen\u003c\/h3\u003e\n\u003cp\u003eAccurate spectroscopy requires two fundamental reference frames. The Alpy Calibration Module includes an Argon-Neon (Ar-Ne) lamp which produces a spectrum with numerous, well-defined emission lines at known wavelengths. This allows you to precisely calibrate the wavelength scale of your scientific spectra. For correcting pixel-to-pixel sensitivity variations and removing dust motes, the module incorporates a halogen lamp that provides a smooth, continuous spectrum for creating high-quality flat-field images.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e3-in-1 Automated Workflow: Servo Control for Calibration, Flats, and Darks\u003c\/h3\u003e\n\u003cp\u003eThis module streamlines your entire calibration sequence. A servo-motor controls a small screen that moves into the telescope's light path on command. Activating one of the lamps illuminates the spectrograph's slit under conditions that mimic the telescope's beam. For dark frames, you can simply leave the lamps off and move the screen into place, effectively blocking all light from the telescope without needing to cap it manually. This three-mode system—calibration, flat, and dark—makes acquiring a complete set of reference images a simple, repeatable process.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eRemote Operation: Dual 12V Inputs for Unattended Spectrography\u003c\/h3\u003e\n\u003cp\u003eDesigned for modern, automated observatories, the Alpy Calibration Module can be fully controlled without physical intervention. In addition to manual switches, two separate connectors accept a 12V signal to activate the Ar-Ne and halogen lamps independently. This allows you to integrate the calibration process directly into your imaging software's automation scripts, enabling a complete, unattended observing session from start to finish. The module requires a 12V DC power supply capable of at least 1A.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the two different lamps in the Shelyak Alpy Calibration Module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module contains two lamps for two distinct calibration tasks. The \u003cstrong\u003eArgon-Neon (Ar-Ne) lamp\u003c\/strong\u003e produces sharp emission lines at known wavelengths, which are used to accurately calibrate the wavelength scale of your spectrum. The \u003cstrong\u003ehalogen lamp\u003c\/strong\u003e produces a continuous, uniform light source used to create flat-field frames, which correct for pixel sensitivity variations and dust on the sensor.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Alpy Calibration Module create dark frames without a separate shutter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module uses its internal servo-controlled screen. When you activate the \"Dark\" mode, the screen moves into the telescope's light path, completely blocking incoming light from the sky. With both internal lamps switched off, this allows the spectrograph to capture a dark frame under the same conditions as your light frames, without you needing to manually cap the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I control the Shelyak Alpy Calibration Module from my computer?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The module is designed for remote operation. It features two 12V trigger inputs that allow you to switch each lamp on and off using a relay box or similar device controlled by your PC. This enables you to integrate the calibration process into automated imaging sequences in software like PRISM or MaxIm DL.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI'm measuring the radial velocity of the star Arcturus (Alpha Boötis) with my UVEX spectrograph. How does this module improve my accuracy?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor precise radial velocity measurements, a stable and immediate wavelength calibration is critical. The Alpy Calibration Module allows you to take an Argon-Neon calibration spectrum immediately before or after your spectrum of Arcturus without touching the instrument. This minimizes errors from instrument flexure or temperature changes, ensuring your wavelength solution is as accurate as possible for measuring the Doppler shift in the star's spectral lines.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eMy observatory is remote. How does the Alpy Calibration Module fit into an automated imaging sequence with an Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module is ideal for remote observatories. Using its 12V inputs, you can script the entire calibration process. A typical automated sequence would be:\n\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eEnd of Night:\u003c\/strong\u003e Telescope slews to a park position.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eDark Frames:\u003c\/strong\u003e Script sends a 12V signal to move the module's screen into place (lamps off) to take darks.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eFlat Frames:\u003c\/strong\u003e Script activates the halogen lamp for a series of flat-field exposures.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eCalibration Frames:\u003c\/strong\u003e Script activates the Argon-Neon lamp for wavelength calibration exposures.\u003c\/li\u003e\n\u003c\/ul\u003e\nThis allows for fully unattended, repeatable data acquisition and calibration.\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat power supply do I need for the Shelyak Alpy Calibration Module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou will need an external power supply that can provide at least \u003cstrong\u003e12V DC at 1A\u003c\/strong\u003e. The power connector type is a standard center-positive barrel plug. This is a common power supply type for many astronomy accessories.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e300g\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e100 x 95 x 30 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Lamp\u003c\/td\u003e\n\u003ctd\u003eArgon-Neon (Ar-Ne)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eFlat-Field Lamp\u003c\/td\u003e\n\u003ctd\u003eHalogen\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDark Frame Function\u003c\/td\u003e\n\u003ctd\u003eYes (via internal servo-controlled mask)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRemote Control\u003c\/td\u003e\n\u003ctd\u003e2x 12V inputs\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003ePower Requirement\u003c\/td\u003e\n\u003ctd\u003e12V DC, 1A (minimum)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy 600, Shelyak UVEX\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Calibration Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Calibration_Module_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Calibration Module Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":44968070643997,"sku":"SHK-PF0037","price":1279.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/products\/PF0037-Alpy-guiding-module-T198x210_135_w__55288.1671741838.1280.1280.png?v=1684348651"},{"product_id":"shelyak-ba0001","title":"Shelyak Lhires III 2-inch adapter","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eAdapts Lhires III Spectroscope to 2-inch focusers\u003c\/li\u003e\n\u003cli\u003eProvides a secure, non-flexing connection\u003c\/li\u003e\n\u003cli\u003eEnables use with a wider range of telescopes\u003c\/li\u003e\n\u003cli\u003eMachined for precise optical alignment\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eLhires III 2-inch adapter\u003c\/h2\u003e\n      \u003cp\u003eThe Lhires III 2-inch adapter provides a robust and secure mechanical link between your Shelyak Lhires III spectroscope and any standard 2-inch telescope focuser. This simple but essential component ensures precise optical alignment and rigidity, preventing flexure that can compromise spectroscopic data. It allows you to mount your Lhires III on larger telescopes that are typically equipped with 2-inch focusers, expanding your instrument's compatibility.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eSecure Mounting for the Lhires III in 2-inch Focusers\u003c\/h3\u003e\n      \u003cp\u003eThis adapter is the standard solution for connecting the Lhires III spectroscope, which typically uses smaller threaded connections, to the larger 2-inch format common on Schmidt-Cassegrains, Ritchey-Chrétiens, and larger refractors. By converting the input of the spectroscope to a simple 2-inch barrel, you gain a solid, stable platform for your scientific work, ensuring the entire optical train remains perfectly collimated through long exposures.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the Lhires III 2-inch adapter?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThis adapter allows you to mount your \u003cstrong\u003eShelyak Lhires III spectroscope\u003c\/strong\u003e into a standard \u003cstrong\u003e2-inch telescope focuser\u003c\/strong\u003e. It provides a secure, rigid connection, ensuring correct optical alignment for accurate data acquisition.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need this adapter for my Lhires III?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYou need this adapter if your telescope has a 2-inch focuser and you do not have another way to adapt the Lhires III's native mounting thread to it. It is the most direct and stable method for using the spectroscope with larger amateur telescopes.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Lhires III 2-inch adapter attach?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe adapter threads directly onto the input side of the Lhires III spectroscope body. The other end is a smooth 2-inch barrel that slides into your telescope's focuser and is secured by the focuser's compression ring or set screws, just like a standard 2-inch eyepiece.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943026290973,"sku":"SHK-BA0001","price":131.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Lhires-III-2-inch-adapter-1_ab4109a8-edcb-4498-9cab-1b087d5b3f84.jpg?v=1789615786"},{"product_id":"shelyak-es0002","title":"Shelyak Lhires III Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eHigh-Resolution Spectroscopic Analysis\u003c\/li\u003e\n\u003cli\u003eOptimized for Schmidt-Cassegrain Telescopes\u003c\/li\u003e\n\u003cli\u003eIntegrated C-Mount Guide Port (0.8x)\u003c\/li\u003e\n\u003cli\u003eMirror Slit for Precise Target Acquisition\u003c\/li\u003e\n\u003cli\u003eCompact and Lightweight at 1.7 kg\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLhires III Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Lhires III Spectroscope packages high-resolution optics into a compact 250 mm x 200 mm x 83 mm chassis weighing just 1.7 kg. Its integrated C-mount guide port features a 0.8x focal reducer and provides a mechanical backfocus of 17.5 mm for a guide camera, enabling precise tracking for detailed stellar analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eGuiding \u0026amp; Slit Design: 0.8x C-Mount Port and 17.5mm Back Focus\u003c\/h3\u003e\n\u003cp\u003eThe Lhires III incorporates a mirror slit, allowing you to view the field around your target for precise centering and guiding. This is critical for high-resolution work where the star must be held perfectly on the narrow slit for the duration of the exposure. To maintain this alignment, an integrated C-mount guide port with a 0.8x focal reducer and 17.5 mm of mechanical backfocus allows you to connect a separate guide camera (not included) for active autoguiding.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003ePhysical Build: A Compact 1.7 kg, 250mm x 200mm x 83mm Chassis\u003c\/h3\u003e\n\u003cp\u003eEngineered for stability and compatibility, the Lhires III weighs only 1.7 kg, making it a manageable payload for a wide range of equatorial mounts. Its 250 mm x 200 mm x 83 mm dimensions ensure it fits within typical imaging train clearances. The instrument is particularly well-suited for Schmidt-Cassegrain telescopes but can be adapted to faster optical systems with the addition of a Barlow lens to achieve the optimal focal ratio.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eHigh-Resolution Science: Doppler Shift Analysis \u0026amp; Pro-Am Collaboration\u003c\/h3\u003e\n\u003cp\u003eThis spectroscope is designed specifically for isolating and analyzing the fine details within individual spectral lines. While this high-resolution focus means the observable spectral range is narrow at any one time, a micrometer adjustment lets you select any wavelength in the visible spectrum. This capability makes the Lhires III an ideal tool for advanced projects, including measuring the Doppler effect to study stellar activity or observing the rotation of planets like Jupiter and Saturn.\u003c\/p\u003e\n\u003cp\u003eThe Lhires III is a proven instrument for scientific collaboration between amateur and professional astronomers. It has been used in numerous published studies on Be-type stars, variable stars, and other dynamic celestial objects, making it a gateway to contributing to real astrophysical research.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of telescope works best with the Lhires III Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Lhires III is optimized for an f\/10 focal ratio, making it an excellent match for Schmidt-Cassegrain (SCT) and Maksutov-Cassegrain telescopes. It can be adapted to faster instruments, such as f\/5 Newtonians or refractors, by placing a Barlow lens in the optical path before the spectroscope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Lhires III Spectroscope to measure the rotation of Jupiter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. By orienting the slit along Jupiter's equator, you can capture the spectrum from both the approaching and receding limbs of the planet simultaneously. The resulting tilt in the spectral lines is a direct measurement of the Doppler shift caused by the planet's rotation, a classic educational and scientific project well within the Lhires III's capabilities.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat do I need to start autoguiding with the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou will need a separate C-mount guide camera and autoguiding software. The Lhires III has a built-in guide port with a \u003cstrong\u003e0.8x focal reducer\u003c\/strong\u003e and \u003cstrong\u003e17.5 mm of backfocus\u003c\/strong\u003e. The mirror slit reflects the field of view to this port, allowing the guide camera to monitor the target star and send corrections to your telescope mount.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I attach my imaging camera to the Lhires III Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Lhires III comes with a standard adapter for ATIK cameras, which have a 13mm mechanical backfocus. Shelyak offers a wide range of optional adapter rings to connect other CCD, CMOS, or DSLR cameras with different backfocus requirements.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the Lhires III a good tool for studying Be stars?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAbsolutely. The Lhires III was originally designed in collaboration with the CNRS Astrophysics School specifically for the observation of Be stars. Its high-resolution capabilities are perfect for monitoring the complex emission line profiles (like Hydrogen-alpha) that characterize these rapidly rotating stars, making it a key instrument for pro-am campaigns.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I select a specific wavelength to observe with the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Lhires III uses a micrometer adjustment to rotate the grating inside the instrument. This allows you to precisely center any wavelength within the visible spectrum (from approximately 400nm to 750nm) onto your camera's sensor, giving you the flexibility to study specific spectral features like the Sodium D lines or H-alpha.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGuide Port Specifications\u003c\/td\u003e\n\u003ctd\u003eDual-lens C-mount with 0.8x focal reducer\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eGuide Camera Back Focus\u003c\/td\u003e\n\u003ctd\u003e17.5 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e1.7 kg\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e250 mm x 200 mm x 83 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDetector Compatibility\u003c\/td\u003e\n\u003ctd\u003eAccepts adaptor rings for CCD, CMOS, and DSLR cameras\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_User_Guide_Add-on_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III User Guide Add-on Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Plus_Update_Kit_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Plus Update Kit Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943030223133,"sku":"SHK-ES0002","price":7395.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Lhires-III-Spectroscope-1_23194ae6-2407-4edb-9048-0f5ef1136ff2.jpg?v=1789615906"},{"product_id":"shelyak-es0006","title":"Shelyak eShel III Complete System","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eProfessional echelle spectrograph system\u003c\/li\u003e\n\u003cli\u003eResolving power of R \u0026gt; 10,000\u003c\/li\u003e\n\u003cli\u003eCovers 390nm to 700nm spectral range\u003c\/li\u003e\n\u003cli\u003eFiber-optic fed for maximum stability\u003c\/li\u003e\n\u003cli\u003eIncludes FIGU, calibration module, and fibers\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak eShel III Complete System\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak eShel III is a complete, professional-level fiber-optic echelle spectrograph system, delivering a resolving power of R \u0026gt; 10,000 across a wide 390nm to 700nm spectral range. It achieves this by capturing diffraction orders 32 through 53 simultaneously, using a 50µm fiber for the target and a 200µm fiber for calibration to ensure maximum stability for demanding applications like exoplanet radial velocity studies.\u003c\/p\u003e\n\u003cp\u003eThis instrument is designed for observers who cannot compromise between spectral range and resolution. Developed from experience with professional spectroscopes like Musicos and Narval, the eShel III provides a turnkey solution for advanced astrophysical research. Please note, this system is available by quote only.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eR\u0026gt;10,000 Resolution Across the Visible Spectrum (390-700nm)\u003c\/h3\u003e\n\u003cp\u003eThe core of the eShel III is an echelle grating that uses over 30 diffraction orders to achieve high resolution. A cross-disperser then stacks these orders across the camera sensor, allowing you to capture the entire visible spectrum from 390nm to 700nm in a single exposure. This multi-order spectrum provides comprehensive data, ideal for monitoring variable stars or classifying stellar objects without sacrificing detail.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThermally Stable Radial Velocity with a Fiber-Fed Design\u003c\/h3\u003e\n\u003cp\u003ePrecision in spectroscopy, especially for exoplanet detection, requires extreme stability. The eShel III uses a 20-meter-long optical fiber to physically separate the spectrograph from the telescope, allowing the instrument to be placed in a temperature-controlled environment. This isolation from thermal fluctuations and mechanical vibrations at the telescope is critical for accurate radial velocity measurements.\u003c\/p\u003e\n\u003cp\u003eThe complete system includes the F\/6 Fiber Injection and Guiding Unit (FIGU) for precise starlight injection into the 50µm object fiber, and a dedicated calibration module with a Thorium-Argon (ThAr) lamp. The calibration spectrum is fed through a separate 200µm fiber, providing a stable reference for sub-pixel velocity measurements.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eIntegrated Control: Remote Acquisition and Data Reduction Software\u003c\/h3\u003e\n\u003cp\u003eThe eShel III system includes Demetra, a powerful and free software suite for MS Windows that manages the entire observation workflow. From the control room, you can remotely operate the FIGU and the calibration module, automate image acquisition, and process the complex echelle spectra. The software handles the extraction and calibration of the multiple orders, converting raw images into scientifically useful data, streamlining what would otherwise be a complex data reduction process.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary advantage of the eShel III's echelle design?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe echelle design solves the classic trade-off in spectroscopy. It delivers both \u003cstrong\u003ehigh resolution (R \u0026gt; 10,000)\u003c\/strong\u003e and a \u003cstrong\u003ewide spectral range (390-700nm)\u003c\/strong\u003e simultaneously. This is impossible with a traditional single-order spectrograph, making the eShel III ideal for comprehensive studies of stellar atmospheres, variable stars, and exoplanet transits.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy does the eShel III system use optical fibers?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe optical fibers are crucial for achieving the high stability required for precise radial velocity measurements. By physically separating the spectrograph from the telescope with a \u003cstrong\u003e20-meter fiber\u003c\/strong\u003e, the instrument can be kept in a thermally stable room, isolated from temperature changes and vibrations that would otherwise compromise the data. This is a standard technique in professional observatories.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat components are included in the eShel III complete system?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe eShel III is sold as a complete, integrated solution. The package includes:\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003eThe eShel spectroscope main module\u003c\/li\u003e\n\u003cli\u003eThe F\/6 Fiber Injection \u0026amp; Guiding Unit (FIGU)\u003c\/li\u003e\n\u003cli\u003eThe calibration module with a Thorium-Argon (ThAr) lamp\u003c\/li\u003e\n\u003cli\u003eA 20m, 50µm optical fiber for the target star\u003c\/li\u003e\n\u003cli\u003eA 20m, 200µm optical fiber for the calibration lamp\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cp\u003eYou will need to provide a suitable astronomical camera and telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of camera do I need for the eShel III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe eShel III does not include a camera. The choice of camera depends on your research goals, but it requires a sensor large enough to capture the full array of stacked spectral orders. A camera like the \u003cstrong\u003eATIK 460EX Monochrome\u003c\/strong\u003e is often recommended, as its sensor size and pixel characteristics are well-matched to the instrument's output when used in 2x2 binning mode.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow would I use the eShel III to study the radial velocity of a star like 51 Pegasi?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eTo measure the subtle Doppler shift caused by an exoplanet, you would use the fiber-fed system to ensure thermal stability. You would acquire a long series of spectra of 51 Pegasi, taking a calibration spectrum with the internal \u003cstrong\u003eThAr lamp\u003c\/strong\u003e before and after each observation. The \u003cstrong\u003eR \u0026gt; 10,000 resolution\u003c\/strong\u003e is high enough to detect the small wavelength shifts, and the Demetra software would be used to precisely measure these shifts against the stable ThAr reference lines, revealing the gravitational \"wobble\" induced by its planet.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan the eShel III capture the spectrum of a pulsating star like BW Vulpeculae in a single exposure?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an ideal application for the eShel III. Its ability to capture the entire \u003cstrong\u003e390-700nm spectrum\u003c\/strong\u003e at high resolution in one shot allows you to monitor changes in spectral lines across the star's atmosphere simultaneously. For a rapidly pulsating star like BW Vulpeculae, taking a series of 5-minute exposures would allow you to build a time-series dataset to analyze the atmospheric dynamics throughout its pulsation cycle.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eInstrument Type\u003c\/td\u003e\n\u003ctd\u003eMulti-order Echelle Spectrograph\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolving Power\u003c\/td\u003e\n\u003ctd\u003eR \u0026gt; 10,000\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Range\u003c\/td\u003e\n\u003ctd\u003e390 nm - 700 nm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDiffraction Orders\u003c\/td\u003e\n\u003ctd\u003e32 to 53\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eInput Connection\u003c\/td\u003e\n\u003ctd\u003eFiber-optic (FC\/PC connector)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eObject Fiber\u003c\/td\u003e\n\u003ctd\u003e50µm diameter, 20m length\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Fiber\u003c\/td\u003e\n\u003ctd\u003e200µm diameter, 20m length\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eIncluded Modules\u003c\/td\u003e\n\u003ctd\u003eF\/6 Fiber Injection \u0026amp; Guiding Unit (FIGU), Calibration Module\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Source\u003c\/td\u003e\n\u003ctd\u003eThorium-Argon (ThAr) Lamp\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eControl Software\u003c\/td\u003e\n\u003ctd\u003eDemetra (MS Windows)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eeShel Spectroscope Main Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eF\/6 Fiber Injection \u0026amp; Guiding Unit (FIGU)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eCalibration Module with ThAr Lamp\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e50µm Target Optical Fiber\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1 (20m length)\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e200µm Calibration Optical Fiber\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1 (20m length)\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Installation_and_Maintenance_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Installation and Maintenance Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Calibration_Power_Supply_Addendum_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Calibration Power Supply Addendum Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_eShel_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra eShel Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943030452509,"sku":"SHK-ES0006","price":31049.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-eShel-III-complete-system-1_1cb6e98a-9887-4619-8862-7a6e9cc69114.jpg?v=1789615915"},{"product_id":"shelyak-es0021","title":"Shelyak UVEX Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eWide spectral range from 350 nm (UV) to 1 µm (IR)\u003c\/li\u003e\n\u003cli\u003eMulti-position slit with 25µm, 50µm, 100µm, and 300µm options\u003c\/li\u003e\n\u003cli\u003eOptimized for F\/8 telescopes\u003c\/li\u003e\n\u003cli\u003eLightweight 1.2 kg body (without camera)\u003c\/li\u003e\n\u003cli\u003eIncludes a 600 lines\/mm grating blazed at 500nm\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eUVEX Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak UVEX Spectroscope is a highly versatile instrument built on an achromatic, crossed Czerny-Turner design, enabling scientific analysis across a vast spectral range from 350 nm in the ultraviolet to 1µm in the near-infrared. Its multi-position slit offers six apertures, from a high-resolution 25µm slit to a wide 3mm hole for easy targeting. Weighing only 1.2 kg (without a camera), the UVEX is engineered for seamless integration with telescopes operating at an optimal F\/8 ratio.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCrossed Czerny-Turner Optics: 350nm to 1µm Spectral Range\u003c\/h3\u003e\n\u003cp\u003eThe UVEX is designed as a \"crossed\" Czerny-Turner spectroscope, an optical configuration optimized for a flat field and high image quality across its entire operational range. This achromatic design ensures that it can capture spectra from the near-ultraviolet at 350 nm to the near-infrared at 1 µm, pushing the limits of what modern CMOS and CCD sensors can detect. This allows you to analyze a wide variety of stellar types and emission phenomena, from the Balmer series in hot stars to the infrared signatures of cooler objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e6-Position Slit and Interchangeable 600 tr\/mm Grating\u003c\/h3\u003e\n\u003cp\u003eControl over spectral resolution is critical, and the UVEX provides this through two key mechanisms. It includes a 6-position slit wheel, easily changed with an included screwdriver, offering 25µm, 50µm, 100µm, and 300µm slits, plus a 25µm pinhole and a 3mm hole for target acquisition. A narrower slit yields higher resolution at the cost of light throughput, giving you the flexibility to adapt to your target's brightness. The spectroscope comes standard with a 600 lines\/mm grating, and a vernier scale allows for precise positioning of the grating to center your desired wavelength on the sensor.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eF\/8 Optimization and Precise M2 Mirror Focusing\u003c\/h3\u003e\n\u003cp\u003eThe UVEX is ideally matched to telescopes with an F\/8 focal ratio, such as Ritchey-Chretien (RC) systems up to 400mm in diameter. While it can be used on systems as fast as F\/5 without vignetting, this comes with a slight degradation in image quality at the edges of the field. Focusing is managed by a precise, multi-turn knob that adjusts the internal M2 mirror, allowing you to achieve a sharp spectrum on your camera sensor without altering your telescope's main focuser.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eOptional Motorization and Included 3.2 kg Padded Case\u003c\/h3\u003e\n\u003cp\u003eDesigned for both field and observatory use, the UVEX can be upgraded with an optional motorization module for fully remote operation. For transport and storage, the instrument ships in a shockproof case with custom-cut foam, bringing the total weight to 3.2 kg. This case has dedicated slots for the spectrograph, a camera, and accessories like additional gratings or filters, ensuring your entire spectroscopy kit remains protected.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat type of telescope is best for the UVEX Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe UVEX is optimized for an \u003cstrong\u003eF\/8 focal ratio\u003c\/strong\u003e, making it an excellent match for Ritchey-Chretien (RC), Schmidt-Cassegrain (SCT), or other catadioptric telescopes. It can be used on scopes as fast as F\/5, but with a minor loss of resolution at the field edges.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I change the spectral resolution with the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou can adjust the resolution in two ways. First, by selecting a different slit width on the \u003cstrong\u003e6-position slit wheel\u003c\/strong\u003e; a narrower slit like the 25µm provides higher resolution. Second, by swapping out the included 600 tr\/mm grating for an optional one with a different line density.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan the UVEX Spectroscope capture the spectrum of a star like Vega (Alpha Lyrae) in the UV?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The UVEX has a spectral range extending down to \u003cstrong\u003e350 nm\u003c\/strong\u003e, which is well into the near-ultraviolet. This makes it ideal for studying the prominent Balmer absorption lines in the spectra of hot, A-type stars like Vega.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat camera do you recommend for the UVEX Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eShelyak recommends the \u003cstrong\u003eZWO ASI533MM Pro\u003c\/strong\u003e monochrome camera for use with the UVEX. The spectroscope is supplied with an adapter ring for ZWO cameras, and adapters for QHY and ATIK cameras are available separately.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the UVEX difficult to focus?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, focusing is straightforward. The UVEX features a dedicated \u003cstrong\u003emulti-turn knob\u003c\/strong\u003e that adjusts the internal M2 collimating mirror. This allows you to achieve a sharp focus for the spectrum on your camera's sensor independently of the main telescope focuser.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I operate the UVEX Spectroscope from a remote observatory?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The UVEX is designed to be compatible with an \u003cstrong\u003eoptional motorization module\u003c\/strong\u003e. When installed, this allows for remote control of the grating angle and other functions, making it suitable for automated or remote observatories.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Range\u003c\/td\u003e\n\u003ctd\u003e350 nm to 1µm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Options\u003c\/td\u003e\n\u003ctd\u003eMulti-position: 25µm, 50µm, 100µm, 300µm, 25µm hole, 3mm hole\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eOptimal Telescope F\/D\u003c\/td\u003e\n\u003ctd\u003eF\/8 (usable to F\/5 with minor quality degradation)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e145 x 140 x 120 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight (Spectroscope only)\u003c\/td\u003e\n\u003ctd\u003e1.2 kg\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight (with carrying case)\u003c\/td\u003e\n\u003ctd\u003e3.2 kg\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eUVEX Spectroscope\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShockproof Carrying Case\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e600 tr\/mm Grating\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1 (installed)\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eZWO Camera Adapter Ring\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003ePhillips Screwdriver\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003ePlastic Vernier for 600 gr\/mm Grating\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eBag of Spare Screws\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eAutoguiding Module Screws\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 4\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e \n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943031795997,"sku":"SHK-ES0021","price":7814.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-UVEX-Spectroscope-1_c215e6c3-6f26-4c18-9eed-3ea279d077a9.jpg?v=1789615956"},{"product_id":"shelyak-es0034","title":"Shelyak UVEX Motorized Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eFull remote control of grating, focus, and calibration\u003c\/li\u003e\n\u003cli\u003eAchromatic design covers a 350 nm to 1µm spectral range\u003c\/li\u003e\n\u003cli\u003e5-position slit module includes 25µm, 50µm, 100µm, and 300µm slits\u003c\/li\u003e\n\u003cli\u003eOptimized for F\/8 telescopes\u003c\/li\u003e\n\u003cli\u003eOpen-source USIS communication protocol for custom software integration\u003c\/li\u003e\n\u003cli\u003eWeighs 1.46 Kg without cameras\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak UVEX Motorized Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak UVEX Motorized spectroscope enables fully remote scientific analysis, integrating motorized control of its grating and focus with an achromatic optical design covering a wide 350 nm to 1µm spectral range. Optimized for F\/8 systems, this 1.46 Kg instrument provides a choice of five slit positions, from a high-resolution 25µm slit to a 300µm option for fainter targets, all controllable via the documented USIS protocol.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAchromatic Optics: The 350 nm to 1µm Spectral Range\u003c\/h3\u003e\n\u003cp\u003eThe UVEX is built around an achromatic optical system, specifically designed to maintain focus across an expansive spectral range from the near-ultraviolet at 350 nm to the near-infrared at 1µm. This allows you to explore phenomena beyond the visible spectrum, capturing data at the limits of modern CMOS and CCD sensor capabilities without needing to constantly refocus for different wavelengths.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eFull Remote Operation at F\/8\u003c\/h3\u003e\n\u003cp\u003eThis motorized version of the UVEX is engineered for unattended, remote operation. From your control software, you can precisely set the central wavelength by adjusting the grating angle, fine-tune instrument focus, and manage an external calibration module. This integration makes it possible to automate an entire observing session: acquiring science data, then capturing dark, flat-field, and calibration lamp frames without any physical intervention at the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 5-Position Slit Module: From 25µm to 300µm\u003c\/h3\u003e\n\u003cp\u003eThe UVEX includes a versatile slit module with five user-selectable options: 25µm, 50µm, 100µm, 300µm, and a 25µm pinhole for precise calibration. This range allows you to balance spectral resolution against signal-to-noise; use the narrow 25µm slit for detailed analysis of bright stars or the wider 300µm slit to maximize light throughput on faint nebulae. Note that slit selection is a manual adjustment performed at the instrument.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eUSIS Protocol: Open Integration for Custom Automation\u003c\/h3\u003e\n\u003cp\u003eControl of the UVEX is managed through the USIS communication protocol, an open standard documented by Shelyak. While designed for seamless integration with Shelyak's own DEMETRA software, the open protocol gives advanced users the freedom to write their own drivers and control scripts. This allows for deep integration into custom observatory automation platforms like N.I.N.A., TheSkyX, or proprietary research environments.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of the UVEX Motorized spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary advantage is \u003cstrong\u003efull remote operation\u003c\/strong\u003e. You can remotely control the central wavelength (grating), instrument focus, and an external calibration module. This allows for completely automated data acquisition sequences, which is essential for robotic observatories or simply for efficiency during a night of observing.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I change the slit on the UVEX Motorized?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eSlit selection on the UVEX is a \u003cstrong\u003emanual process\u003c\/strong\u003e. You must physically access the instrument and use a screwdriver to rotate the slit wheel to one of the five positions (25µm, 50µm, 100µm, 300µm, or 25µm hole). While the grating and focus are motorized, the slit is not.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of telescope works best with the UVEX Motorized at its optimal F\/8 ratio?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe UVEX is optimized for an \u003cstrong\u003eF\/8\u003c\/strong\u003e focal ratio, which is common for many Schmidt-Cassegrain (SCT) and Ritchey-Chrétien (RC) telescopes, especially when used with a focal reducer. A standard C8 or a 10-inch RC would be excellent matches, providing a bright, well-focused beam to the spectroscope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan the UVEX Motorized resolve the Balmer series in the spectrum of Vega (Alpha Lyrae)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. Vega is a bright A-type star with very prominent hydrogen absorption lines (the Balmer series). Using one of the narrower slits, such as the \u003cstrong\u003e25µm or 50µm\u003c\/strong\u003e option, the UVEX can easily achieve the resolution needed to clearly separate and study these lines, from H-alpha in the red down to the higher-order lines in the blue and near-UV portion of its 350 nm to 1µm range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat does the motorized focus on the UVEX Motorized adjust?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe motorized focus adjusts the internal optics of the spectroscope to ensure the spectrum is perfectly sharp on your camera's sensor. This is critical for achieving the highest possible resolution and is especially useful for compensating for small thermal shifts in focus over the course of a long observing night.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the USIS communication protocol difficult to use for custom software?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe USIS protocol is designed to be straightforward for developers. Shelyak provides documentation for the protocol, allowing programmers to integrate UVEX control into various platforms. While it requires some programming knowledge, it is a well-defined serial communication protocol, making it accessible for those familiar with creating ASCOM drivers or scripting with languages like Python.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Range\u003c\/td\u003e\n\u003ctd\u003e350 nm to 1µm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eOptimal Telescope F-ratio\u003c\/td\u003e\n\u003ctd\u003eF\/8\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Module\u003c\/td\u003e\n\u003ctd\u003eMulti-position: 25µm, 50µm, 100µm, 300µm, and 25µm hole\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Control\u003c\/td\u003e\n\u003ctd\u003eMotorized (selects central wavelength)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eFocus Control\u003c\/td\u003e\n\u003ctd\u003eMotorized (fine-tunes instrument focus)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Control\u003c\/td\u003e\n\u003ctd\u003eMotorized control of external calibration module\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCommunication Protocol\u003c\/td\u003e\n\u003ctd\u003eUSIS\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e153 x 154 x 133 mm (without cameras)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e1.46 Kg (without camera)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Motorized_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Motorized Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943032647965,"sku":"SHK-ES0034","price":9205.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-UVEX-motorized-1_c831c97a-5022-461b-8e52-940b2be7bd11.jpg?v=1789615972"},{"product_id":"shelyak-pf0011","title":"Shelyak eShel III Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eSpectral Range: 390nm to 750nm\u003c\/li\u003e\n\u003cli\u003eInstrument Type: Professional Echelle Spectroscope\u003c\/li\u003e\n\u003cli\u003eInput: Fiber-Optic Fed\u003c\/li\u003e\n\u003cli\u003eDesign: Modular Core Component\u003c\/li\u003e\n\u003cli\u003eApplication Focus: High-Resolution Astrophysical Analysis\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eeShel III Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak eShel III is a professional, fiber-fed echelle spectrograph designed for high-resolution analysis across a wide spectral range of 390nm to 750nm, enabling advanced research in topics such as exoplanetary science and stellar dynamics.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eProfessional Echelle Spectroscopy from 390nm to 750nm\u003c\/h3\u003e\n\u003cp\u003eThe eShel III achieves its high resolving power by employing an echelle grating, which uses high diffraction orders to spread light out in great detail. A cross-disperser prism then slices this spectrum into successive orders, stacking them to fill the entire surface of a camera sensor. This technique allows the instrument to capture the complete visible spectrum from 390nm to 750nm in a single exposure, without sacrificing resolution at any point in the range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eFiber-Fed Design for High-Accuracy Radial Velocity\u003c\/h3\u003e\n\u003cp\u003ePrecision is paramount in spectroscopy, especially for radial velocity measurements used to detect exoplanets. The eShel III uses a fiber-optic feed to physically decouple the spectrograph from the telescope. This isolates the instrument from mechanical vibrations, flexure, and thermal fluctuations at the telescope, allowing it to be housed in a stable, temperature-controlled environment. This stability is the key to achieving the consistent, repeatable measurements required for professional research.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe eShel III Core: Building a Complete Spectrographic System\u003c\/h3\u003e\n\u003cp\u003eThis product is the core eShel III spectroscope module and is not a standalone instrument. To create a fully operational system, it must be paired with a Fiber Injection and Guiding Unit (FIGU), a dedicated calibration module, and the required 50µm optical fibers for the target and calibration source. These components are available separately or as part of the complete eShel III system package. The entire system is controlled by the free Demetra software, which handles acquisition, remote control of the modules, and data reduction.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is an echelle spectroscope and why is the eShel III designed this way?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAn \u003cstrong\u003eechelle spectroscope\u003c\/strong\u003e uses a special grating at a high angle to achieve very high spectral resolution. This creates overlapping spectral orders, which a second optical element (a cross-disperser) separates and stacks vertically on the sensor. This design allows the eShel III to capture a very wide spectral range (390nm to 750nm) at high resolution in a single image, something a traditional single-order spectrograph cannot do.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat additional components do I need to operate the eShel III Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe eShel III Spectroscope is the central module of a larger system. For operation, you will require:\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003eA \u003cstrong\u003eFiber Injection \u0026amp; Guiding Unit (FIGU)\u003c\/strong\u003e to inject the starlight into the fiber.\u003c\/li\u003e\n\u003cli\u003eA \u003cstrong\u003eCalibration Module\u003c\/strong\u003e for wavelength and flat-field calibration.\u003c\/li\u003e\n\u003cli\u003eTwo \u003cstrong\u003eoptical fibers\u003c\/strong\u003e (one for the star, one for calibration).\u003c\/li\u003e\n\u003cli\u003eA compatible astronomical camera, such as the ATIK 460Ex.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the fiber-fed design of the eShel III improve data quality for exoplanet hunting?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eDetecting the tiny Doppler shift in a star's light caused by an orbiting exoplanet requires extreme stability. By using an optical fiber, the \u003cstrong\u003eeShel III can be placed in a temperature-controlled room\u003c\/strong\u003e, completely isolated from the telescope's movement, vibrations, and changing orientation. This prevents instrumental shifts that could mimic or mask the real stellar signal, ensuring the measured radial velocity is highly accurate.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the eShel III for studying the spectral evolution of a variable star like BW Vulpeculae?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. The eShel III is ideal for this type of research. Its ability to capture the entire visible spectrum at high resolution in a single exposure allows you to monitor changes in multiple spectral lines simultaneously over time. This is crucial for understanding the complex atmospheric pulsations and dynamics of stars like the Beta Cephei variable BW Vulpeculae.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat software is required to control the eShel III and its modules?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe entire eShel III system is controlled by Shelyak's \u003cstrong\u003eDemetra software\u003c\/strong\u003e, which is available as a free download. Demetra manages spectra acquisition, controls the FIGU and calibration modules remotely, and includes tools for data reduction, from raw images to calibrated spectra.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the eShel III Spectroscope a standalone instrument?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. This product is the \u003cstrong\u003ecore spectroscope module only\u003c\/strong\u003e. It is designed to be the heart of a complete spectrographic system and requires the additional components listed above for operation. Shelyak offers a complete package that includes all necessary modules for a functioning instrument.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eInstrument Type\u003c\/td\u003e\n\u003ctd\u003eFiber-Fed Echelle Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Range\u003c\/td\u003e\n\u003ctd\u003e390nm to 750nm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eInput Connector Type\u003c\/td\u003e\n\u003ctd\u003eFC\/PC\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSystem Requirement\u003c\/td\u003e\n\u003ctd\u003eRequires FIGU, Calibration Module, and Optical Fibers (sold separately)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eControl Software\u003c\/td\u003e\n\u003ctd\u003eDemetra (Free Download)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943035072797,"sku":"SHK-PF0011","price":15573.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-eShel-III-Spectroscope-1_347805d2-ec23-482e-97ee-2fcea894c69b.jpg?v=1789616046"},{"product_id":"shelyak-pf0012","title":"Shelyak eShel Calibration Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eContains Thorium-Argon (ThAr) and Flat-Field Lamps\u003c\/li\u003e\n\u003cli\u003eDesigned for eShel and Whoppshel Spectroscopes\u003c\/li\u003e\n\u003cli\u003eCompatible with other fiber-fed Echelle systems\u003c\/li\u003e\n\u003cli\u003eRemotely controlled via RS 232 interface\u003c\/li\u003e\n\u003cli\u003eIntegrates with Demetra and Audela software\u003c\/li\u003e\n\u003cli\u003eControls FIGU mirror for source selection\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak eShel Calibration Module\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak eShel Calibration Module is an essential component for high-resolution spectroscopy, providing the necessary Thorium-Argon (ThAr) and flat-field light sources for professional-grade data reduction. Designed for seamless integration with the eShel and Whoppshel spectroscopes, this unit automates the entire calibration process. It allows you to acquire precise wavelength references and correct for instrument signatures remotely, ensuring your scientific data is both accurate and repeatable.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThorium-Argon and Flat-Field Lamps for Full Calibration\u003c\/h3\u003e\n\u003cp\u003eThis module houses the two critical light sources required for echelle spectroscopy. The Thorium-Argon lamp produces a dense forest of known emission lines across the visible spectrum, serving as an absolute reference for wavelength calibration. The internal flat lamp illuminates the entire optical path, allowing you to create master flat fields to correct for pixel-to-pixel variations in the sensor and remove artifacts like dust shadows.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eIntegrated Remote Control for Automated Observations\u003c\/h3\u003e\n\u003cp\u003eThrough its RS 232 interface, the eShel Calibration Module connects directly to your control computer, enabling full remote operation from software like Demetra or Audela. This integration extends to controlling the FIGU mirror, which selects the light source fed to the spectroscope. You can programmatically switch between capturing your science target from the telescope and acquiring calibration frames without any manual intervention, streamlining your workflow for unattended or robotic observations.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the Shelyak eShel Calibration Module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe eShel Calibration Module provides the two light sources necessary for calibrating high-resolution echelle spectrographs. It contains a \u003cstrong\u003eThorium-Argon (ThAr) lamp\u003c\/strong\u003e for precise wavelength calibration and a \u003cstrong\u003eflat lamp\u003c\/strong\u003e for creating flat-fields to correct for detector and optical path imperfections.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the eShel Calibration Module with a non-Shelyak spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. While it is designed for native integration with the Shelyak eShel and Whoppshel, the module can be used to calibrate any other fiber-fed Echelle spectroscope that requires ThAr and flat-field illumination.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does remote control of the eShel Calibration Module work?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module is controlled via an \u003cstrong\u003eRS 232 serial interface\u003c\/strong\u003e from your PC. It integrates directly with acquisition software like \u003cstrong\u003eDemetra\u003c\/strong\u003e or \u003cstrong\u003eAudela\u003c\/strong\u003e, allowing you to turn the lamps on\/off and switch the FIGU mirror between the telescope and calibration sources as part of an automated observing sequence.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy are both a ThAr and a flat lamp needed for the eShel?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eEach lamp serves a distinct purpose:\n\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eThorium-Argon (ThAr):\u003c\/strong\u003e Produces a spectrum with thousands of well-documented emission lines. These act as a \"ruler\" to accurately map pixels on your detector to specific wavelengths.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eFlat Lamp:\u003c\/strong\u003e Provides a uniform, featureless light source. This reveals pixel sensitivity differences, vignetting, and the location of dust on your optics, allowing these effects to be mathematically removed from your science images.\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the eShel Calibration Module improve measurements of a star like 51 Pegasi?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWhen searching for exoplanets via the radial velocity method, as was done with 51 Pegasi, incredibly small Doppler shifts in the star's spectrum must be measured. The ThAr lamp in the eShel Calibration Module provides the stable, high-precision wavelength reference required to detect these minute shifts, making such scientific work possible.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I am building a spectral library with my Whoppshel, is this module necessary?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, it is essential for creating an accurate library. The flat lamp corrects instrumental signatures, ensuring the spectral profile you record is that of the star, not your equipment. The ThAr lamp provides the absolute wavelength calibration, so you can confidently compare your spectra to other observations and databases.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eeShel, Whoppshel, and other fiber-fed Echelle spectrographs\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Sources\u003c\/td\u003e\n\u003ctd\u003eThorium-Argon (ThAr) Lamp, Flat Lamp\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eControl Interface\u003c\/td\u003e\n\u003ctd\u003eRS 232\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSoftware Integration\u003c\/td\u003e\n\u003ctd\u003eDemetra, Audela\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRemote Functions\u003c\/td\u003e\n\u003ctd\u003eLamp control, FIGU mirror source selection\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Calibration_Unit_Upgrade_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Calibration Unit Upgrade Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_eShel_Calibration_Power_Supply_Addendum_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak eShel Calibration Power Supply Addendum Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943035564317,"sku":"SHK-PF0012","price":7882.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-eShel-calibration-module-1_c0ff1be3-f396-41a5-882e-b70e961c715a.jpg?v=1789616054"},{"product_id":"shelyak-pf0021v","title":"Shelyak LISA Spectroscope (VIS)","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eDesigned for spectroscopy of faint deep-sky objects\u003c\/li\u003e\n\u003cli\u003eFast optical design optimized for modern telescopes\u003c\/li\u003e\n\u003cli\u003eInterchangeable slits to balance resolution and brightness\u003c\/li\u003e\n\u003cli\u003eMirror slit design for accurate target acquisition and guiding\u003c\/li\u003e\n\u003cli\u003eLightweight 1.4 kg chassis\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLISA Spectroscope (VIS)\u003c\/h2\u003e\n\u003cp\u003eThe LISA Spectroscope is a lightweight 1.4 kg instrument designed for the scientific analysis of faint celestial objects from comets to quasars. It features a 4 mm long slit and an optical system with custom-made components, enabling you to capture detailed spectra of targets like novae, supernovae, and the redshift of distant galaxies.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eEngineered for Faint Object Spectroscopy\u003c\/h3\u003e\n\u003cp\u003eThe LISA's optical path is specifically engineered for low-light targets. Its fast focal ratio makes it an ideal match for telescopes operating natively at f\/5, or for Schmidt-Cassegrain and Ritchey-Chrétien systems paired with a focal reducer. This design maximizes throughput for challenging subjects such as faint variable stars or confirming planetary nebulae.\u003c\/p\u003e\n\u003cp\u003eWith a resolving power of approximately 1,000, the LISA separates spectral lines with enough detail for serious scientific work. Its spectral range covers the entire visible spectrum and extends into the near-ultraviolet and near-infrared, providing broad coverage for a wide variety of astronomical targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eMirror Slit and Interchangeable Slits\u003c\/h3\u003e\n\u003cp\u003eAcquiring and holding a faint object on a narrow slit is a primary challenge in spectroscopy. The LISA incorporates a mirror slit that allows you to see the entire starfield, making it simple to accurately position your target. For long exposures, a C-mount guide port allows you to connect an autoguiding camera to maintain perfect tracking.\u003c\/p\u003e\n\u003cp\u003eTo adapt to different targets and conditions, the LISA includes a standard set of four interchangeable slits (15, 19, 23, and 35µm). This allows you to prioritize high resolution for brighter objects or greater light throughput for the faintest targets. Additional specialized slits, such as wide or photometric versions, are available separately to further expand the instrument's capabilities.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eStandardized Telescope and Camera Interfaces\u003c\/h3\u003e\n\u003cp\u003eThe LISA connects to your telescope via a standard 2\" nosepiece, which is included. This nosepiece can be removed to expose a female M42x0.75 T-thread for more rigid connections. The imaging camera also connects via a T-thread, with a backfocus of 54.9 mm to accommodate filter wheels and other accessories.\u003c\/p\u003e\n\u003cp\u003eThe dedicated guiding camera port uses a standard C-mount thread with a 17.5 mm backfocus. For users of ATIK cameras, the LISA also includes a 13 mm T-thread extension ring to ensure the sensor is placed at the correct distance from the optics.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of objects is the LISA Spectroscope designed for?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe LISA Spectroscope is optimized for faint deep-sky objects. Its primary targets include \u003cstrong\u003ecomets, novae, supernovae, faint variable stars, distant galaxies, and quasars\u003c\/strong\u003e. It is an ideal instrument for pro-am research and scientific characterization of these challenging targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of telescope do I need to use the LISA Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe LISA performs best with telescopes that have a fast focal ratio, around f\/5. It can be used directly on instruments with this native focal ratio. For telescopes with longer focal ratios, such as most \u003cstrong\u003eSchmidt-Cassegrains or Ritchey-Chrétiens (f\/8 to f\/10)\u003c\/strong\u003e, you will need to use a \u003cstrong\u003efocal reducer\u003c\/strong\u003e to achieve optimal performance.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I keep a star centered on the LISA Spectroscope's slit for long exposures?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe LISA Spectroscope features two key systems for this. First, its \u003cstrong\u003emirror slit\u003c\/strong\u003e allows you to see the starfield around the slit for easy initial positioning. Second, it has a dedicated \u003cstrong\u003eC-mount guide port\u003c\/strong\u003e, allowing you to attach an autoguiding camera that sends corrections to your mount, keeping the target perfectly centered automatically.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I change the resolution of the LISA Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The LISA comes with a set of four interchangeable slits of different widths. Using a narrower slit provides higher spectral resolution, which is ideal for separating close spectral lines on brighter targets. A wider slit allows more light to pass through, which is better for capturing a signal on very faint objects at the cost of lower resolution.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow would I use the LISA Spectroscope to study a supernova like SN 2023ixf in the Pinwheel Galaxy (M101)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor a faint target like a supernova in a distant galaxy, you would likely select one of the wider slits (e.g., 23µm or 35µm) to maximize light throughput. You would use the mirror slit to locate the supernova within M101 and position it precisely. For the necessary long exposures, an autoguiding camera attached to the C-mount port would be essential to ensure the target does not drift off the slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the LISA Spectroscope with my 8\" f\/10 SCT?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, but you will need two accessories for optimal results. First, you'll need a \u003cstrong\u003efocal reducer (e.g., 0.63x or 0.5x)\u003c\/strong\u003e to shorten your SCT's focal ratio to be closer to f\/5. Second, for a secure mechanical connection to the SCT's rear cell, you will need a specific adapter like the Shelyak BA0027 variable T-adapter instead of the standard 2\" nosepiece.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Length\u003c\/td\u003e\n\u003ctd\u003e4 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e1.4 kg (without camera)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolving Power\u003c\/td\u003e\n\u003ctd\u003e~1,000 (with 23 µm slit)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Range\u003c\/td\u003e\n\u003ctd\u003e400 - 700 nm (extends to near-UV\/IR)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eAperture\u003c\/td\u003e\n\u003ctd\u003ef\/5\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eIncluded Slits\u003c\/td\u003e\n\u003ctd\u003e15, 19, 23, 35 µm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eTelescope Connection\u003c\/td\u003e\n\u003ctd\u003e2\" Nosepiece or M42x0.75 T-thread (female)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eImaging Camera Connection\u003c\/td\u003e\n\u003ctd\u003eM42x0.75 T-thread (male)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eImaging Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e54.9 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eGuiding Camera Connection\u003c\/td\u003e\n\u003ctd\u003eC-mount\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eGuiding Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e17.5 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eLISA Spectroscope\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eInterchangeable Slit Holder with 4 Slits (15, 19, 23, 35µm)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e2\" Telescope Nosepiece\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e13mm T-thread Extension Ring (for ATIK cameras)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_LISA_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak LISA Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943037530397,"sku":"SHK-PF0021V","price":6882.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-LISA-Spectroscope-VIS-1_8002f53b-c8de-4ff5-ad2b-60eccfc54f16.jpg?v=1789616078"},{"product_id":"shelyak-pf0074","title":"Shelyak Uvex Motors Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eMotorizes your existing Shelyak UVEX Spectrograph\u003c\/li\u003e\n\u003cli\u003eEnables remote control of central wavelength via motorized grating\u003c\/li\u003e\n\u003cli\u003eProvides remote fine-focus adjustment for optimal resolution\u003c\/li\u003e\n\u003cli\u003eAdds only 1.46 kg to the UVEX assembly (without camera)\u003c\/li\u003e\n\u003cli\u003eIntegrates control for an external calibration module\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Uvex Motors Module\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Uvex Motors module transforms your manually-operated spectrograph into a fully remote instrument, adding just 1.46 kg to your optical train. Housed within a 153 x 154 x 133 mm frame when installed, this upgrade provides precise, repeatable motorized control over both the grating for central wavelength selection and the fine focus mechanism for achieving optimal spectral resolution from your observatory control room.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eRemote and Automated Spectroscopy with the UVEX Motors Module\u003c\/h3\u003e\n\u003cp\u003eThis module is a direct upgrade for the Shelyak UVEX spectrograph, converting it from a hands-on instrument to a fully automated component of your imaging setup. By motorizing the critical adjustments, you can now operate the UVEX remotely, eliminating vibrations and enabling long, scripted observation sequences without being physically present at the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eMotorized Grating and Focus: Precision Control in a 1.46 kg Package\u003c\/h3\u003e\n\u003cp\u003eThe core of this upgrade lies in its two primary motorized functions. The motorized grating allows you to remotely select the central wavelength of your spectrum, making it possible to study different spectral features of a target in a single session. The motorized focus is critical for compensating for temperature changes throughout the night, ensuring your spectra remain perfectly sharp for the highest possible resolution.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eWavelength Selection:\u003c\/strong\u003e Remotely scan different areas of the spectrum without touching the instrument, ideal for variable stars or objects with complex spectral features.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eFocus Adjustment:\u003c\/strong\u003e Achieve and maintain critical focus to resolve fine spectral lines, a task that is nearly impossible to perfect manually on a remote system.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eMinimal Footprint:\u003c\/strong\u003e The entire motorized system adds 1.46 kg to the UVEX, a manageable weight that typically requires only minor rebalancing of your mount.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAutomated Calibration: 4-Position Control for Sky, Dark, Flat \u0026amp; Cal Frames\u003c\/h3\u003e\n\u003cp\u003eBeyond mechanical control, the Uvex Motors module integrates the logic for a complete, automated calibration workflow. It includes the same control features as the SPOX module, allowing it to manage an external calibration unit. This enables you to seamlessly switch between acquiring data from the sky and capturing necessary dark, flat, and calibration lamp frames for professional-grade data reduction.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eSoftware Integration:\u003c\/strong\u003e The module is fully supported by Shelyak's DEMETRA software for a plug-and-play experience.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eOpen Protocol:\u003c\/strong\u003e For users with custom observatory software, Shelyak has published the USIS communication protocol, allowing for deep integration into any control environment.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary benefit of adding the Uvex Motors module to my spectrograph?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary benefit is \u003cstrong\u003eremote operation\u003c\/strong\u003e. The Uvex Motors module allows you to control the spectrograph's grating (central wavelength) and focus from a computer, eliminating the need to be physically at the telescope. This is essential for automated observatories and for maintaining optimal focus as temperatures change during the night.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need a separate calibration module to use all the features of the Uvex Motors module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The Uvex Motors module includes the electronic control system for an \u003cstrong\u003eexternal calibration module\u003c\/strong\u003e, but the calibration unit itself is a separate item. This feature allows you to automate your entire data acquisition sequence, from capturing the target's spectrum (Sky) to taking Flat, Dark, and reference lamp (Calibration) frames.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I control the Uvex Motors module with software other than DEMETRA?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. While it is designed for seamless integration with Shelyak's DEMETRA software, the module uses an open communication protocol called \u003cstrong\u003eUSIS\u003c\/strong\u003e. Shelyak provides documentation for this protocol, allowing advanced users to write their own scripts or integrate control into third-party observatory software like N.I.N.A. or SGP via custom drivers.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Uvex Motors module help when observing a Be star like Gamma Cassiopeiae?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eBe stars like Gamma Cassiopeiae (gamma Cas) have dynamic emission lines (like H-alpha) that change over time. The Uvex Motors module allows you to precisely and repeatedly center your grating on these specific lines night after night. You can also remotely check focus to ensure you achieve the highest possible resolution to measure subtle changes in the line profiles, which is crucial for this type of scientific work.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill I need to rebalance my telescope after installing the 1.46 kg Uvex Motors module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eMost likely, yes. The module and the UVEX spectrograph together weigh 1.46 kg (without a camera). This additional weight will almost certainly require you to rebalance your mount in both axes to ensure accurate tracking and guiding.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI use an 8\" SCT at f\/10. How does motorized focus on the Uvex Motors module improve my results?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eOn an SCT, temperature changes can cause significant focus shift. The motorized focus control of the Uvex Motors module is a major advantage. It allows you to make tiny, precise adjustments to the spectrograph's internal focus remotely throughout the night, ensuring your spectral lines remain sharp and narrow without having to touch the telescope's primary focuser, which can introduce mirror shift.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eMotorized Grating Control\u003c\/td\u003e\n\u003ctd\u003eAllows remote selection of the central observation wavelength.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eMotorized Focus Control\u003c\/td\u003e\n\u003ctd\u003eAllows remote fine-tuning of focus for optimal optical quality.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Module Control\u003c\/td\u003e\n\u003ctd\u003eRemotely controls an external calibration unit, switching between Sky, Dark, Flat, and Calibration light sources.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions (with UVEX)\u003c\/td\u003e\n\u003ctd\u003e153 x 154 mm, Height: 133 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight (with UVEX, no camera)\u003c\/td\u003e\n\u003ctd\u003e1.46 kg\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eUvex Motors Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Motors_Module_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Motors Module Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943040053533,"sku":"SHK-PF0074","price":2453.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Uvex-Motors-module-1_d2d12418-d094-4058-ae73-21a70450c813.jpg?v=1789616127"},{"product_id":"shelyak-pf0083","title":"Shelyak Alpy 200 Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eResolving power of R~130 optimized for faint targets\u003c\/li\u003e\n\u003cli\u003eFast F\/4 optical design\u003c\/li\u003e\n\u003cli\u003eMulti-position wheel with 25µm, 50µm, 100µm, and 300µm slits\u003c\/li\u003e\n\u003cli\u003eCompact and lightweight at 65mm long and only 200g\u003c\/li\u003e\n\u003cli\u003eVariable mechanical backfocus from 10.5mm to 21mm\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAlpy 200 Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThe Alpy 200 Spectroscope is engineered for a specific scientific purpose: capturing the spectra of extremely faint celestial objects. Its optical design delivers a resolving power of R~130 through a fast F\/4 system, prioritizing signal collection on targets like distant quasars and supernovae. The entire instrument is housed in a compact 65mm x 45mm body that weighs only 200g, making it compatible with a wide range of telescopes. A multi-position slit wheel offers options from a 25µm pinhole to a 300µm slit, while the standard T-mount (M42x0.75mm) interface accommodates science cameras with a mechanical backfocus between 10.5mm and 21mm.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eLow-Resolution Spectroscopy: An R~130 Grism for Faint Targets\u003c\/h3\u003e\n\u003cp\u003eThe core of the Alpy 200 is a 200 gr\/mm grism (grating + prism) that provides a resolving power of R~130. This low-resolution design is a deliberate trade-off, spreading the light from a faint object over fewer pixels to maximize signal-to-noise ratio. This makes it possible to acquire usable spectra on faint galaxies, novae, and supernovae that would be undetectable with higher-resolution systems. The F\/4 aperture is exceptionally fast for a spectroscope, further enhancing its sensitivity and reducing required exposure times across its operational range of 375nm to 750nm.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eMulti-Position Slit Wheel: From 25µm to 300µm\u003c\/h3\u003e\n\u003cp\u003eThe Alpy 200 incorporates a multi-position wheel with a selection of slits to adapt to different targets and observing conditions. It includes a 25µm pinhole, four slits of 25µm, 50µm, 100µm, and 300µm, and a 3mm hole for easy target acquisition. The narrower slits provide the maximum resolving power, while the wider slits are crucial for very faint targets or nights of poor seeing, ensuring more of the star's light enters the spectroscope. This flexibility allows you to optimize the instrument for everything from extended nebulae to point-like quasars.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCompact 200g Design: Spectroscopy on an 80mm Telescope\u003c\/h3\u003e\n\u003cp\u003eWeighing just 200g and measuring 65mm in length with a 45mm diameter, the Alpy 200 is one of the most compact and lightweight scientific spectroscopes available. Its minimal weight and size mean it can be mounted on telescopes as small as 80mm in diameter without creating significant balance or stability issues. This opens the door to serious astrophysical research for observers using modest, portable mounts and optical tubes, removing the need for a heavy-duty observatory setup.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eModular System: 10.5-21mm Backfocus and Demetra Software\u003c\/h3\u003e\n\u003cp\u003eThe Alpy 200 is designed as the core of a modular system. It connects to your science camera via a standard M42x0.75mm T-mount and supports a mechanical backfocus range of 10.5mm to 21mm, compatible with many popular astronomy cameras. For a complete scientific workflow, optional autoguiding and calibration modules can be added, bringing the total required backfocus to 64mm. The entire system is supported by the free Demetra software, which handles everything from image acquisition to final data reduction.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAlpy 200 vs. Alpy 600: Choosing Faintness Over Resolution\u003c\/h3\u003e\n\u003cp\u003eThe Alpy 200 was developed as a specialized version of its sibling, the Alpy 600, for a different observational goal. The choice between them is a direct trade-off between resolving power and sensitivity.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eAlpy 600 Advantage:\u003c\/strong\u003e With a resolving power of R~600, the Alpy 600 can reveal much finer detail in the spectra of bright stars, resolving closer spectral lines and enabling more detailed analysis of stellar atmospheres.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eAlpy 200 Advantage:\u003c\/strong\u003e The Alpy 200's R~130 resolving power concentrates the target's light, making it vastly more efficient for extremely faint objects. It is the superior choice for classifying supernovae, identifying quasars, and studying the general characteristics of faint galaxies where capturing any spectrum at all is the primary challenge.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of camera works best with the Alpy 200 Spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Alpy 200 connects via a standard \u003cstrong\u003eM42x0.75mm T-mount\u003c\/strong\u003e. It is compatible with any monochrome camera that has a mechanical backfocus between \u003cstrong\u003e10.5mm and 21mm\u003c\/strong\u003e. For optimal results, a sensor with a diagonal of 14mm or larger is recommended to capture the full spectral range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the Alpy 200's low R~130 resolution?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eLow resolution is a feature, not a limitation, for faint-object spectroscopy. By spreading the light over a smaller area on the sensor, the Alpy 200 achieves a much higher signal-to-noise ratio per pixel. This allows you to obtain a usable spectrum from targets like supernovae, quasars, and faint galaxies that would be too dim to analyze with a higher-resolution spectroscope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Alpy 200 to get a spectrum of a supernova in an 8-inch SCT?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. The Alpy 200's compact \u003cstrong\u003e200g\u003c\/strong\u003e weight and high sensitivity make it an ideal match for common telescopes like 8\" Schmidt-Cassegrains. This combination is powerful enough to capture spectra from very faint targets; for example, scientific data has been published on magnitude 18+ supernovae using this spectroscope on similar amateur instruments.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the different slits (25µm, 50µm, 100µm, 300µm) on the Alpy 200?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe interchangeable slits allow you to adapt the spectroscope to your target and atmospheric conditions.\n\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eNarrow slits (25µm, 50µm):\u003c\/strong\u003e Provide the highest possible spectral resolution (up to R~130) for brighter objects where detail is important.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eWider slits (100µm, 300µm):\u003c\/strong\u003e Allow more light to enter the spectroscope, which is critical for very faint objects or when seeing is poor. This sacrifices some resolution for a much stronger signal.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the Alpy 200 perform on extended objects like the Orion Nebula (M42)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Alpy 200 is excellent for extended objects. The slit, which is \u003cstrong\u003e3mm\u003c\/strong\u003e long, allows you to isolate a specific region of the nebula. By positioning the slit across different areas—such as the Trapezium cluster versus the outer loops—you can take separate spectra to study how the physical conditions (like ionization) change across the object.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need the optional guiding and calibration modules for the Alpy 200?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, they are not required to start, but they complete the scientific workflow. The base Alpy 200 module is fully functional for capturing spectra. The optional guiding module makes it easier to keep your target precisely on the slit for long exposures. The calibration module provides a reference lamp (Argon-Neon) for highly accurate wavelength calibration, which is essential for scientific measurements like redshift.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolving Power\u003c\/td\u003e\n\u003ctd\u003eR ~130 with 23µm slit\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eAperture\u003c\/td\u003e\n\u003ctd\u003eF\/4\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Options\u003c\/td\u003e\n\u003ctd\u003e25µm, 50µm, 100µm, 300µm slits; 25µm \u0026amp; 3mm holes\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Length\u003c\/td\u003e\n\u003ctd\u003e3mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCamera Interface\u003c\/td\u003e\n\u003ctd\u003eT-mount (M42x0.75mm)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eMechanical Backfocus\u003c\/td\u003e\n\u003ctd\u003e10.5mm to 21mm range\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eTotal Backfocus (with optional modules)\u003c\/td\u003e\n\u003ctd\u003e64mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eDimensions\u003c\/td\u003e\n\u003ctd\u003e65mm length, 45mm diameter\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eWeight\u003c\/td\u003e\n\u003ctd\u003e200g\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_200_Core_Module_Assembly_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 200 Core Module Assembly Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/www.shelyak.com\/software\/?lang=en\" target=\"_blank\"\u003e\u003csvg xmlns=\"http:\/\/www.w3.org\/2000\/svg\" viewbox=\"0 0 640 512\" class=\"DAV-img-box\"\u003e\u003cpath fill=\"#0047a7\" d=\"M128 32C92.7 32 64 60.7 64 96l0 256 64 0 0-256 384 0 0 256 64 0 0-256c0-35.3-28.7-64-64-64L128 32zM19.2 384C8.6 384 0 392.6 0 403.2C0 445.6 34.4 480 76.8 480l486.4 0c42.4 0 76.8-34.4 76.8-76.8c0-10.6-8.6-19.2-19.2-19.2L19.2 384z\"\u003e\u003c\/path\u003e\u003c\/svg\u003e \n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eDownload Software\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Backfocus_Diagram.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Backfocus Diagram\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943040839965,"sku":"SHK-PF0083","price":1349.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Alpy-200-Spectroscope-1_176240af-29c8-496c-99b2-dcd0a2cd3d0c.jpg?v=1789616153"},{"product_id":"shelyak-pu0019","title":"Shelyak T-mount front part for the Lhires III","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eReplaces the standard Lhires III front panel\u003c\/li\u003e\n\u003cli\u003eProvides a female M42x0.75mm T-mount thread\u003c\/li\u003e\n\u003cli\u003eEnables direct connection to custom optical trains\u003c\/li\u003e\n\u003cli\u003eInstalls with the original 8 screws\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eT-mount front part for the Lhires III\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak T-mount Front Part for the Lhires III converts the spectroscope's input to a standard female M42x0.75mm thread for direct connection to custom optical trains. Installation replaces the stock panel via 8 screws, creating a secure interface when the default Schmidt-Cassegrain adapter or 2-inch nosepiece is unsuitable for your setup.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eLhires III T-Mount Adapter: M42x0.75mm Female Thread for Custom Setups\u003c\/h3\u003e\n\u003cp\u003eThis T-mount adapter is the dedicated solution for integrating the Lhires III spectroscope into imaging setups that cannot use the standard Schmidt-Cassegrain adapter or a 2-inch nosepiece. It creates a direct, threaded M42x0.75mm connection point, eliminating potential flexure from slip-fit adapters and ensuring rigid collimation.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eDirect Threaded Connection:\u003c\/strong\u003e Provides a secure M42x0.75mm female T-thread for direct attachment to off-axis guiders, filter wheels, or custom camera spacers.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eReplaces Stock Panel:\u003c\/strong\u003e The part is a complete replacement for the original Lhires III front panel, installed by removing the existing 8 screws for a rigid, factory-fit integration.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eAlternative to Standard Adapters:\u003c\/strong\u003e Specifically designed for astronomers whose setups require a T-thread interface instead of the included SCT or 2-inch adapters.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen would I need the T-mount Front Part for my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou need this part if your telescope, focuser, or camera setup requires a direct M42x0.75mm T-thread connection. It replaces the standard Lhires III front panel to provide this common interface, bypassing the need for the included SCT adapter or 2\" nosepiece.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow is the T-mount Front Part installed on the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eInstallation is straightforward. You simply remove the 8 screws holding the standard front panel on your Lhires III spectroscope, take the old panel off, and attach this new T-mount front part using the same 8 screws.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this T-mount Front Part with my 8\" f\/10 Schmidt-Cassegrain?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWhile you can, the standard adapter included with the Lhires III is already designed for Schmidt-Cassegrain telescopes. This T-mount part is intended for situations where the standard SCT adapter does not work, such as when you have an off-axis guider or filter wheel with T-threads in your imaging train.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes this part change the back focus of the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis part replaces the front panel and establishes a new, standard M42x0.75mm connection point. You will need to calculate your spacing from this new reference plane to your camera sensor. It is not a simple spacer but a fundamental change to the instrument's input interface.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the T-mount Front Part for the Lhires III compatible with ZWO or QHY cameras?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Most dedicated astronomy cameras from brands like ZWO and QHY use M42x0.75mm T-threads as their primary connection standard. This front part allows you to create a direct, rigid, all-threaded connection from your camera and accessories to the Lhires III spectroscope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the thread specification for this Lhires III T-mount adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe adapter provides a standard female T-mount thread, which is specified as \u003cstrong\u003eM42x0.75mm\u003c\/strong\u003e. This ensures compatibility with the vast majority of T-rings, spacers, and accessories in the astronomy market.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eThread Type\u003c\/td\u003e\n\u003ctd\u003eFemale T-Mount (M42x0.75mm)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eInstallation\u003c\/td\u003e\n\u003ctd\u003eReplaces front panel (8 screws)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eT-mount front part for Lhires III\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943041134877,"sku":"SHK-PU0019","price":172.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-T-mount-front-part-for-the-Lhires-III-1_e0df2661-9fc7-4d82-849e-e3dc76a1c68d.jpg?v=1789616162"},{"product_id":"shelyak-pu0024","title":"Shelyak Lhires III Photo Tripod Adapter","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eMounts Lhires III Spectroscope to a Standard Photo Tripod\u003c\/li\u003e\n\u003cli\u003eUses Standard Kodak Tripod Thread\u003c\/li\u003e\n\u003cli\u003eIdeal for Public Outreach and Solar Observation\u003c\/li\u003e\n\u003cli\u003eSimple Two-Screw Installation\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Lhires III Photo Tripod Adapter\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Lhires III Photo Tripod Adapter provides a dedicated, secure connection between your spectroscope and any standard photo tripod, attaching quickly with just two screws for a stable, portable setup.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eQuick Two-Screw Mounting for the Lhires III Spectroscope\u003c\/h3\u003e\n\u003cp\u003eThis adapter is designed specifically for situations where an astronomical mount is impractical, such as public outreach events or quick visual solar checks. By mounting the Lhires III on a standard photographic tripod, you can create a stable, accessible platform for naked-eye solar spectrum demonstrations.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eStandard Tripod Compatibility:\u003c\/strong\u003e Features a standard Kodak thread for use with virtually any photo or video tripod.\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eSecure Attachment:\u003c\/strong\u003e Mounts directly to the underside of the Lhires III body with two screws for a rigid, stable connection.\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eIdeal for Outreach:\u003c\/strong\u003e Perfect for daytime solar viewing at public events, schools, or science fairs where portability and ease of use are critical.\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the Shelyak Lhires III Photo Tripod Adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter allows you to mount the Lhires III spectroscope directly onto a standard photographic tripod. This provides a stable, portable setup ideal for public outreach, educational demonstrations, and visual observation of the Sun's spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of tripod is compatible with the Lhires III Photo Tripod Adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe adapter uses a standard Kodak thread, which is the universal standard for photographic tripods. It will connect to virtually any photo or video tripod head.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I install the Photo Tripod Adapter on my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eInstallation is straightforward. The adapter is designed to be quickly mounted to the underside of the Lhires III body using two screws, providing a secure fit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the Lhires III Photo Tripod Adapter suitable for long-exposure spectroscopy?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this adapter is intended for quick setups and visual use, particularly for solar observation. For long-exposure scientific work that requires tracking, you should mount the Lhires III to a telescope on a properly polar-aligned equatorial mount.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary use case for putting a Lhires III on a photo tripod?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe most common use is for public events or educational settings to observe the Sun's spectrum visually. A photo tripod provides a simple, stable, and easily transportable platform that doesn't require the complexity of an astronomical mount.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I mount a Lhires III directly to an equatorial mount with this adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. This adapter features a photo tripod thread, not a Vixen or Losmandy-style dovetail bar. To attach the Lhires III to an astronomical mount, you would typically attach it to a telescope that is already on the mount.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943041495325,"sku":"SHK-PU0024","price":99.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Photo-tripod-adapter-1_0c022ee9-6aff-4d9e-9e42-fb7c98bfb134.jpg?v=1789616170"},{"product_id":"shelyak-pu0149","title":"Shelyak ST8\/10 adapter for Alpy 600","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eCustom adapter for SBIG ST7, ST8, ST10, and ST2000 cameras\u003c\/li\u003e\n\u003cli\u003eMounts compatible SBIG cameras to a Shelyak Alpy 600 spectroscope\u003c\/li\u003e\n\u003cli\u003eReplaces the camera's standard front plate\u003c\/li\u003e\n\u003cli\u003eSolves the mechanical backfocus incompatibility between these devices\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eST8\/10 adapter for Alpy 600\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak ST8\/10 Adapter for Alpy 600 is the specific mechanical flange required to mount classic SBIG ST7, ST8, ST10, and ST2000 series cameras onto the Alpy 600 spectroscope. This adapter directly addresses the excessive mechanical backfocus of these cameras, which otherwise prevents a secure and focused connection.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eSolving SBIG Backfocus for Alpy 600 Spectroscopy\u003c\/h3\u003e\n\u003cp\u003eThe mechanical design of SBIG's ST7, ST8, ST10, and ST2000 cameras results in a backfocus distance that is too large for direct attachment to an Alpy 600 spectroscope. This adapter is not a simple spacer; it is a replacement front plate for the camera body. By removing the camera's original plate and installing this custom flange, you physically shorten the optical path to achieve the correct spacing for spectroscopy with the Alpy 600.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCritical Installation and Focusing Warning for ST7\/ST8\/ST10\/ST2000 Cameras\u003c\/h3\u003e\n\u003cp\u003eWhen this adapter is installed, the front lens of the Alpy 600 spectroscope is positioned extremely close to the protective window of the CCD sensor. You must exercise extreme care when focusing the spectrum. Racking the focuser in too far can cause the Alpy's lens to make physical contact with the camera's window, risking permanent damage to both optics.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhich SBIG cameras is the ST8\/10 adapter for Alpy 600 compatible with?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter is specifically designed for the SBIG ST7, ST8, ST10, and ST2000 model CCD cameras. It will not work with other SBIG models or cameras from other manufacturers.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy is the ST8\/10 adapter necessary for using my SBIG ST7 with an Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe standard mechanical backfocus of the SBIG ST7 camera is too long to allow the Alpy 600 spectroscope to reach focus. This adapter replaces the camera's front plate, effectively reducing the distance to bring it within the Alpy's required range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I install the Shelyak ST8\/10 adapter on my SBIG camera?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eInstallation requires you to carefully remove the original front plate from your SBIG camera body. This adapter flange is then mounted in its place. This is a modification to your camera and should be done with care.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the biggest risk when using the ST8\/10 adapter with my Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary risk is optical damage during focusing. The adapter brings the Alpy's lens very close to the CCD window. You must focus slowly and carefully to avoid the two surfaces touching, which could scratch or crack the optics.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I want to capture the spectrum of Vega (Alpha Lyrae) with my SBIG ST8 and Alpy 600, is this adapter all I need?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter is the essential mechanical link between your SBIG ST8 and the Alpy 600. Once they are physically connected using this adapter, you will still need to mount the entire assembly to your telescope and proceed with standard spectroscopic acquisition procedures, including focusing and calibration.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Alpy 600 ST8\/10 adapter to connect my camera to other Shelyak spectroscopes like the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. This adapter is engineered exclusively for the Alpy 600 spectroscope. The backfocus requirements and mechanical interfaces for other spectroscopes, like the Lhires III, are different and require their own specific adapters.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy 600 Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCamera Compatibility\u003c\/td\u003e\n\u003ctd\u003eSBIG ST7, ST8, ST10, ST2000\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eFunction\u003c\/td\u003e\n\u003ctd\u003eCorrects mechanical backfocus for camera attachment\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eST8\/10 adapter for Alpy 600\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943042085149,"sku":"SHK-PU0149","price":139.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-ST8-10-adapter-for-Alpy-600-1_4bf08066-01f7-436f-8ae7-9e98ff2ba9ea.jpg?v=1789616187"},{"product_id":"shelyak-se0005","title":"Shelyak Grating module for the Lhires III - 2400 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eGrating Ruling: 2400 lines\/mm\u003c\/li\u003e\n\u003cli\u003eInstrument Compatibility: Shelyak Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003ePrimary Application: High-Resolution Spectroscopy\u003c\/li\u003e\n\u003cli\u003eFunction: Direct replacement for the standard Lhires III grating\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the Lhires III - 2400 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis is the standard, high-resolution grating module for the Shelyak Lhires III spectroscope, featuring a 2400 lines\/mm ruling. The Lhires III instrument is supplied from the factory with this 2400 l\/mm grating to deliver its maximum native resolving power.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe Standard 2400 l\/mm High-Resolution Grating for Lhires III\u003c\/h3\u003e\n\u003cp\u003eEngineered as the default optical component for the Lhires III, this 2400 lines\/mm grating module is the key to achieving the instrument's highest spectral resolution. It is designed for detailed analysis of stellar atmospheres, Be star emission lines, and other targets requiring fine spectral detail.\u003c\/p\u003e\n\u003cp\u003eThis module serves as a direct replacement for the original grating included with your Lhires III. While other complementary gratings are available to change the instrument's resolution for different applications, the 2400 l\/mm version remains the primary choice for high-resolution work.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary purpose of the 2400 l\/mm grating for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe \u003cstrong\u003e2400 lines\/mm grating\u003c\/strong\u003e is designed to provide the highest possible spectral resolution for the Lhires III spectroscope. It is intended for scientific applications where resolving fine details in a star's spectrum is critical, such as measuring doppler shifts or analyzing narrow emission and absorption lines.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this 2400 l\/mm grating an upgrade for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this is not an upgrade. The Shelyak Lhires III spectroscope is sold with the \u003cstrong\u003e2400 l\/mm grating module\u003c\/strong\u003e as its standard component. This product is a direct, factory-spec replacement for a lost or damaged original grating.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I need to replace the 2400 l\/mm grating on my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou would typically purchase this module only if the original grating that came with your Lhires III was damaged, degraded, or lost. Since it is the standard grating, this module ensures your instrument is restored to its original high-resolution capabilities.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 2400 l\/mm grating perform on a Be star like Gamma Cassiopeiae?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe high resolution of the \u003cstrong\u003e2400 l\/mm grating\u003c\/strong\u003e is ideal for studying Be stars like Gamma Cassiopeiae (γ Cas). It allows you to clearly resolve the double-peaked profile of the Hydrogen-alpha (Hα) emission line, which originates from the star's circumstellar disk. This level of detail is essential for monitoring V\/R (violet-to-red peak) variations and changes in the disk structure.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I use a lower-resolution grating instead of this 2400 l\/mm module for my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWhile the \u003cstrong\u003e2400 l\/mm grating\u003c\/strong\u003e provides maximum detail, it covers a very small spectral range. You should switch to a lower-resolution grating (e.g., 600 or 1200 l\/mm) when you need to:\n\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eCapture a wider wavelength range\u003c\/strong\u003e in a single exposure, such as when classifying star types.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eStudy faint objects\u003c\/strong\u003e like quasars or supernovae, where collecting more light over a broader band is more important than high resolution.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003ePerform initial surveys\u003c\/strong\u003e of targets before focusing on a specific spectral line with the high-resolution grating.\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs it difficult to install the 2400 l\/mm grating module in the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the grating modules for the Lhires III are designed to be user-interchangeable. The process involves opening the instrument cover and carefully swapping the modules. Refer to the official Lhires III user manual for detailed, step-by-step instructions to ensure proper handling and alignment.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943042412829,"sku":"SHK-SE0005","price":1035.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_90238cf8-88d4-4d27-85e3-f830bc715a3d.jpg?v=1789616196"},{"product_id":"shelyak-se0006","title":"Shelyak Grating module for the Lhires III - 1200 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e1200 lines\/mm Grating\u003c\/li\u003e\n\u003cli\u003eDirect-Fit Module for Lhires III\u003c\/li\u003e\n\u003cli\u003eExpands Spectrograph Wavelength Coverage\u003c\/li\u003e\n\u003cli\u003eIdeal for Spectroscopic Surveys\u003c\/li\u003e\n\u003cli\u003eInterchangeable with Standard Grating\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the Lhires III - 1200 l\/mm\u003c\/h2\u003e\n\u003cp\u003eSwap the standard 2400 l\/mm grating in your Shelyak Lhires III spectrograph for this 1200 lines\/mm module to trade high resolution for significantly broader spectral coverage in a single exposure. This module is an essential accessory for observers who need to characterize objects with unknown features or monitor phenomena across a wide spectral range, such as supernovae or comets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 1200 l\/mm Trade-Off: Broader Wavelength Coverage at Lower Resolution\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, a grating's line density dictates the trade-off between spectral resolution and wavelength coverage. A higher line count, like the Lhires III's standard 2400 l\/mm grating, spreads the light out more, delivering higher resolution over a smaller spectral window. This 1200 l\/mm grating does the opposite; with fewer lines, it produces a less dispersed spectrum, allowing a much wider range of wavelengths to fall onto your sensor in a single frame.\u003c\/p\u003e\n\u003cp\u003eThis capability is critical for survey work, initial classification of variable stars, or capturing the full profile of objects with broad emission lines. Instead of taking multiple exposures to piece together a spectrum, you can capture the entire visible range at once, saving valuable observing time.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e1200 l\/mm vs. 2400 l\/mm: Choosing the Right Grating for Your Target\u003c\/h3\u003e\n\u003cp\u003eThe standard 2400 l\/mm grating is the correct tool for the high-resolution work the Lhires III is famous for—measuring precise radial velocities, studying detailed line profiles of Be stars, or resolving close binary systems spectroscopically. It prioritizes detail over breadth.\u003c\/p\u003e\n\u003cp\u003eThe 1200 l\/mm grating module excels when the scientific goal is characterization rather than fine measurement. It is the superior choice for:\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eSupernova and Nova Spectroscopy:\u003c\/strong\u003e Capturing the evolution of multiple, broad spectral features (like Silicon II or Hydrogen lines) simultaneously as the object brightens and fades.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eQuasar and AGN Characterization:\u003c\/strong\u003e Identifying highly redshifted emission lines across a wide spectral range to determine the object's distance and nature.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eCometary Analysis:\u003c\/strong\u003e Observing molecular emission bands from species like C2 (Swan bands) which span a significant portion of the visible spectrum.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the 1200 l\/mm grating for my Lhires III over the standard 2400 l\/mm?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou would choose the \u003cstrong\u003e1200 l\/mm grating\u003c\/strong\u003e when your primary goal is to capture the widest possible range of wavelengths in a single exposure. The standard \u003cstrong\u003e2400 l\/mm grating\u003c\/strong\u003e provides higher resolution but covers a much narrower spectral window. The 1200 l\/mm module is for survey work and broad characterization, not fine detail analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of a lower-resolution grating like this 1200 l\/mm module for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe main advantage is \u003cstrong\u003eefficiency\u003c\/strong\u003e. For objects like supernovae, comets, or quasars, important spectral features can be spread far apart. The 1200 l\/mm grating allows you to capture all of them in one shot, saving time and simplifying data acquisition compared to creating a mosaic of multiple high-resolution exposures.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 1200 l\/mm grating module difficult to install in the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the Lhires III is designed for interchangeable grating modules. The process involves opening the access panel and carefully swapping the existing module with the new one. Always refer to your Lhires III manual for the specific procedure to avoid damaging the delicate grating surface.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I want to study the H-alpha line profile of Vega (Alpha Lyrae) with my Lhires III, is the 1200 l\/mm grating the right choice?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. For detailed analysis of a single, narrow spectral line like H-alpha, the standard \u003cstrong\u003e2400 l\/mm grating is the correct tool\u003c\/strong\u003e. Its higher resolution is necessary to reveal subtle shifts and profile changes. The 1200 l\/mm grating would show the line, but without the detail needed for scientific measurement of its profile.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI'm using my Lhires III on an 8\" SCT to monitor a supernova. Why is the 1200 l\/mm grating module a good tool for this?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eSupernovae exhibit broad, evolving spectral features across the entire visible spectrum. The \u003cstrong\u003e1200 l\/mm grating's\u003c\/strong\u003e wide spectral coverage is ideal for this task, as it allows you to capture the appearance and evolution of key features like the Silicon II (Si II) absorption line in Type Ia supernovae and the broad Hydrogen lines in Type II, all within a single frame.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes using the 1200 l\/mm grating module change the calibration process for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. You must perform a new spectral calibration after installing the 1200 l\/mm grating. The dispersion (angstroms per pixel) is different from the 2400 l\/mm grating, so your previous calibration files will no longer be accurate. You will need to create and save a new calibration profile for this specific setup.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Density\u003c\/td\u003e\n\u003ctd\u003e1200 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectrograph\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eApplication\u003c\/td\u003e\n\u003ctd\u003eLow Resolution, Wide Field Spectroscopy\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e1200 l\/mm Grating Module for Lhires III\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943042740509,"sku":"SHK-SE0006","price":1018.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_b61d3287-6af2-4150-ae9e-8b534d66107a.jpg?v=1789616204"},{"product_id":"shelyak-se0007","title":"Shelyak Grating module for the Lhires III - 600 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e\n\u003cstrong\u003eGrating Density:\u003c\/strong\u003e 600 lines\/mm\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eInstrument Compatibility:\u003c\/strong\u003e Shelyak Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003ePrimary Application:\u003c\/strong\u003e Low-resolution, wide-band spectroscopy\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eFunction:\u003c\/strong\u003e Expands the Lhires III's capabilities for observing faint, broad-emission objects\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the Lhires III - 600 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis 600 lines\/mm grating module fundamentally alters the capabilities of your Lhires III spectroscope, trading the high resolution of the standard 2400 l\/mm grating for significantly broader wavelength coverage in a single exposure. It transforms the Lhires III from a specialized high-resolution instrument into a more versatile tool for surveying a wider range of celestial targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe Core Trade-Off: Swapping Resolution for Broad Spectral Range\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, resolution and spectral range are inversely related. The standard 2400 l\/mm grating disperses light widely to resolve fine details, but can only capture a narrow slice of the spectrum. This 600 l\/mm grating module does the opposite, concentrating the spectrum to fit a much wider range of wavelengths onto your sensor at the expense of resolving power.\u003c\/p\u003e\n\u003cp\u003eThis lower dispersion makes the 600 l\/mm grating ideal for initial characterization of unknown objects or for studying phenomena that span the entire visible spectrum. It also increases throughput, delivering a brighter spectrum that is critical for faint targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eNew Targets for Your Lhires III: From Novae to Comets\u003c\/h3\u003e\n\u003cp\u003eBy prioritizing spectral range over detail, this module opens up new observational possibilities for the Lhires III. It allows you to effectively study objects with broad emission or absorption features that are difficult to analyze with a high-resolution grating.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eTransient Events:\u003c\/strong\u003e Capture the entire visible spectrum of a supernova or nova in a single shot to classify its type and evolution.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eComets:\u003c\/strong\u003e Analyze the broad emission bands from molecules like C2 (Swan bands) in a comet's coma.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eEmission Nebulae:\u003c\/strong\u003e Measure the relative intensities of key emission lines (like H-alpha, H-beta, and OIII) across a wide spectral range simultaneously.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e600 l\/mm vs. the Standard 2400 l\/mm Grating\u003c\/h3\u003e\n\u003cp\u003eChoosing the right grating depends entirely on your scientific goal. This 600 l\/mm module complements the stock grating, giving your Lhires III dual-mode capability.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003e600 l\/mm Grating (This Module):\u003c\/strong\u003e Best for low-resolution survey work, spectral classification, and observing faint, extended objects. It captures a wide spectral range, ideal for understanding the overall nature of a target.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003e2400 l\/mm Grating (Standard):\u003c\/strong\u003e Best for high-resolution studies of specific, narrow spectral lines. It is the tool for measuring precise Doppler shifts to determine stellar radial velocities or for analyzing the detailed profiles of absorption lines in bright stars.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main reason to use the 600 l\/mm grating in my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary reason is to capture a much \u003cstrong\u003ewider range of wavelengths\u003c\/strong\u003e in a single image. While the standard 2400 l\/mm grating provides very high resolution for studying fine details, this 600 l\/mm grating is designed for survey work, classifying objects like supernovae, or studying targets with broad emission features like comets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow will the 600 l\/mm grating change my Lhires III's view of a bright star like Vega (Alpha Lyrae)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWith the standard 2400 l\/mm grating, you might focus on the detailed shape of a single hydrogen line (like H-alpha) in Vega's spectrum. With the 600 l\/mm grating, you would see the entire Balmer series of hydrogen lines across the visible spectrum at once, along with Vega's overall spectral curve, but with much less detail in each individual line.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 600 l\/mm grating to study the spectrum of a comet?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an ideal application. Comets often show broad emission bands from various molecules. The 600 l\/mm grating allows you to capture these features across a wide spectral range, which is perfect for identifying the comet's chemical composition.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 600 l\/mm grating module difficult to install in the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the Lhires III was designed for interchangeable grating modules. The process is straightforward, allowing you to swap between high and low-resolution modes depending on your observing target for the night. Refer to the Lhires III manual for detailed instructions.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill this 600 l\/mm grating work with other spectroscopes besides the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis module is specifically designed and mounted for the Shelyak Lhires III spectroscope. It is not intended for use in other instruments due to its specific mechanical interface.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes lower resolution mean lower quality data with the 600 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNot at all. \"Resolution\" refers to the ability to separate closely spaced spectral lines. Lower resolution is a deliberate choice to achieve a different scientific goal—namely, wider spectral coverage. For tasks like classifying a supernova or measuring the overall color of an asteroid, the data from the 600 l\/mm grating is not only high quality but is the more appropriate choice.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Density\u003c\/td\u003e\n\u003ctd\u003e600 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eIntended Instrument\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolution Class\u003c\/td\u003e\n\u003ctd\u003eLow Resolution\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectral Coverage\u003c\/td\u003e\n\u003ctd\u003eWide Band\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e600 l\/mm Grating Module for Lhires III\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943043068189,"sku":"SHK-SE0007","price":1018.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_6e2fbb50-e60f-4907-985d-753b59101eb6.jpg?v=1789616212"},{"product_id":"shelyak-se0008","title":"Shelyak Grating module for the Lhires III - 300 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eGrating for Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003e300 lines\/mm Ruling\u003c\/li\u003e\n\u003cli\u003eProvides Lower Resolution and Wider Spectral Range\u003c\/li\u003e\n\u003cli\u003eComplements the Standard 2400 l\/mm Grating\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the Lhires III - 300 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Grating module for the Lhires III - 300 l\/mm is an optional component designed to trade the high resolution of the standard 2400 l\/mm grating for significantly broader spectral coverage in a single exposure. This 300 lines\/mm grating fundamentally alters the instrument's capabilities, making it suitable for analyzing entire spectral classes of stars or faint, extended objects where capturing the full spectrum is more critical than resolving fine absorption lines.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eFrom 2400 l\/mm to 300 l\/mm: Expanding Your Lhires III's Capabilities\u003c\/h3\u003e\n\u003cp\u003eThe Shelyak Lhires III spectroscope is supplied with a 2400 lines\/mm grating, engineered specifically for high-resolution studies of specific spectral features. This 300 l\/mm grating module offers the inverse capability, transforming your specialized instrument into a versatile survey tool.\u003c\/p\u003e\n\u003cp\u003eBy reducing the line count, the 300 l\/mm grating disperses light over a smaller angle, allowing a much wider range of wavelengths to fall onto your sensor at once. This trade-off is the core purpose of the module: sacrificing resolving power to gain spectral breadth.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eStandard 2400 l\/mm Grating:\u003c\/strong\u003e Delivers high resolution over a narrow spectral window. It is ideal for measuring the Doppler shift in a binary star's H-alpha line or studying the fine structure of a planetary nebula.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eOptional 300 l\/mm Grating:\u003c\/strong\u003e Provides lower resolution across a very wide spectral window. It is built for capturing the overall spectral energy distribution of an object, classifying a star's type, or monitoring a supernova's evolution across its entire visible spectrum.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eApplications for Low-Resolution Spectroscopy with the 300 l\/mm Grating\u003c\/h3\u003e\n\u003cp\u003eWith this module, your Lhires III becomes an ideal instrument for spectrophotometry and the study of faint targets. Capturing the spectrum of a dim comet, a distant quasar, or a faint nova becomes feasible, as the lower dispersion concentrates the object's faint light, increasing the signal-to-noise ratio per pixel.\u003c\/p\u003e\n\u003cp\u003eThis grating is also essential for spectral classification. To determine if a star is a hot, blue O-type or a cool, red M-type, you need to see the overall shape of its blackbody curve and the presence of broad absorption features. The 300 l\/mm grating allows you to capture this full \"fingerprint\" in a single frame, making it a powerful tool for stellar astrophysics projects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the 300 l\/mm grating for my Lhires III when it comes with a 2400 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou would choose the \u003cstrong\u003e300 l\/mm grating\u003c\/strong\u003e when your scientific goal requires a wide spectral range rather than high resolution. The standard 2400 l\/mm grating is for detailed study of narrow spectral lines, while the 300 l\/mm grating is for capturing the entire visible spectrum of an object at once, which is necessary for spectral classification or studying objects with broad emission features like novae and quasars.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of the 300 l\/mm Lhires III grating module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe main advantage is \u003cstrong\u003espectral coverage\u003c\/strong\u003e. It allows your Lhires III to capture a much wider range of wavelengths in a single exposure compared to the standard high-resolution grating. This makes it possible to analyze the overall energy distribution of a star or capture the full spectrum of faint, extended objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 300 l\/mm grating module for the Lhires III good for studying faint objects like comets?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, it is an excellent choice. Because the 300 l\/mm grating has a lower dispersion, it concentrates the faint light from objects like \u003cstrong\u003ecomets, faint novae, or distant galaxies\u003c\/strong\u003e more effectively on your camera's sensor. This results in a higher signal-to-noise ratio, making it easier to obtain a usable spectrum from challenging targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 300 l\/mm grating affect the spectrum I can capture with my Lhires III and an 8\" SCT?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWith an \u003cstrong\u003e8\" SCT\u003c\/strong\u003e, the 300 l\/mm grating will allow your Lhires III to function as a powerful survey and classification instrument. You will be able to capture the entire visible spectrum of moderately bright stars in a single shot, allowing you to classify them based on their overall spectral features (e.g., O, B, A, F, G, K, M types). This is a task that would be impossible with the narrow-band view of the standard 2400 l\/mm grating.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 300 l\/mm grating for spectral classification of stars like Vega (Alpha Lyrae)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAbsolutely. The 300 l\/mm grating is perfect for this application. For a star like \u003cstrong\u003eVega (Alpha Lyrae)\u003c\/strong\u003e, an A0V-class star, this grating will allow you to easily capture the prominent, broad absorption lines of the Balmer series (Hydrogen-alpha, beta, gamma, etc.) that define its spectral type, all within a single image.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs swapping the grating in the Lhires III difficult?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe grating module is designed for user installation, allowing you to switch between resolutions based on your observing targets for the night. While the process is straightforward, it requires care to avoid damaging the optical components. We strongly recommend consulting the official \u003cstrong\u003eLhires III user manual\u003c\/strong\u003e for detailed, step-by-step instructions before changing the grating.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Ruling\u003c\/td\u003e\n\u003ctd\u003e300 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e300 l\/mm Grating Module for Lhires III\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943043395869,"sku":"SHK-SE0008","price":1018.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_bfdfdc51-9b7a-4e59-9b7a-94c104a85295.jpg?v=1789616219"},{"product_id":"shelyak-se0009","title":"Shelyak Grating module for the Lhires III - 150 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e150 lines\/mm Grating\u003c\/li\u003e\n\u003cli\u003eLow Resolution \/ Wide Spectral Range\u003c\/li\u003e\n\u003cli\u003eDesigned for the Shelyak Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003eEnables Faint Object Spectroscopy\u003c\/li\u003e\n\u003cli\u003eUser-Interchangeable Module\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the Lhires III - 150 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis 150 lines\/mm grating module transforms the Shelyak Lhires III from a specialized high-resolution instrument into a versatile survey spectroscope. By replacing the standard 2400 l\/mm grating, you dramatically lower the dispersion to capture a much wider spectral range in a single exposure, opening up new targets for scientific analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eSurvey Mode for the Lhires III: The 150 l\/mm Advantage\u003c\/h3\u003e\n\u003cp\u003eThe core purpose of the Lhires III is high-resolution spectroscopy, but this requires bright targets and isolates a very narrow slice of the spectrum. The 150 l\/mm grating module intentionally trades that high resolution for a massive increase in spectral bandwidth and throughput, allowing you to analyze faint, extended, or continuum-source objects that are inaccessible with the standard grating.\u003c\/p\u003e\n\u003cp\u003eThis makes the 150 l\/mm module the ideal tool for rapid classification of transient events like supernovae and novae, studying the broad emission features of comets, or capturing the full visible spectrum of faint deep-sky objects. It effectively adds a \"survey mode\" to your Lhires III, expanding its research capabilities significantly.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e150 l\/mm vs. 2400 l\/mm: Choosing the Right Grating for Your Target\u003c\/h3\u003e\n\u003cp\u003eSelecting the correct grating is critical for matching the instrument to your scientific goals. The two options serve fundamentally different purposes.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eStandard 2400 l\/mm Grating:\u003c\/strong\u003e This is for high-resolution work on bright stars. Use it to detect the subtle Doppler shifts in binary star systems, analyze the fine absorption lines in a stellar atmosphere (like the Sodium D-lines), or measure precise radial velocities. Its spectral range is very narrow.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003e150 l\/mm Grating Module:\u003c\/strong\u003e This is for low-resolution \"big picture\" spectroscopy. Use it to obtain a spectrum of a faint comet, classify a supernova by its broad spectral features, or monitor the spectral evolution of a variable star across the entire visible range at once.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main application for the Shelyak 150 l\/mm grating module for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary application is for low-resolution spectroscopy of faint or transient objects. It allows you to capture a wide spectral range in a single shot, which is essential for classifying objects like supernovae, analyzing the broad emission bands of comets, or studying faint nebulae.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 150 l\/mm grating change the data I can collect with my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIt fundamentally changes the trade-off between spectral resolution and wavelength coverage. Instead of a very detailed view of a tiny part of the spectrum (like with the standard 2400 l\/mm grating), the \u003cstrong\u003e150 l\/mm grating\u003c\/strong\u003e provides a lower-detail view of a much wider portion of the spectrum. This is better for understanding the overall nature of an object rather than its fine atmospheric details.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need to recalibrate my Lhires III when I switch to the 150 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. Any time you change the grating in a spectroscope, you must perform a new wavelength calibration. The dispersion, or how much the light is spread out per pixel, is completely different for the 150 l\/mm grating compared to the standard 2400 l\/mm grating. You will need to take new calibration frames with a reference lamp.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 150 l\/mm grating suitable for classifying a newly discovered supernova like SN 2023ixf with an 11\" SCT?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an ideal use case. An 11\" SCT provides enough light-gathering power, and the \u003cstrong\u003e150 l\/mm grating\u003c\/strong\u003e provides the wide spectral coverage needed to identify the characteristic broad absorption lines (like Silicon II for a Type Ia) used for supernova classification. The standard 2400 l\/mm grating would be unsuitable for this task as it would only show a tiny, unidentifiable fraction of the spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 150 l\/mm grating to study the changing tail composition of Comet C\/2022 E3 (ZTF)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis is another excellent application. Cometary spectra are dominated by broad emission bands from molecules like C2 (the Swan bands) and CN. The \u003cstrong\u003e150 l\/mm grating\u003c\/strong\u003e allows you to capture all these features simultaneously to monitor how the comet's outgassing and composition evolve as it approaches and leaves the sun.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I use the standard 2400 l\/mm grating instead of this 150 l\/mm module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou should use the standard \u003cstrong\u003e2400 l\/mm grating\u003c\/strong\u003e when your scientific goal requires very high spectral resolution for bright targets. This includes measuring precise radial velocity shifts from stellar wobble, studying the detailed profiles of spectral lines in Be stars, or resolving close spectroscopic binaries.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943043690781,"sku":"SHK-SE0009","price":1018.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_4dbbeda5-5e16-4f2e-800a-130d89ab377d.jpg?v=1789616227"},{"product_id":"shelyak-se0012","title":"Shelyak Lhires III adapter set (23 mm camera)","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConnects cameras to the Shelyak Lhires III spectroscope\u003c\/li\u003e\n\u003cli\u003eDesigned for cameras with a backfocus between 21.35 mm and 25.35 mm\u003c\/li\u003e\n\u003cli\u003eOptimized for common camera backfocus distances around 23 mm\u003c\/li\u003e\n\u003cli\u003eProvides a rigid, secure connection for precise sensor alignment\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLhires III adapter set (23 mm camera)\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Lhires III adapter set for 23 mm cameras enables you to mount a camera with a native backfocus between 21.35 mm and 25.35 mm to your Lhires III spectroscope, ensuring the sensor is positioned at the precise focal plane required for high-resolution spectroscopy.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003ePrecision Mounting for Cameras with 21.35mm to 25.35mm Backfocus\u003c\/h3\u003e\n\u003cp\u003eThis adapter is the critical link between your Lhires III spectroscope and a camera with a backfocus in the 21.35 mm to 25.35 mm range. Achieving the correct spacing is non-negotiable in spectroscopy, and this component creates a rigid, repeatable connection for accurate data acquisition.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eTargeted Compatibility:\u003c\/strong\u003e Specifically engineered for the Lhires III, this adapter solves the mounting problem for a popular class of cameras, such as those with a nominal backfocus of 23 mm.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eSimplified Integration:\u003c\/strong\u003e By using this adapter, you eliminate the need for custom-machined parts or unstable stacks of generic extenders, securing your camera directly to the spectroscope's optical path.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the Lhires III adapter set for 23 mm cameras?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter connects a camera with a specific backfocus range (21.35 mm to 25.35 mm) to a Shelyak Lhires III spectroscope. It ensures the camera sensor is placed at the correct distance from the spectroscope's optics for a sharp spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhich cameras are compatible with this Lhires III adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAny camera with a native backfocus that falls between \u003cstrong\u003e21.35 mm and 25.35 mm\u003c\/strong\u003e can be used with this adapter. While the title refers to \"23 mm cameras,\" it supports the full specified range. You must confirm your camera's backfocus before purchasing.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need this specific Lhires III adapter for my spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou need this adapter only if your imaging camera has a backfocus within the 21.35 mm to 25.35 mm range. Shelyak offers different adapters for cameras with other backfocus distances, such as standard 17.5 mm C-mount cameras.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does this Lhires III adapter ensure I get a good spectrum of a star like Vega (Alpha Lyrae)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eBy precisely setting the camera distance, this adapter guarantees that the light from Vega passing through the Lhires III slit and grating forms a sharply focused spectrum on your sensor. Incorrect spacing would result in blurred spectral lines, making it impossible to measure features like the Balmer absorption lines accurately.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this Lhires III adapter with a standard DSLR on my f\/8 refractor?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIt is highly unlikely. Most DSLRs have a much longer backfocus (typically 44 mm for Canon EF or 46.5 mm for Nikon F-mount) and would not be compatible with this adapter. This adapter is designed for dedicated astronomy cameras that fall within the 21.35 mm to 25.35 mm range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this adapter difficult to install on the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eInstallation is straightforward. The adapter is designed to thread or bolt directly onto the Lhires III's camera port, providing a secure mechanical and optical interface for your camera.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatible Spectroscope\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRequired Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e21.35 mm to 25.35 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eLhires III adapter set (23 mm camera)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943043952925,"sku":"SHK-SE0012","price":171.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Lhires-III-adapter-set-23-mm-camera-1_6e4d4cf1-fcda-4c9a-816a-590b4451e658.jpg?v=1789616236"},{"product_id":"shelyak-se0014","title":"Shelyak Adapter set for Lhires III (camera with backfocus 17 mm)","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConnects cameras with 17 mm backfocus to a Lhires III spectrograph\u003c\/li\u003e\n\u003cli\u003eEnsures precise sensor-to-spectrograph spacing\u003c\/li\u003e\n\u003cli\u003eCritical for achieving optimal spectral focus and resolution\u003c\/li\u003e\n\u003cli\u003eDesigned specifically for the Shelyak Lhires III\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eAdapter set for Lhires III (camera with backfocus 17 mm)\u003c\/h2\u003e\n      \u003cp\u003eThis Shelyak adapter set is the essential component for coupling a camera with a specific 17 mm backfocus to the Lhires III spectrograph. Achieving this exact 17 mm spacing is not optional; it is the fundamental requirement for placing the camera sensor at the precise focal plane of the spectrograph's optical system, ensuring your spectra are sharply focused from one end to the other.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eAchieving Critical 17 mm Spacing for the Lhires III\u003c\/h3\u003e\n      \u003cp\u003eIn high-resolution spectroscopy, focus is paramount. The Lhires III is designed with a specific focal plane, and this adapter set ensures your camera's sensor lands exactly on it. Using the correct adapter for your camera's 17 mm backfocus eliminates vignetting and image degradation, producing clean, scientifically valid data for stellar classification, radial velocity measurements, or emission line analysis.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is this Shelyak adapter set for the Lhires III used for?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThis adapter set is designed to physically connect a camera with a \u003cstrong\u003e17 mm backfocus\u003c\/strong\u003e to the Shelyak Lhires III spectrograph. Its primary purpose is to establish the precise, rigid spacing required for the camera's sensor to be at the spectrograph's focal plane.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhy is the 17 mm backfocus specification so important for the Lhires III?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eSpectrographs like the Lhires III have a fixed optical design with a very specific focal plane. If the camera sensor is too close or too far away, the resulting spectrum will be out of focus, blurred, and unusable for scientific analysis. This adapter guarantees the correct \u003cstrong\u003e17 mm distance\u003c\/strong\u003e is maintained.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this adapter set for a camera with a different backfocus, like 13 mm, on my Lhires III?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eNo. This adapter set is machined specifically for cameras that have a native backfocus of \u003cstrong\u003e17 mm\u003c\/strong\u003e. Using it with a camera that has a different backfocus will result in an incorrect sensor position and poorly focused spectra. You must use the adapter set that matches your camera's backfocus.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhich cameras are compatible with this Lhires III adapter set?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eAny astronomical camera that has a native backfocus of \u003cstrong\u003e17 mm\u003c\/strong\u003e is compatible with this adapter set. It is crucial to check your camera's technical specifications to confirm its backfocus distance before purchasing an adapter.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIf I use this 17 mm adapter with my Lhires III on an 8\" SCT to observe Vega (Alpha Lyrae), what is the goal?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe goal is to obtain a high-resolution spectrum of Vega, a type A0V star. This adapter ensures your camera is perfectly focused to capture the distinct hydrogen Balmer absorption lines (like H-alpha and H-beta) in Vega's atmosphere. Precise focus is critical for measuring the width and depth of these lines, which is a key part of stellar classification.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I install this adapter set on my Lhires III spectrograph?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eInstallation typically involves threading the components of the adapter set onto the camera port of the Lhires III and then attaching your camera to the other side. For detailed instructions, you should refer to the main user manual for the Shelyak Lhires III spectrograph, as the adapter is a component of that system.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003ctable class=\"DAV-specifications\"\u003e\n    \u003ctbody\u003e\n      \u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectrograph\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eRequired Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e17 mm\u003c\/td\u003e\n\u003c\/tr\u003e\n    \u003c\/tbody\u003e\n  \u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cul class=\"DAV-grid\"\u003e\n    \u003cli class=\"DAV-grid-item\"\u003e\n      \u003cdiv\u003e\n        \u003cp class=\"DAV-item-title\"\u003eAdapter Set for Lhires III (17 mm Backfocus)\u003c\/p\u003e\n        \u003cp class=\"DAV-item-subtitle\"\u003eComponents as required\u003c\/p\u003e\n      \u003c\/div\u003e\n    \u003c\/li\u003e\n  \u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943044247837,"sku":"SHK-SE0014","price":171.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Adapter-set-for-Lhires-III-camera-with-backfocus-17-mm-1_4645ba94-e147-42ae-9cb3-95b72ff04884.jpg?v=1789616244"},{"product_id":"shelyak-se0080","title":"Shelyak Adapter set for Lhires III (camera with 25mm backfocus)","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eCompatibility: Shelyak Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003eRequired Camera Backfocus: 23.35mm to 27.35mm\u003c\/li\u003e\n\u003cli\u003eEnsures Precise Sensor-to-Optics Spacing\u003c\/li\u003e\n\u003cli\u003eCritical for High-Resolution Spectroscopy\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAdapter set for Lhires III (camera with 25mm backfocus)\u003c\/h2\u003e\n\u003cp\u003eThis adapter set for the Shelyak Lhires III spectroscope provides the precise mechanical connection for cameras that require a backfocus between 23.35mm and 27.35mm, ensuring the sensor is positioned correctly at the focal plane for high-resolution spectroscopy.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003ePrecise Spacing for Lhires III: The 23.35mm to 27.35mm Backfocus Solution\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, achieving perfect focus is paramount. This adapter set is engineered to solve the specific backfocus challenge for cameras in the 23.35mm to 27.35mm range, positioning the sensor precisely where the Lhires III forms its spectrum. This specificity is its strength, but also its limitation: it is not a universal adapter and will only work for cameras within this exact window.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eCritical for Resolution:\u003c\/strong\u003e Without this exact spacing, spectral lines will appear blurred, compromising the resolution and scientific value of your data by destroying the sharpness of emission and absorption lines.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eEliminates Guesswork:\u003c\/strong\u003e Provides a rigid, repeatable connection that removes a major variable from your optical train, allowing you to focus on data acquisition.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eDesigned for Lhires III:\u003c\/strong\u003e Mates seamlessly with the spectroscope's optical output, maintaining the alignment necessary for accurate results.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat cameras are compatible with this Shelyak Lhires III adapter set?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter set is designed for any camera, typically a CCD or CMOS model, that has a native backfocus distance between \u003cstrong\u003e23.35mm and 27.35mm\u003c\/strong\u003e. You must check your camera's technical specifications to confirm its backfocus before purchasing this adapter.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy is a specific backfocus adapter like this needed for the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Shelyak Lhires III spectroscope has a fixed focal plane where the spectrum is formed. This adapter ensures the camera's sensor is placed exactly at that plane. Incorrect spacing results in a defocused spectrum, which blurs spectral lines and makes the data unusable for scientific analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this Lhires III adapter if my camera's backfocus is outside the 23.35mm to 27.35mm range?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this adapter set is not suitable for cameras outside the specified 23.35mm to 27.35mm backfocus range. Using it would prevent you from reaching proper focus. Shelyak offers different adapter sets for cameras with other backfocus requirements.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI'm trying to capture the spectrum of Vega (Alpha Lyrae) with my Lhires III. Will this adapter work with a camera that has a 25mm backfocus?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. A camera with a 25mm backfocus falls perfectly within the 23.35mm to 27.35mm range of this adapter set. It will provide the correct spacing to achieve a sharp, high-resolution spectrum of bright stars like Vega with your Lhires III.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I'm studying the H-alpha emission line of a nebula with the Lhires III, how does this adapter help?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eBy ensuring your camera sensor is perfectly focused, this adapter allows the Lhires III to resolve fine details within the H-alpha emission profile. Precise focus is critical for detecting subtle Doppler shifts or structural changes in the emission line, which would be lost with incorrect spacing.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this the only part I need to connect my camera to the Lhires III spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter set provides the correct backfocus spacing. However, you must also ensure that your camera's body has the appropriate mechanical threads to connect to the adapter itself. Please verify the thread type on both your camera and the Lhires III's output before assembly.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRequired Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e23.35mm to 27.35mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eAdapter set for Lhires III (25mm Backfocus)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943044608285,"sku":"SHK-SE0080","price":171.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Adapter-set-for-Lhires-III-camera-with-25mm-backfocus-1_aa8a58b1-29c1-4b4d-86a5-0b8edcc97e35.jpg?v=1789616252"},{"product_id":"shelyak-se0082","title":"Shelyak Adapter set for Lhires III (camera backfocus 34mm)","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConnects CCD\/CMOS cameras to a Shelyak Lhires III spectroscope\u003c\/li\u003e\n\u003cli\u003eEngineered for a nominal camera backfocus of 34mm\u003c\/li\u003e\n\u003cli\u003eAccommodates a backfocus range from 32.85mm to 36.85mm\u003c\/li\u003e\n\u003cli\u003eEnsures correct sensor placement for optimal spectral resolution\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAdapter set for Lhires III (camera backfocus 34mm)\u003c\/h2\u003e\n\u003cp\u003eThis adapter set is engineered specifically for the Shelyak Lhires III spectroscope, enabling you to mount a camera with a backfocus between 32.85mm and 36.85mm. Achieving this precise 34mm nominal spacing is critical for maintaining the spectroscope's optical resolution and preventing blurred spectral lines.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003ePrecision Spacing: Achieving the Critical 34mm Backfocus for Lhires III\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, sensor placement is not flexible. The optical design of the Lhires III demands that the camera sensor sits at a precise distance to record a sharp, well-resolved spectrum. This adapter set eliminates the guesswork and custom machining required to connect cameras that have a native backfocus in the 34mm range.\u003c\/p\u003e\n\u003cp\u003eIf your camera's sensor-to-flange distance falls between 32.85mm and 36.85mm, this set provides the exact mechanical interface needed for a rigid, perfectly spaced connection to your Lhires III. This ensures that the only variable you need to manage is focus, not component spacing.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of this Lhires III adapter set?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis adapter set is designed to securely mount a camera onto a Shelyak Lhires III spectroscope, ensuring the camera's sensor is positioned at the correct optical distance. It is specifically made for cameras that have a native backfocus between \u003cstrong\u003e32.85mm and 36.85mm\u003c\/strong\u003e.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy is the 34mm backfocus so important for the Lhires III spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Lhires III's optical system is designed to form a sharp spectrum at a very specific focal plane. If the camera sensor is too close or too far, spectral lines will appear blurred and the instrument's resolving power will be compromised. This adapter guarantees the \u003cstrong\u003ecritical 34mm nominal spacing\u003c\/strong\u003e is achieved.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I know if my camera is compatible with this Lhires III adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eCheck your camera's technical documentation for its backfocus, sometimes called \"sensor to flange distance.\" If this value is within the \u003cstrong\u003e32.85mm to 36.85mm range\u003c\/strong\u003e, this adapter is the correct solution for connecting it to your Lhires III.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this adapter set with a spectroscope other than the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. This adapter set is custom-designed for the specific mechanical threads and required focal distance of the Shelyak Lhires III spectroscope. It is not compatible with other instruments.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI have a planetary camera with 12.5mm of backfocus. Will this adapter work with my Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this adapter will not work. It is designed for cameras with a much longer native backfocus of around 34mm. To use a camera with 12.5mm of backfocus, you would need a different solution involving extension tubes to make up the distance difference.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I use this adapter with my Lhires III to study the spectrum of Vega (Alpha Lyrae), will it ensure correct focus?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Provided your camera's backfocus is within the specified 32.85mm to 36.85mm range, this adapter places the sensor at the correct plane. This allows you to achieve a sharply focused spectrum of bright stellar targets like Vega, which is essential for detailed analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Lhires III Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRequired Camera Backfocus\u003c\/td\u003e\n\u003ctd\u003e32.85mm to 36.85mm (34mm nominal)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eLhires III Adapter Set for 34mm Backfocus\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943045067037,"sku":"SHK-SE0082","price":171.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Adapter-set-for-Lhires-III-camera-backfocus-34mm-1_5818606c-89a6-41f3-98ef-d430dd8b7c7f.jpg?v=1789616261"},{"product_id":"shelyak-se0096","title":"Shelyak LISA Near-Infrared Conversion Kit","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eExtends Spectral Range to 650-1000nm\u003c\/li\u003e\n\u003cli\u003eOptimized for Near-Infrared (NIR) Spectroscopy\u003c\/li\u003e\n\u003cli\u003eReplaces Camera Ring to Correct NIR Chromatism\u003c\/li\u003e\n\u003cli\u003eAdds an Order Filter to Prevent Spectral Overlap\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLISA Near-Infrared Conversion Kit\u003c\/h2\u003e\n\u003cp\u003eTransform your Shelyak LISA spectrograph's standard visible range of 400-700nm for near-infrared work, extending its reach to 1000nm with this dedicated conversion kit. By re-calibrating the optical path for the 650-1000nm band, you gain access to the spectral signatures of cooler stars and other phenomena with prominent features beyond the visible spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eExtend Your LISA's Range to 1000nm for Near-Infrared Spectroscopy\u003c\/h3\u003e\n\u003cp\u003eThe standard LISA spectrograph is engineered for high-resolution analysis in the visible spectrum from 400-700nm. This kit modifies the instrument to perform in the near-infrared, shifting its optimized operational window to cover the 650-1000nm range. This conversion allows you to investigate the spectral features of M-type stars, carbon stars, and Be stars with prominent lines in the near-IR.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCorrecting IR Artifacts from 650nm to 1000nm\u003c\/h3\u003e\n\u003cp\u003eA successful conversion to near-infrared requires specific optical corrections. Two critical components achieve this: a new, angled camera ring corrects for chromatism inherent to longer wavelengths, while an included order filter prevents the overlapping of spectral orders to ensure clean, unambiguous data. Please note that the manufacturer describes the installation as a meticulous operation requiring time and precision, intended for users comfortable making fine adjustments to their equipment.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary function of the Shelyak LISA near infrared kit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis kit's function is to convert a standard Shelyak LISA spectrograph, originally designed for the visible spectrum (\u003cstrong\u003e400-700nm\u003c\/strong\u003e), into an instrument optimized for near-infrared spectroscopy in the \u003cstrong\u003e650-1000nm\u003c\/strong\u003e range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the LISA NIR kit adapt the spectrograph for infrared light?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe kit modifies the optical path in two key ways. It replaces the standard camera ring with an angled one to correct for chromatic aberration in the near-infrared, and it adds an order filter to eliminate spectral order overlap, which can contaminate data at these wavelengths.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I use this LISA NIR kit, can I still observe H-alpha at 656nm?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. The converted instrument's optimized range begins at \u003cstrong\u003e650nm\u003c\/strong\u003e, placing the critical Hydrogen-alpha emission line at 656.3nm well within its observational capability. Your LISA will remain a powerful tool for studying objects with strong H-alpha signatures.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat astronomical targets are ideal for a LISA spectrograph in the 650-1000nm range?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis range is excellent for studying cooler stars like M-type red dwarfs and carbon stars, which exhibit strong molecular absorption bands (e.g., Titanium Oxide) in the near-IR. It is also ideal for observing the Paschen series of hydrogen lines in the spectra of Be stars.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the installation of the LISA near infrared kit difficult?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe manufacturer states that the conversion is a \"meticulous operation, requiring time and precision.\" This kit is recommended for users who are confident in their ability to make precise mechanical adjustments to sensitive optical instruments. It is not a quick, field-swappable accessory.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I easily switch my LISA back to the visible range after this conversion?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe conversion is not designed for rapid or frequent changes between visible and NIR configurations. Reverting the LISA spectrograph back to its original 400-700nm visible-light optimization would require a full reversal of the meticulous installation process.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpecifications\u003c\/td\u003e\n\u003ctd\u003eThere are no specifications available for this product.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n    \u003cli class=\"DAV-grid-item\"\u003e\n      \u003cdiv\u003e\n        \u003cp class=\"DAV-item-title\"\u003eNo contents list available for this product.\u003c\/p\u003e\n      \u003c\/div\u003e\n    \u003c\/li\u003e\n  \u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_LISA_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak LISA Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943045493021,"sku":"SHK-SE0096","price":1201.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-LISA-near-infrared-kit-1_ed951e99-a699-4581-82cb-f5b16b2a5577.jpg?v=1789616269"},{"product_id":"shelyak-se0103","title":"Shelyak LISA Calibration Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eIntegrates with the Shelyak LISA Spectroscope\u003c\/li\u003e\n\u003cli\u003eInternal Halogen Lamp for Flat-Field Correction\u003c\/li\u003e\n\u003cli\u003eInternal Argon-Neon (Ar-Ne) Lamp for Wavelength Calibration\u003c\/li\u003e\n\u003cli\u003eDual 12V DC Power Inputs for Independent Lamp Control\u003c\/li\u003e\n\u003cli\u003eEnables Fully Remote Calibration Sequences\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLISA Calibration Module\u003c\/h2\u003e\n\u003cp\u003eThe LISA Calibration Module adds essential remote capabilities to your LISA spectroscope, incorporating two internal lamps—a halogen flat lamp and an Argon-Neon calibration lamp. Power is supplied via two separate 12V inputs using standard 5.5\/2.5mm center-positive connectors, allowing for independent, automated control of your entire calibration sequence from a remote location.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAutomated Flats and Wavelength Calibration for the LISA\u003c\/h3\u003e\n\u003cp\u003eThis single module provides both sources required for professional-grade spectroscopic calibration. The internal halogen lamp produces a uniform, continuous spectrum, allowing you to create flat-field frames that correct for dust, vignetting, and pixel-to-pixel variations in your imaging sensor. The Argon-Neon (Ar-Ne) lamp produces a spectrum with well-defined emission lines at known wavelengths, providing the precise reference needed to accurately calibrate your data's wavelength scale.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eDesigned for Remote Observatories with Dual 12V Inputs\u003c\/h3\u003e\n\u003cp\u003eThe key advantage of the LISA Calibration Module is its suitability for remote, unattended operation. It features two distinct 12V DC inputs, one for each lamp, enabling you to connect them to a relay box or switched power supply. This separation allows your automation software to trigger each lamp independently, running a full calibration routine—flats and wavelength references—without any manual intervention at the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the two lamps in the LISA calibration module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe LISA calibration module contains two essential lamps for spectroscopy. The \u003cstrong\u003ehalogen lamp\u003c\/strong\u003e provides a smooth, continuous light source for taking flat-field frames, which correct for optical imperfections and sensor variations. The \u003cstrong\u003eArgon-Neon (Ar-Ne) lamp\u003c\/strong\u003e produces a spectrum with sharp, known emission lines, used to accurately calibrate the wavelength scale of your scientific data.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the LISA calibration module enable remote observations?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe module features two separate 12V power inputs, one for each lamp. This allows you to connect each lamp to an independent channel on a remote power switch or relay box. Your observatory automation software can then turn each lamp on and off in sequence to acquire calibration frames without you needing to be physically present at the telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need two separate power outputs for the LISA calibration module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, for automated remote operation, you need two independently switchable 12V DC outputs. This allows your software to trigger the halogen lamp for flats and the Ar-Ne lamp for wavelength calibration as separate steps in a sequence. Using a single output would require you to manually swap the power cable between inputs.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of power supply do I need for the LISA calibration module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou will need a 12V DC power source capable of supplying two outputs. The connectors on the module are 5.5 \/ 2.5mm barrel jacks with a center-positive polarity. These are common connectors for astronomical equipment, but power supplies are not included.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I'm studying the spectrum of Vega (Alpha Lyrae) with my C11 and LISA, how do I use the LISA calibration module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIn a typical workflow, after acquiring the spectrum of Vega, you would use automation software to trigger the LISA calibration module. First, it would turn on the halogen lamp to take several flat-field frames. Then, it would switch to the Argon-Neon lamp to record a wavelength calibration spectrum. These two calibration files are then used in software like Demetra to process your raw data of Vega into a scientifically accurate spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy do I need to take flat frames with my LISA spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFlat frames are crucial for high-precision spectroscopy. They record the response of your entire optical system—including dust on the sensor or slit, and pixel-to-pixel sensitivity variations. By dividing your science image by a master flat, you remove these instrumental artifacts, ensuring that the spectral features you measure are from your astronomical target, not your equipment.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak LISA Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eFlat Lamp Type\u003c\/td\u003e\n\u003ctd\u003eHalogen\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCalibration Lamp Type\u003c\/td\u003e\n\u003ctd\u003eArgon-Neon (Ar-Ne)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003ePower Input\u003c\/td\u003e\n\u003ctd\u003e2x 12V DC\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eConnector Type\u003c\/td\u003e\n\u003ctd\u003e5.5 \/ 2.5mm, Center-Positive\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eLISA Calibration Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943045755165,"sku":"SHK-SE0103","price":679.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-LISA-calibration-module-1_26d9aa25-a5ec-4a83-98d1-77f0001bde3f.jpg?v=1789616277"},{"product_id":"shelyak-se0121","title":"Shelyak Grating module for the Lhires III - 1800 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e\n\u003cstrong\u003eGrating Ruling:\u003c\/strong\u003e 1800 lines\/mm\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eCompatibility:\u003c\/strong\u003e Shelyak Lhires III Spectroscope\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eFunction:\u003c\/strong\u003e Alternative module to change native resolution\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eUse Case:\u003c\/strong\u003e Wider spectral coverage at lower resolution\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eGrating module for the Lhires III - 1800 l\/mm\u003c\/h2\u003e\n      \u003cp\u003eThis interchangeable grating module provides a ruling of 1800 lines\/mm, specifically designed to alter the native high-resolution capabilities of the Shelyak Lhires III spectroscope. It allows you to trade the maximum resolving power of the standard 2400 l\/mm grating for a significantly wider spectral window in a single exposure.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eThe 1800 l\/mm Grating: Trading Resolution for Spectral Range\u003c\/h3\u003e\n      \u003cp\u003eIn spectroscopy, there is a fundamental trade-off between resolution and spectral coverage. This 1800 l\/mm grating module for the Lhires III is engineered for situations where capturing a broader range of wavelengths is more critical than achieving the highest possible resolution. By decreasing the line density from the standard 2400 l\/mm, this grating disperses light less, fitting more of the spectrum onto your camera sensor.\u003c\/p\u003e\n      \u003cp\u003eThis makes the 1800 l\/mm grating ideal for analyzing objects with broad emission or absorption features, such as supernovae (SNe), comets, or cataclysmic variable stars. It's the right choice when the scientific goal is classification or monitoring changes across a wide spectral range, rather than measuring the precise radial velocity of a single spectral line.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eLhires III 1800 l\/mm vs. Standard 2400 l\/mm Grating\u003c\/h3\u003e\n      \u003cp\u003eThe Lhires III spectroscope ships with a 2400 l\/mm grating, which is optimized for high-resolution studies of specific, narrow spectral regions. This alternate 1800 l\/mm module extends the instrument's capabilities, turning it into a more adaptable research tool.\u003c\/p\u003e\n      \u003cul\u003e\n        \u003cli\u003e\n\u003cstrong\u003eStandard 2400 l\/mm Grating:\u003c\/strong\u003e Use this for maximum resolving power. It excels at splitting close binary star lines, measuring the Doppler shift in stellar spectra, or studying the fine structure of nebular emission lines like H-alpha and OIII.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003eOptional 1800 l\/mm Grating:\u003c\/strong\u003e Choose this module for survey work or for targets where context is key. It allows you to capture, for example, the H-alpha, H-beta, and H-gamma lines of a Be star in a single frame, something not possible with the higher-resolution grating.\u003c\/li\u003e\n      \u003c\/ul\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the 1800 l\/mm grating for my Lhires III instead of the standard 2400 l\/mm?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYou would choose the \u003cstrong\u003e1800 l\/mm grating\u003c\/strong\u003e when your primary goal is to capture a wider range of wavelengths in a single exposure. The standard \u003cstrong\u003e2400 l\/mm grating\u003c\/strong\u003e offers higher resolution but sees a smaller piece of the spectrum. The 1800 l\/mm module is for applications like classifying supernovae or studying comets, where broad spectral features are more important than resolving fine details.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat astronomical targets are best for the Lhires III with the 1800 l\/mm grating?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe 1800 l\/mm grating is ideal for targets with broad or multiple, widely-spaced spectral features. Good examples include:\u003c\/p\u003e\n    \u003cul\u003e\n      \u003cli\u003e\n\u003cstrong\u003eSupernovae (SNe):\u003c\/strong\u003e For classification based on broad silicon or hydrogen absorption lines.\u003c\/li\u003e\n      \u003cli\u003e\n\u003cstrong\u003eComets:\u003c\/strong\u003e To capture multiple molecular emission bands (like C2) simultaneously.\u003c\/li\u003e\n      \u003cli\u003e\n\u003cstrong\u003eBe Stars:\u003c\/strong\u003e To observe the profile of hydrogen Balmer lines (H-alpha, H-beta, etc.) in one frame.\u003c\/li\u003e\n      \u003cli\u003e\n\u003cstrong\u003eVariable Stars:\u003c\/strong\u003e For general spectrophotometry across a wide passband.\u003c\/li\u003e\n    \u003c\/ul\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 1800 l\/mm grating a direct replacement for the Lhires III's original grating?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYes, this is a fully compatible, interchangeable module designed by Shelyak specifically for the Lhires III spectroscope. It is intended to be swapped with the standard 2400 l\/mm grating to change the instrument's optical characteristics based on your observing target.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWill the Lhires III 1800 l\/mm grating let me capture the spectrum of a star like Vega (Alpha Lyrae) in one shot?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe 1800 l\/mm grating provides a much wider field of view than the standard 2400 l\/mm grating, making it better suited for capturing broad stellar spectra. While the exact spectral range you can capture depends on your camera's sensor size and the specific wavelength you center on, this grating is the correct choice for projects that require observing multiple hydrogen Balmer lines in A-type stars like Vega in a single frame.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 1800 l\/mm grating affect the brightness of the spectrum from my Lhires III?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eBy dispersing starlight over a smaller area (lower dispersion), the 1800 l\/mm grating can produce a brighter continuum in the resulting spectrum compared to the 2400 l\/mm grating, assuming equal exposure time and conditions. This can be advantageous for obtaining a better signal-to-noise ratio on the overall spectrum of fainter objects.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDoes installing the 1800 l\/mm grating on the Lhires III require recalibration?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYes, absolutely. Any time you change the diffraction grating in a spectroscope, you change the instrument's dispersion (how many angstroms per pixel). You will need to perform a new spectral calibration using a calibration lamp to accurately measure wavelengths with the 1800 l\/mm grating installed.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943046607133,"sku":"SHK-SE0121","price":1018.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-Lhires-III-2400-l-mm-1_615c59cc-77ae-4187-b3f8-b440ca16be11.jpg?v=1789616301"},{"product_id":"shelyak-se0128","title":"Shelyak Alpy Barlow Lens for Alpy 600 Spectroscope","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eEnables DSLR camera use with Alpy 600 spectroscope\u003c\/li\u003e\n\u003cli\u003eIncreases available backfocus for long imaging trains\u003c\/li\u003e\n\u003cli\u003eAccommodates cameras with integrated filter wheels\u003c\/li\u003e\n\u003cli\u003eScrews directly to the rear of the ALPY 600\u003c\/li\u003e\n\u003cli\u003eCorrects focus for cameras with standard T-ring spacing\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Alpy Barlow Lens for Alpy 600 Spectroscope\u003c\/h2\u003e\n\u003cp\u003eThis dedicated Barlow lens is the essential component for connecting a DSLR or a camera with a long backfocus requirement to the Shelyak Alpy 600 spectroscope. It solves the critical problem of insufficient backfocus, extending the focal plane to meet the standard spacing of DSLRs with T-rings and astronomy cameras equipped with filter wheels. By screwing directly onto the rear of the Alpy 600, it makes it possible to achieve a sharp, focused spectrum with imaging systems that would otherwise be incompatible.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe Essential Adapter for DSLR Spectroscopy with Alpy 600\u003c\/h3\u003e\n\u003cp\u003eThe standard Alpy 600 has a very short backfocus distance, designed for compact, dedicated astronomy cameras. This Barlow lens modifies the optical path to significantly increase that distance, specifically to accommodate the deeper sensor position found in DSLR and mirrorless cameras. If you want to use your existing digital camera for spectroscopy, this lens is not optional—it is the required adapter to bring your camera to focus.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAccommodating Filter Wheels and Long Imaging Trains\u003c\/h3\u003e\n\u003cp\u003eModern imaging setups often include accessories like filter wheels or off-axis guiders that add considerable length to the imaging train. This Barlow provides the necessary focal extension to accommodate these bulkier configurations. It ensures you can integrate your preferred camera and accessories with the Alpy 600 without being limited by its native backfocus, giving you the flexibility to use your primary imaging rig for scientific analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the Shelyak Alpy Barlow Lens?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIts sole purpose is to \u003cstrong\u003eincrease the backfocus\u003c\/strong\u003e of the Shelyak Alpy 600 spectroscope. This allows you to achieve focus with cameras that have a long backfocus distance, such as DSLR cameras or astronomy cameras used with a filter wheel.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need this Barlow to use my Canon or Nikon DSLR with the Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. A standard DSLR camera's sensor is located too far from the mounting flange to reach focus on a native Alpy 600. This Barlow lens is required to extend the focal point to where your DSLR sensor can capture a sharp spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill this Barlow help if I use a ZWO filter wheel with my camera on the Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Adding a filter wheel to your imaging train increases the required backfocus beyond what the standard Alpy 600 provides. This Barlow lens provides the necessary additional spacing to bring your camera and filter wheel combination to focus.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I install the Alpy Barlow Lens?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eInstallation is straightforward. The Barlow element is designed to be screwed directly onto the rear of the Alpy 600 unit, where you would normally attach your camera adapter.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this Barlow compatible with any other spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this is a dedicated optical component designed specifically for the Shelyak Alpy 600. It is not a general-purpose Barlow and is not intended for use with other instruments or for visual observation.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes this Barlow lens change the resolution of the Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAs a Barlow lens, it increases the effective focal length of the system. This will change the image scale on your sensor, but it is designed to work with the Alpy 600's native resolution and optical design to produce a usable spectrum with longer backfocus cameras.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd colspan=\"2\" style=\"text-align:center;\"\u003eNo specifications provided.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item-full\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eNo items were listed in the box for this product.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943047262493,"sku":"SHK-SE0128","price":205.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Barlow-lens-1_a57ee582-85e9-4edd-8090-b7ec863f89c6.jpg?v=1789616317"},{"product_id":"shelyak-se0129","title":"Shelyak C-mount adapter for the Alpy 600","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConnects C-mount cameras to the Shelyak Alpy 600\u003c\/li\u003e\n\u003cli\u003eProvides an adjustable backfocus range from 9.5mm to 20mm\u003c\/li\u003e\n\u003cli\u003eReplaces the standard T-mount thread on the spectroscope\u003c\/li\u003e\n\u003cli\u003eEnables use of common scientific and guiding cameras\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eC-mount adapter for the Alpy 600\u003c\/h2\u003e\n\u003cp\u003eThis C-mount adapter for the Alpy 600 spectroscope allows you to set a precise camera backfocus between 9.5mm and 20mm. It replaces the native T-mount, opening up compatibility for C-mount cameras commonly used in spectroscopy that require a backfocus within this 9.5mm to 20mm range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eC-Mount Compatibility and a 9.5mm to 20mm Backfocus Range\u003c\/h3\u003e\n\u003cp\u003eThe Shelyak Alpy 600 spectroscope is supplied with a standard T-mount for attaching a science camera. This adapter allows you to convert that interface to the C-mount standard, which is widely used by many compact, high-speed CMOS cameras ideal for spectroscopy.\u003c\/p\u003e\n\u003cp\u003eThe key feature is the adjustable backfocus, which can be set anywhere between 9.5mm and 20mm. This range gives you the flexibility to achieve a sharp focus with various camera models that have different sensor flange depths.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy do I need this C-mount adapter for my Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Alpy 600 ships with a T-mount. This adapter is necessary if your science or guiding camera uses the C-mount standard, which is common for many high-frame-rate CMOS cameras. It physically converts the mount to ensure a secure, threaded connection.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat does the 9.5mm to 20mm backfocus range on the Alpy 600 C-mount adapter mean?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis is the range of distances you can set between the adapter's mounting flange and your camera's sensor to achieve a sharp focus on the spectroscope's slit. You will need to adjust within this range to match your specific camera's flange focal distance to get a sharp spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI have a guide camera with a 12.5mm backfocus. Can I use it with the Alpy 600 and this adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Since that camera's 12.5mm backfocus falls comfortably within the adapter's \u003cstrong\u003e9.5mm to 20mm adjustment range\u003c\/strong\u003e, you will be able to achieve proper focus. This makes it compatible with many popular C-mount cameras.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill this adapter work for attaching my DSLR to the Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo. DSLR cameras typically use T-mounts (via a T-ring) and have a much longer backfocus requirement (around 55mm), which is far outside this adapter's 9.5mm to 20mm range. The Alpy 600's standard T-mount is the correct interface for a DSLR.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs a C-mount connection as secure as a T-mount for the Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, for the cameras it's designed for. C-mount cameras are typically small and lightweight. The threaded C-mount connection provides a secure, non-flexing attachment essential for stable and repeatable spectroscopic work.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow do I set the correct backfocus with this Alpy 600 adapter?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou will typically start by referencing your camera's documentation for its flange-to-sensor distance. Set the adapter within its 9.5mm to 20mm range to match that distance, then perform fine focusing adjustments on the telescope to get a sharp spectrum.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eCamera Mount\u003c\/td\u003e\n\u003ctd\u003eC-mount\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpectroscope Interface\u003c\/td\u003e\n\u003ctd\u003eReplaces Alpy 600 T-mount\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eBackfocus Range\u003c\/td\u003e\n\u003ctd\u003e9.5mm - 20mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatible Spectroscope\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy 600\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eC-mount adapter for the Alpy 600\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943047590173,"sku":"SHK-SE0129","price":106.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-C-mount-adapter-for-the-Alpy-600-1_615451ca-76cd-4092-970c-608bf37473a2.jpg?v=1789616326"},{"product_id":"shelyak-se0131","title":"Shelyak Fiber Optic Adapter for Alpy 600","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConnects FC Standard Fiber Optics to the Alpy 600 Spectroscope\u003c\/li\u003e\n\u003cli\u003eReplaces the Standard 25µm Slit for Remote Light Injection\u003c\/li\u003e\n\u003cli\u003eEnables Bench-Mounted Setups and Remote Observatory Integration\u003c\/li\u003e\n\u003cli\u003eDesigned Specifically for the Shelyak Alpy 600\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eFiber Optic Adapter for Alpy 600\u003c\/h2\u003e\n      \u003cp\u003eThis FC-standard fiber optic adapter replaces the standard slit on the Shelyak Alpy 600 spectroscope, enabling remote light acquisition for permanent observatory setups or controlled laboratory environments. While this adapter adds significant operational flexibility, it involves a direct trade-off: using a standard 50µm object fiber will result in lower spectral resolution than the Alpy 600's native 25µm slit.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eThe 50µm Fiber vs. the 25µm Slit\u003c\/h3\u003e\n      \u003cp\u003eThe primary function of this adapter is to couple your Alpy 600 to a fiber optic cable, allowing the spectroscope to be mounted on a stable bench away from the telescope. This isolates the instrument from vibration and temperature changes at the scope, but introduces a change in the optical path. A typical 50µm fiber optic core acts as a wider entrance aperture than the Alpy 600's standard 25µm slit, which reduces the instrument's resolving power. This is a critical consideration for users whose scientific goals demand the highest possible resolution; for applications where convenience and stability are paramount, the trade-off may be acceptable.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary use for the Alpy 600 Fiber Optic Adapter?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThis adapter allows you to feed light into your Alpy 600 spectroscope via a fiber optic cable. This is ideal for \u003cstrong\u003eremote observatories\u003c\/strong\u003e where the telescope and spectroscope are physically separated, or for \u003cstrong\u003elaboratory work\u003c\/strong\u003e where the instrument is kept on a stable optical bench.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWill using this adapter with the Alpy 600 affect my spectral resolution?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003e\u003cstrong\u003eYes, it will lower the resolution.\u003c\/strong\u003e The adapter is designed for standard 50µm optical fibers, which have a larger diameter than the Alpy 600's native 25µm slit. This wider entrance aperture reduces the spectroscope's resolving power. You gain remote capability at the cost of spectral detail.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I use the Fiber Optic Adapter for the Alpy 600 if it lowers resolution?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe main benefit is operational stability and convenience. By moving the Alpy 600 off the telescope and onto a stable bench, you can better control its temperature and isolate it from vibrations, which is crucial for long-term projects or precise calibration. This setup is common in permanently mounted observatory systems.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat type of fiber optic connector does this Alpy 600 adapter use?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe adapter uses the industry-standard \u003cstrong\u003eFC connector\u003c\/strong\u003e, a common type used in telecommunications and scientific instrumentation for its secure, threaded connection.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this Alpy 600 adapter to study a star like Vega (Alpha Lyrae) from my remote setup?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eAbsolutely. You would connect a fiber optic cable from your telescope's focal plane to this adapter on the Alpy 600. This allows you to acquire the spectrum of Vega while the spectroscope remains in a controlled indoor environment, isolated from the telescope's movement and outdoor conditions. Just be mindful of the inherent reduction in resolution when planning your observation.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDoes this adapter replace or add to the existing slit on the Alpy 600?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eIt \u003cstrong\u003ereplaces\u003c\/strong\u003e the standard slit module. You must remove the existing slit assembly from the Alpy 600 and install this fiber optic adapter in its place.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003ctable class=\"DAV-specifications\"\u003e\n    \u003ctbody\u003e\n      \u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy 600 Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n      \u003ctr\u003e\n\u003ctd\u003eConnector Type\u003c\/td\u003e\n\u003ctd\u003eFC Standard\u003c\/td\u003e\n\u003c\/tr\u003e\n    \u003c\/tbody\u003e\n  \u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cul class=\"DAV-grid\"\u003e\n    \u003cli class=\"DAV-grid-item\"\u003e\n      \u003cdiv\u003e\n        \u003cp class=\"DAV-item-title\"\u003eFiber Optic Adapter for Alpy 600\u003c\/p\u003e\n        \u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n      \u003c\/div\u003e\n    \u003c\/li\u003e\n  \u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943047917853,"sku":"SHK-SE0131","price":230.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Fiber-optic-adapter-for-Alpy-600-1_ac7f339d-5cf4-4066-ab5a-173860cec57c.jpg?v=1789616334"},{"product_id":"shelyak-se0145","title":"Shelyak Photometric Slit 23\/200µm for Alpy 600 \u0026 UVEX","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eDual slit design with 23µm and 200µm widths\u003c\/li\u003e\n\u003cli\u003eEnables high-resolution spectroscopy and spectrophotometry\u003c\/li\u003e\n\u003cli\u003eDesigned for Shelyak Alpy 600 and UVEX spectroscopes\u003c\/li\u003e\n\u003cli\u003eRequires the Alpy Guiding Module for operation\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003ePhotometric Slit 23\/200µm for Alpy 600 \u0026amp; UVEX\u003c\/h2\u003e\n\u003cp\u003eThis Photometric Slit for Alpy 600 and UVEX spectroscopes enables true spectrophotometry by integrating two distinct apertures in a single component: a narrow 23µm slit for maximum resolution and a wide 200µm slit for capturing total stellar flux.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 23µm \/ 200µm Slit: A Dual-Purpose Tool for Spectrophotometry\u003c\/h3\u003e\n\u003cp\u003eThis accessory allows you to switch between two fundamental modes of spectroscopic observation without changing hardware. The 23µm slit provides the narrowest aperture, maximizing the spectral resolution of your Alpy 600 or UVEX to resolve fine details in stellar spectra. When your goal is to measure the precise brightness of an object across different wavelengths—true spectrophotometry—the wider 200µm slit ensures that all the light from the star enters the spectroscope, even in moments of poor seeing, for an accurate flux measurement.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the dual slits on the 23\/200µm Photometric Slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe two slits serve two different scientific goals. The narrow \u003cstrong\u003e23µm slit\u003c\/strong\u003e is used to achieve the highest possible spectral resolution for detecting fine absorption or emission lines. The wide \u003cstrong\u003e200µm slit\u003c\/strong\u003e is used for spectrophotometry, where the goal is to capture all of a star's light to accurately measure its brightness, sacrificing some resolution for photometric precision.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I use the 23µm slit with my Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eUse the 23µm slit when your primary objective is resolving detail in a spectrum. This is ideal for classifying star types, identifying chemical compositions, or measuring the doppler shift of spectral lines in objects like binary stars or quasars.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen is the 200µm slit the right choice for the Photometric Slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe 200µm slit is essential for spectrophotometry. If you are studying variable stars, supernovae, or any object where you need to create an accurate spectral energy distribution curve, the wide slit ensures you are measuring the total energy output of the star without light loss at the aperture.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this Photometric Slit compatible with all Shelyak spectrographs?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this slit is specifically designed for use with the \u003cstrong\u003eShelyak Alpy 600\u003c\/strong\u003e and \u003cstrong\u003eShelyak UVEX\u003c\/strong\u003e spectroscope models. It is not compatible with other instruments like the Lhires III or LISA.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need other accessories to use the 23\/200µm Photometric Slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this photometric slit must be used with the \u003cstrong\u003eAlpy Guiding Module\u003c\/strong\u003e. The guiding module is required to position the target star accurately on the desired slit and maintain that position during an exposure.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 200µm slit on the Photometric Slit help with poor seeing?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAtmospheric turbulence (seeing) causes a star's image to move and swell. A narrow slit can block some of this light as the star image shifts, leading to an inaccurate brightness measurement. The wide 200µm slit provides a large enough opening to contain the entire star image even under poor seeing conditions, ensuring all its light enters the spectroscope for a valid photometric reading.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Widths\u003c\/td\u003e\n\u003ctd\u003e23µm (High Resolution) \/ 200µm (Photometry)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003ePrimary Function\u003c\/td\u003e\n\u003ctd\u003eSpectrophotometry \u0026amp; High-Resolution Spectroscopy\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy 600, Shelyak UVEX\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eRequired Accessory\u003c\/td\u003e\n\u003ctd\u003eAlpy Guiding Module\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943048638749,"sku":"SHK-SE0145","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Photometric-slit-23-200-m-1_d73fed93-587d-42fe-8a9a-5716c60391fd.jpg?v=1789616359"},{"product_id":"shelyak-se0150","title":"Shelyak Alpy \u0026 UVEX 35 µm slit","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e35 µm Precision Slit Width\u003c\/li\u003e\n\u003cli\u003eIntegrated Guiding Mirror Surface\u003c\/li\u003e\n\u003cli\u003eCompatible with Shelyak Alpy \u0026amp; UVEX Spectrographs\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAlpy \u0026amp; UVEX 35 µm slit\u003c\/h2\u003e\n\u003cp\u003eThe Alpy \u0026amp; UVEX 35 µm slit is a core component for Shelyak spectrographs, functioning as both a precision entrance aperture and a guiding mirror. Its 35 µm width strikes a versatile balance between spectral resolution and light throughput, making it a standard choice for a wide range of astronomical targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 35µm Slit: Balancing Resolution and Light Throughput\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, the slit width directly controls the trade-off between the detail in your spectrum and its brightness. The 35 µm slit for the Alpy and UVEX spectrographs is a popular choice because it represents a highly effective compromise for many observing conditions and targets.\u003c\/p\u003e\n\u003cp\u003eThe polished, reflective surface surrounding the slit allows you to view the entire star field through your guiding camera. This ensures you can keep your target perfectly centered on the nearly invisible slit for long exposures, maximizing signal and preventing drift.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eSlit Selection for Alpy \u0026amp; UVEX: The 35µm Slit vs. Other Options\u003c\/h3\u003e\n\u003cp\u003eChoosing the correct slit is fundamental to achieving your scientific goals. While the 35µm slit is an excellent all-rounder, understanding its context helps you make the right decision for your specific target.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003evs. Narrower Slits (e.g., 25 µm):\u003c\/strong\u003e A narrower slit yields higher spectral resolution but passes significantly less light. It is the superior choice for studying fine absorption lines in the spectra of bright stars, where signal is plentiful.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003evs. Wider Slits (e.g., 50 µm+):\u003c\/strong\u003e A wider slit captures more photons, which is critical for obtaining a usable signal on very faint objects like distant galaxies or low-surface-brightness nebulae. The trade-off is a lower-resolution spectrum where fine details may be blurred.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cp\u003eThe 35µm slit is the workhorse option, ideal for general stellar classification, analyzing emission lines in planetary nebulae, and capturing spectra of moderately bright comets and supernovae.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main purpose of the Alpy \u0026amp; UVEX 35 µm slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIt serves two critical functions. The precision-cut \u003cstrong\u003e35 µm slit\u003c\/strong\u003e acts as the entrance aperture for the spectrograph, determining the resolution of the spectrum. The reflective surface around the slit acts as a \u003cstrong\u003eguiding mirror\u003c\/strong\u003e, allowing you to see the star field and keep your target perfectly centered for the duration of an exposure.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 35 µm slit affect the spectral resolution of my Alpy or UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe slit width is a primary factor in determining spectral resolution. A narrower slit produces a sharper, higher-resolution spectrum, allowing you to resolve finer details. The \u003cstrong\u003e35 µm slit\u003c\/strong\u003e provides a strong intermediate resolution, suitable for many projects from stellar classification to emission line studies in nebulae.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I choose the 35 µm slit over a narrower one for my Alpy\/UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou should choose the \u003cstrong\u003e35 µm slit\u003c\/strong\u003e when light throughput is as important as resolution. While a narrower slit (e.g., 25µm) offers higher resolution, it passes less light, requiring longer exposures. The 35µm slit is ideal for moderately faint targets or when seeing conditions don't support the highest possible resolution.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Alpy \u0026amp; UVEX 35 µm slit for guiding on my target star?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. The component is a guiding mirror with a slit at its center. The light from your target that doesn't pass through the slit is reflected into your guiding camera, allowing you to monitor the star's position and make precise tracking corrections.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 35 µm slit a good choice for observing faint nebulae like the Orion Nebula (M42) with a Shelyak spectrograph?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, the \u003cstrong\u003e35 µm slit\u003c\/strong\u003e is an excellent choice for targets like the Orion Nebula (M42). It allows enough light from the extended object to pass through to achieve a good signal-to-noise ratio in a reasonable time, while still providing enough resolution to separate key emission lines like Hydrogen-alpha and Oxygen-III.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eFor measuring the redshift of a bright quasar like 3C 273, would the 35 µm slit be appropriate for my UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe \u003cstrong\u003e35 µm slit\u003c\/strong\u003e is a very capable option for a bright quasar like 3C 273. It provides a good balance, capturing enough light for a clear continuum while delivering the resolution needed to accurately measure the shift in prominent spectral lines, such as the broad Hydrogen-beta line used for redshift calculations.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Width\u003c\/td\u003e\n\u003ctd\u003e35 µm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy and UVEX series spectrographs\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eAlpy \u0026amp; UVEX 35 µm slit\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943049195805,"sku":"SHK-SE0150","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Alpy-UVEX-35-m-slit-1_b2bb2b2b-316f-4f80-84b8-877210aaf9ff.jpg?v=1789616376"},{"product_id":"shelyak-se0151","title":"Shelyak Alpy Guiding Mirror with 50 µm Slit","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e50 µm Slit Width\u003c\/li\u003e\n\u003cli\u003eIntegrated Guiding Mirror\u003c\/li\u003e\n\u003cli\u003eCompatible with Alpy Spectrograph Systems\u003c\/li\u003e\n\u003cli\u003eOptimized for Faint Object Spectroscopy\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eShelyak Alpy Guiding Mirror with 50 µm Slit\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Alpy Guiding Mirror with a 50 µm slit is a key component for the Alpy series of spectrographs, engineered to maximize light throughput from faint celestial targets. This specific slit width offers a practical balance, capturing more photons from diffuse objects like galaxies and nebulae compared to narrower slits, making it an essential choice for low-signal scientific work.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe Dual-Function Alpy Guiding Mirror: A 50 µm Aperture\u003c\/h3\u003e\n\u003cp\u003eThis component serves a dual purpose critical to successful spectroscopy. The precision-cut 50 µm slit allows the focused starlight to pass through to the spectrograph's grating, while the highly reflective mirrored surface surrounding the slit directs the rest of the field of view to your guiding camera. This allows for precise, long-exposure guiding directly on your target, ensuring the star remains perfectly centered on the narrow slit for the duration of the observation.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e50 µm vs. 25 µm Slit: Trading Resolution for Throughput\u003c\/h3\u003e\n\u003cp\u003eChoosing a slit size is a fundamental compromise between spectral resolution and signal-to-noise ratio. The 50 µm slit is the preferred option when the primary goal is capturing a spectrum from a faint object, where every photon counts.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003e50 µm Slit (This Product):\u003c\/strong\u003e Doubles the light-gathering area compared to a 25 µm slit, significantly improving the signal on faint galaxies, nebulae, or low-magnitude stars. This comes at the cost of lower spectral resolution, where fine spectral lines may appear broader.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003e25 µm Slit:\u003c\/strong\u003e Offers higher spectral resolution, allowing for the separation of closely spaced spectral lines. This is ideal for studying bright stars with complex spectra but can make it challenging to acquire a usable signal from fainter targets.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I choose the 50 µm slit for my Alpy spectrograph?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou should choose the \u003cstrong\u003e50 µm slit\u003c\/strong\u003e when your primary targets are faint, diffuse objects. This includes galaxies, planetary nebulae, and low-magnitude variable stars. The wider aperture allows more light to enter the spectrograph, improving your signal-to-noise ratio at the expense of some spectral resolution.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow will the Alpy 50 µm slit affect the spectrum of a faint galaxy like the Whirlpool Galaxy (M51)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor a target like M51, the \u003cstrong\u003e50 µm slit\u003c\/strong\u003e is highly advantageous. It will allow you to capture a usable signal from the galaxy's core in a much shorter time than a narrower slit. While you will lose some resolution, you will be able to clearly identify major features like H-alpha emissions and determine the galaxy's overall redshift.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I study the emission lines of a bright Be star like Gamma Cassiopeiae with the 50 µm slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, you can absolutely use the \u003cstrong\u003e50 µm slit\u003c\/strong\u003e for a bright star like Gamma Cassiopeiae. You will easily capture the prominent Hydrogen-alpha emission line. However, for resolving very fine structures or subtle Doppler shifts in the line profile, a narrower slit like the 25 µm version would provide higher resolution and more detailed results.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of the Alpy 50 µm slit over a 25 µm slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe main advantage is \u003cstrong\u003elight throughput\u003c\/strong\u003e. The 50 µm slit has a larger open area, allowing significantly more light to pass into the spectrograph. This is critical for reducing exposure times and achieving a better signal-to-noise ratio on faint objects, which might be impossible to record with a narrower slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the guiding mirror on the 50 µm slit work?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe component is a mirror with a tiny, central slit. Your telescope focuses the star field onto this mirror. The light from the target star goes through the \u003cstrong\u003e50 µm slit\u003c\/strong\u003e into the spectrograph. The surrounding stars in the field of view are reflected off the mirror's surface and into a separate guiding camera, allowing you to maintain perfect tracking for long exposures.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 50 µm slit compatible with all Shelyak Alpy models?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, the \u003cstrong\u003e50 µm slit\u003c\/strong\u003e is designed as a modular component for the Shelyak Alpy ecosystem. It is compatible with spectrograph models like the Alpy 600 and the Alpy 200 base module, allowing you to swap slits based on your observing goals for the night.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSlit Width\u003c\/td\u003e\n\u003ctd\u003e50 µm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eType\u003c\/td\u003e\n\u003ctd\u003eGuiding Mirror Slit\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak Alpy Spectrographs\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class.dav-grid\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003e50 µm Guiding Mirror Slit\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Guiding_Module_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Guiding Module Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943049457949,"sku":"SHK-SE0151","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-50-m-slit-1_a440b1ee-2783-4775-bcef-a31672128820.jpg?v=1789616384"},{"product_id":"shelyak-se0192","title":"Shelyak Lhires III Slit Holder","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eEnables rapid slit changes for the Lhires III spectroscope\u003c\/li\u003e\n\u003cli\u003eImproves observational efficiency in the field\u003c\/li\u003e\n\u003cli\u003eCompatible with standard, wide, and photometric slits\u003c\/li\u003e\n\u003cli\u003eSecurely holds slits for repeatable results\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eLhires III Slit Holder\u003c\/h2\u003e\n      \u003cp\u003eThe Shelyak Lhires III Slit Holder is an essential accessory designed to significantly streamline your spectroscopic workflow. It allows for the rapid exchange of different slits, enabling you to quickly adapt the Lhires III spectroscope for various observational targets and scientific goals. This holder is compatible with Shelyak's wide, photometric, and standard slits, providing critical operational flexibility during an observing session.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eStreamline Slit Changes on the Lhires III\u003c\/h3\u003e\n      \u003cp\u003eFor observers using the Lhires III for multiple projects in a single night, changing slits can be a time-consuming process. The Lhires III Slit Holder eliminates this bottleneck by allowing you to swap between different slit types in seconds. This ensures you spend more time acquiring data and less time reconfiguring your instrument in the dark.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n  \n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eAdapt to Multiple Spectroscopic Targets\u003c\/h3\u003e\n      \u003cp\u003eThis holder is the key to unlocking the full scientific potential of your Lhires III by providing a secure and repeatable mounting point for Shelyak's range of specialized slits.\u003c\/p\u003e\n      \u003cul\u003e\n        \u003cli\u003e\n\u003cstrong\u003eStandard Slits:\u003c\/strong\u003e Use for general-purpose, high-resolution stellar spectra of bright targets.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003eWide Slits:\u003c\/strong\u003e Switch to these for capturing more light from faint objects like comets or nebulae, sacrificing some resolution for a stronger signal.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003ePhotometric Slits:\u003c\/strong\u003e Install for precise brightness measurements, where capturing the total flux from a star is more critical than fine spectral detail.\u003c\/li\u003e\n      \u003c\/ul\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of using the Lhires III Slit Holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003e\u003cstrong\u003eEfficiency.\u003c\/strong\u003e The primary benefit of the Lhires III Slit Holder is the ability to change slits very quickly without complex disassembly of the spectroscope. This saves valuable observing time and allows you to adapt your instrument to changing targets or conditions with minimal downtime.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhich slits are compatible with the Lhires III Slit Holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe Lhires III Slit Holder is specifically designed to be used with the family of slits made by Shelyak for the Lhires III spectroscope. This includes their \u003cstrong\u003estandard, wide, and photometric slits\u003c\/strong\u003e.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need a separate Lhires III Slit Holder for each slit I own?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eNo, a single holder is installed in the spectroscope, and you can insert your various slits into it. However, some advanced users purchase multiple holders and pre-install their most-used slits to make field swaps nearly instantaneous.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIf I am studying a Be star like Gamma Cassiopeiae and then a faint comet, how does the Lhires III Slit Holder help?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThis is a perfect use case. You would use a narrow, standard slit for the high-resolution spectrum of the bright Be star. With the Lhires III Slit Holder, you can then quickly swap to a wide slit to maximize light collection from the faint, diffuse comet, all without a lengthy and difficult reconfiguration in the dark.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eI want to perform photometry on an eclipsing binary with my Lhires III. Which slit should I use with the holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eFor photometry, you would use the dedicated \u003cstrong\u003ephotometric slit\u003c\/strong\u003e with your Lhires III Slit Holder. This type of slit is designed to ensure all the starlight enters the spectroscope, which is critical for accurate brightness measurements, even if it results in lower spectral resolution.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIs installation of the Lhires III Slit Holder difficult?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe holder is designed for straightforward integration into the Lhires III spectroscope body. For detailed instructions, please refer to the official Shelyak Lhires III user manual, which covers the replacement of the slit assembly.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Lhires_III_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Lhires III Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943050440989,"sku":"SHK-SE0192","price":197.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Lhires-III-slit-holder-1_8610993a-8ede-4c31-b8ed-4de9a5be8e5e.jpg?v=1789616417"},{"product_id":"shelyak-se0193","title":"Shelyak LISA Slit Holder","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eEnables rapid interchange of spectroscopic slits\u003c\/li\u003e\n\u003cli\u003eDesigned specifically for the Shelyak LISA Spectroscope\u003c\/li\u003e\n\u003cli\u003eCompatible with standard, wide, and photometric slits\u003c\/li\u003e\n\u003cli\u003eStreamlines workflow for varied astronomical targets\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003eLISA Slit Holder\u003c\/h2\u003e\n      \u003cp\u003eThe Shelyak LISA Slit Holder is the essential accessory for adding operational flexibility to your LISA spectroscope. It provides the core mechanism for rapidly and easily swapping between different slits, allowing you to adapt your instrument's configuration in the field to match the scientific requirements of any target, from faint nebulae to bright variable stars.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eInterchangeable Slit System for the LISA Spectroscope\u003c\/h3\u003e\n      \u003cp\u003eThis holder transforms the LISA from a single-slit instrument into a modular system. Instead of being locked into one slit width for an entire night, you can pre-load multiple slits into individual holders and exchange them in moments. This capability is critical for observers who need to switch between different types of spectroscopy during a single session.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eAdapt Your LISA for Different Scientific Targets\u003c\/h3\u003e\n      \u003cp\u003eThe LISA Slit Holder is designed to accept a range of Shelyak slits, each optimized for a specific astronomical application. By using this holder, you can seamlessly switch between different observational modes.\u003c\/p\u003e\n      \u003cul\u003e\n        \u003cli\u003e\n\u003cstrong\u003eStandard Slits:\u003c\/strong\u003e Use for general-purpose, high-resolution spectroscopy of stars and other point sources.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003eWide Slits:\u003c\/strong\u003e Ideal for capturing the spectra of faint, extended objects like galaxies or nebulae where maximizing light throughput is more important than resolution.\u003c\/li\u003e\n        \u003cli\u003e\n\u003cstrong\u003ePhotometric Slits:\u003c\/strong\u003e Designed for spectrophotometry, allowing for accurate measurements of an object's flux, which is crucial for studying variable stars or supernovae.\u003c\/li\u003e\n      \u003c\/ul\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the LISA Slit Holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe LISA Slit Holder is designed specifically for the Shelyak LISA spectroscope to make changing slits fast and simple. This allows an observer to use multiple slit types (e.g., standard, wide, photometric) during a single observing session without complex disassembly, adapting the instrument to different targets and scientific goals.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eDoes the LISA Slit Holder include any slits?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eNo, this product is only the holder itself. The various slits (standard, wide, photometric) must be purchased separately. This allows you to build a custom kit with only the slit types you need for your specific research or observing program.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat types of slits can I use with the LISA Slit Holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe holder is compatible with Shelyak's dedicated slits for the LISA spectroscope, which include standard slits for high-resolution work, wide slits for faint objects, and photometric slits for flux analysis.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I need to change slits on my LISA spectroscope during an observing session?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eDifferent astronomical targets require different slit widths for optimal results. You might start a session by capturing a high-resolution spectrum of a bright star with a narrow slit, then switch to a wide slit to capture more light from a faint galaxy. The holder makes this transition efficient.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow does using a wide slit with the LISA Slit Holder affect my spectra of a faint galaxy like the Whirlpool Galaxy (M51)?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eFor a faint, extended object like M51, a wide slit allows more photons from the galaxy's core or spiral arms to enter the spectroscope. This increases the signal-to-noise ratio, making it possible to detect faint emission or absorption features that would be lost with a narrow slit, though it does so at the cost of lower spectral resolution.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIf I want to measure the flux of a variable star like Betelgeuse with my LISA, which slit should I use in the holder?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eFor measuring accurate brightness (flux), you should use a \u003cstrong\u003ephotometric slit\u003c\/strong\u003e in your LISA Slit Holder. These slits are designed to be wide enough to ensure all the light from the star enters the spectroscope, even with minor tracking errors or poor seeing, which is essential for reliable spectrophotometry.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943050834205,"sku":"SHK-SE0193","price":197.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-LISA-slit-holder-1_ce663029-18d0-44db-9ebd-e4a8a70b33cf.jpg?v=1789616426"},{"product_id":"shelyak-se0194","title":"Shelyak LISA \u0026 Lhires III Photometric Slit","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eEnables true spectrophotometry with LISA \u0026amp; Lhires III spectrographs\u003c\/li\u003e\n\u003cli\u003eDual-width design for simultaneous high-resolution spectra and total flux measurement\u003c\/li\u003e\n\u003cli\u003eCaptures all starlight for precise photometric data\u003c\/li\u003e\n\u003cli\u003eIdeal for studying variable stars, novae, and supernovae\u003c\/li\u003e\n\u003cli\u003eDirect-fit accessory for specified Shelyak instruments\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eLISA \u0026amp; Lhires III Photometric Slit\u003c\/h2\u003e\n\u003cp\u003eThis Photometric Slit set for the Shelyak LISA and Lhires III spectrographs enables true scientific spectrophotometry by combining high-resolution spectral analysis with precise brightness measurement. Each slit features a unique dual-width design, with a narrow section to maintain the full resolving power of your instrument and a wide section to ensure every photon from your target star is collected. This allows you to create fully flux-calibrated spectra, essential for analyzing variable stars, novae, and other transient astronomical events.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eDual-Width Slit Design: The Key to Accurate Spectrophotometry\u003c\/h3\u003e\n\u003cp\u003eStandard spectroscopic slits are a compromise; narrow for high resolution, but at the risk of losing starlight due to atmospheric seeing, which corrupts brightness data. This photometric slit solves that problem by providing two slit widths in one. You can acquire a high-resolution spectrum using the narrow portion and a separate, photometrically accurate reading through the wide portion.\u003c\/p\u003e\n\u003cp\u003eBy combining observations from both sections, you can normalize the high-resolution spectrum to the total, accurate brightness of the star. This unlocks the ability to measure not just the composition and velocity of an object, but its absolute energy output across the spectrum—the core purpose of spectrophotometry.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCompatibility and Use Case: For Shelyak LISA \u0026amp; Lhires III Spectrographs\u003c\/h3\u003e\n\u003cp\u003eThis set of slits is designed specifically as an accessory for the Shelyak LISA and Lhires III spectrographs. It replaces the standard slit, allowing observers to upgrade their instrument's capability from pure spectroscopy to quantitative spectrophotometry.\u003c\/p\u003e\n\u003cp\u003eThe primary application is for any research where both the spectral features and the absolute brightness of an object are changing. This is critical for characterizing the physics of cataclysmic variable stars, tracking the light curve and spectral evolution of a supernova, or monitoring the activity of young stellar objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the purpose of the LISA \u0026amp; Lhires III Photometric Slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Photometric Slit allows you to perform \u003cstrong\u003espectrophotometry\u003c\/strong\u003e, which is the measurement of a star's spectrum (its light broken down by color) combined with an accurate measurement of its total brightness (photometry). This is crucial for creating scientifically accurate, flux-calibrated stellar spectra.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the dual-width design of the Photometric Slit work?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eEach slit has two sections:\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003eA \u003cstrong\u003enarrow part\u003c\/strong\u003e that provides the high spectral resolution needed to see fine details in a star's spectrum.\u003c\/li\u003e\n\u003cli\u003eA \u003cstrong\u003ewide part\u003c\/strong\u003e that ensures all the light from the star enters the spectrograph, even with poor seeing. This is essential for getting an accurate brightness measurement.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cp\u003eBy taking observations with both parts of the slit, you can combine the detailed spectrum from the narrow part with the accurate brightness data from the wide part.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the Photometric Slit compatible with spectrographs other than the Shelyak LISA and Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this accessory is specifically designed for use with the Shelyak Instruments \u003cstrong\u003eLISA\u003c\/strong\u003e and \u003cstrong\u003eLhires III\u003c\/strong\u003e spectrographs. It is not intended for use with other models or brands.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy can't I just use a single wide slit for both spectroscopy and photometry?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eWhile a wide slit captures all the star's light for good photometry, it dramatically reduces the spectrograph's resolution. Spectral lines would appear blurry and smeared, and fine details would be lost. The dual-width design allows you to get the best of both worlds: high resolution and accurate photometry, by taking separate, specialized exposures.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow would I use the Photometric Slit to study a variable star like Algol (Beta Persei)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eTo study an eclipsing binary like Algol (Beta Persei), you would take a series of exposures over time. For each observation, you would capture one spectrum with the narrow part of the slit to record any changes in the spectral lines (like doppler shifts), and another with the wide part to precisely measure the drop in brightness during the eclipse. This provides a complete picture of the system's dynamics.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I'm observing a supernova in a galaxy like the Whirlpool Galaxy (M51), what advantage does this slit give me?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor a supernova in M51, the Photometric Slit is invaluable. You would use the narrow slit to capture high-resolution spectra of the expanding debris, identifying elements and measuring their velocities. You would then use the wide slit to accurately measure the supernova's changing brightness, creating a light curve. Combining these allows you to calculate the total energy output and model the physics of the explosion far more accurately than with a standard slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943051063581,"sku":"SHK-SE0194","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-LISA-Lhires-III-Photometric-Slit-1_96e40eb5-63be-4000-a492-6d82fc431e67.jpg?v=1789616434"},{"product_id":"shelyak-se0238","title":"Shelyak Fiber Optic Connector Kit for UVEX","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eAdapts the Shelyak UVEX spectrograph for fiber optic input\u003c\/li\u003e\n\u003cli\u003eEnables physical separation of the telescope and spectrograph\u003c\/li\u003e\n\u003cli\u003eIdeal for permanent observatory installations to reduce vibration and thermal influence\u003c\/li\u003e\n\u003cli\u003eFacilitates a stable and repeatable setup for long-term projects\u003c\/li\u003e\n\u003cli\u003eEngineered for a trade-off between light throughput and spectral resolution\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eFiber Optic Connector Kit for UVEX\u003c\/h2\u003e\n\u003cp\u003eThis Fiber Optic Connector Kit adapts the Shelyak UVEX spectrograph for use with a fiber optic feed, allowing you to physically decouple the instrument from your telescope. This capability is essential for permanent observatory setups where the spectrograph can be mounted on a stable pier or bench, isolated from telescope vibrations and thermal variations. By feeding light directly from the telescope's focal plane via an optical fiber, you gain significant stability for long-term scientific projects, such as exoplanet transit monitoring or variable star photometry.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eRemote Light Injection for the UVEX Spectrograph\u003c\/h3\u003e\n\u003cp\u003eThe primary function of this kit is to enable remote spectroscopy. Instead of mounting the heavy and sensitive UVEX directly onto your moving telescope, this adapter allows you to place it in a controlled environment. This minimizes mechanical flexure, focus drift due to temperature changes, and vibrations, which are critical sources of error in high-resolution spectroscopy.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eUnderstanding the Resolution Trade-Off\u003c\/h3\u003e\n\u003cp\u003eUsing an optical fiber feed involves a deliberate engineering trade-off. A typical optical fiber has a larger diameter than the UVEX's standard entrance slit. This increases light throughput, which is beneficial for faint targets, but it also reduces the instrument's ultimate spectral resolution. This kit is therefore optimized for applications where stability and light-gathering are more critical than achieving the highest possible resolution the UVEX can offer with its narrowest slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary purpose of the UVEX Fiber Optic Connector Kit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary purpose of this kit is to allow you to connect a fiber optic cable to your Shelyak UVEX spectrograph. This enables you to physically separate the spectrograph from the telescope, which is ideal for permanent observatory setups to improve stability and reduce environmental interference like vibration and temperature changes.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does using this fiber optic kit affect the resolution of my UVEX spectrograph?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eUsing an optical fiber reduces the spectrograph's resolution compared to using its standard, narrower slit. The larger core of a typical fiber acts as a wider entrance slit, increasing light throughput for fainter targets but resulting in broader spectral lines. This is a known trade-off for gaining the stability of a fiber-fed system.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I use a fiber optic feed with my UVEX for a project on a star like Betelgeuse (Alpha Orionis)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor long-term monitoring of a variable star like Betelgeuse, stability is paramount. A fiber feed isolates the UVEX spectrograph from the telescope's movement and thermal shifts, ensuring that any changes you record in the star's spectrum are genuine and not artifacts from the equipment. This stable, repeatable setup is crucial for differential photometry and radial velocity studies over weeks or months.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use this kit to build a remote-controlled spectroscopy setup in my observatory?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this kit is a key component for such a setup. By placing the UVEX on a stable bench and running a fiber optic cable to the telescope, you can automate your data acquisition without having to physically interact with the spectrograph, minimizing disturbances and allowing for fully remote operation.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes the Fiber Optic Connector Kit for UVEX include the fiber optic cable itself?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this kit is an adapter to connect a fiber to the spectrograph. The optical fiber cable itself is sold separately, allowing you to choose the appropriate length and core diameter for your specific observatory configuration.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs this connector kit compatible with other spectrographs, like the Lhires III?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis kit is specifically designed for the Shelyak UVEX spectrograph. It is not compatible with other models like the Lhires III, which have different mechanical interfaces and optical designs.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eSpecifications\u003c\/td\u003e\n\u003ctd\u003eNo specifications available for this accessory.\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003ePackage contents not specified.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943051686173,"sku":"SHK-SE0238","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Fiber-optic-connector-kit-for-UVEX-1_864bbaf8-6b09-4703-aeb1-1f99092dd2dd.jpg?v=1789616451"},{"product_id":"shelyak-se0242","title":"Shelyak Grating module for the UVEX - 150 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e150 lines\/mm Grating Density\u003c\/li\u003e\n\u003cli\u003eDesigned for the Shelyak UVEX Spectroscope\u003c\/li\u003e\n\u003cli\u003eOptimized for Low-Resolution, Wide-Coverage Spectroscopy\u003c\/li\u003e\n\u003cli\u003eInterchangeable Module for UVEX System\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the UVEX - 150 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis optional 150 lines\/mm grating module expands the capabilities of your UVEX spectroscope, sitting at the lowest-resolution end of a lineup that includes 300, 600, 1200, and 1800 l\/mm options. By trading the high resolution of the standard 600 l\/mm grating for maximum wavelength coverage, the 150 l\/mm module is purpose-built for survey work and classifying a wide range of celestial objects in a single exposure.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e150 l\/mm Grating: Maximizing Spectral Range for Survey Work\u003c\/h3\u003e\n\u003cp\u003eThe primary role of the 150 l\/mm grating is to capture the widest possible spectral range that your camera sensor can accommodate in a single frame. This low-dispersion capability is essential for survey projects where the goal is to quickly characterize many targets, such as classifying stars, identifying supernova types, or monitoring cometary emissions.\u003c\/p\u003e\n\u003cp\u003eFor faint targets, lower dispersion concentrates the object's light over fewer pixels, increasing the signal-to-noise ratio of the continuum. This makes the 150 l\/mm grating the most efficient choice for obtaining usable spectra of faint novae, asteroids, or distant quasars where capturing the overall spectral shape is more critical than resolving fine details.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eUVEX 150 l\/mm vs. 600 l\/mm Grating: Resolution vs. Wavelength Coverage\u003c\/h3\u003e\n\u003cp\u003eChoosing between the optional 150 l\/mm grating and the standard 600 l\/mm grating is a direct trade-off between spectral detail and wavelength coverage. Your scientific objective determines which is the correct tool for the job.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eStandard 600 l\/mm Grating:\u003c\/strong\u003e This grating provides four times the resolution, making it the superior choice for resolving fine spectral features. It is ideal for measuring subtle Doppler shifts, studying complex stellar atmospheres, or separating closely spaced emission lines in planetary nebulae.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eOptional 150 l\/mm Grating:\u003c\/strong\u003e This grating captures a much wider band of the spectrum on the same sensor. This allows you to see the entire visible spectrum of an object at once, from the violet H-delta line to the red H-alpha line, without creating a mosaic of multiple images. This is invaluable for transient events or initial object classification.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the 150 l\/mm grating for my UVEX instead of the standard 600 l\/mm?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou should choose the \u003cstrong\u003e150 l\/mm grating\u003c\/strong\u003e when your primary goal is to capture the widest possible range of wavelengths in a single exposure. It is ideal for survey work, classifying unknown objects, or studying targets with very broad spectral features. The standard \u003cstrong\u003e600 l\/mm grating\u003c\/strong\u003e is better when you need high resolution to study fine details within a narrow spectral window.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of objects, like a Type Ia supernova or a Wolf-Rayet star, are best studied with the UVEX 150 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe UVEX 150 l\/mm grating is excellent for both. \u003cstrong\u003eType Ia supernovae\u003c\/strong\u003e are identified by a characteristic broad silicon absorption feature (Si II) at 6150Å, which is easily captured with this grating's wide coverage. \u003cstrong\u003eWolf-Rayet stars\u003c\/strong\u003e have extremely broad emission lines (sometimes hundreds of angstroms wide) from stellar winds, and the 150 l\/mm grating ensures the entire profile of these features fits within a single frame.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes the 150 l\/mm grating affect exposure times with the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Because the 150 l\/mm grating disperses light less than a higher-density grating, it concentrates the starlight onto fewer pixels on your camera sensor. This results in a higher signal-to-noise ratio for the stellar continuum in a given exposure time, making it more efficient for capturing spectra of faint objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-Q\"\u003eCan I use the UVEX 150 l\/mm grating to measure precise radial velocities?\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this is not the right tool for that task. The low resolution of the 150 l\/mm grating is insufficient for measuring the small Doppler shifts required for precise radial velocity work. For those applications, a higher resolution grating, such as the standard 600 l\/mm or the optional 1200 l\/mm, is necessary.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIf I'm trying to classify a newly discovered comet with my UVEX, is the 150 l\/mm or the 600 l\/mm grating a better choice?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe \u003cstrong\u003e150 l\/mm grating\u003c\/strong\u003e is the better choice for initial comet classification. Cometary spectra often show broad emission bands from molecules like C2 (the Swan bands) and CN spread across the visible spectrum. The wide coverage of the 150 l\/mm grating allows you to capture all these features simultaneously to quickly assess the comet's composition.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs it difficult to swap gratings on the Shelyak UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the Shelyak UVEX is designed as a modular system. Swapping gratings is a straightforward process, allowing you to reconfigure the spectroscope in the field to match your observing target and scientific goals for the night. Always refer to the UVEX manual for the correct procedure.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Density\u003c\/td\u003e\n\u003ctd\u003e150 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak UVEX Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eUVEX 150 l\/mm Grating Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943051948317,"sku":"SHK-SE0242","price":992.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-UVEX-150-l-mm-1_8c7669aa-09e4-416e-a28d-be125b6cbaa3.jpg?v=1789616459"},{"product_id":"shelyak-se0243","title":"Shelyak Grating module for the UVEX - 300 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e300 lines\/mm Grating Density\u003c\/li\u003e\n\u003cli\u003eOptional Interchangeable Module\u003c\/li\u003e\n\u003cli\u003eDesigned for the Shelyak UVEX Spectroscope\u003c\/li\u003e\n\u003cli\u003eLower Resolution, Wider Spectral Coverage\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the UVEX - 300 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis optional Grating Module for the Shelyak UVEX spectroscope features a line density of 300 lines\/mm, offering a different balance of resolution and spectral coverage compared to the standard 600 l\/mm grating. It is a key component in a modular system that includes gratings from 150 l\/mm up to 1800 l\/mm, allowing you to tailor the instrument's capabilities to specific scientific targets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 300 l\/mm Grating: Balancing Resolution and Spectral Range\u003c\/h3\u003e\n\u003cp\u003eIn spectroscopy, grating choice dictates a fundamental trade-off. The 300 lines\/mm grating disperses incoming light less aggressively than higher-density gratings. This results in lower spectral resolution but allows a significantly wider range of wavelengths to fit onto your camera's sensor in a single exposure.\u003c\/p\u003e\n\u003cp\u003eThis capability is critical for survey work, initial classification of variable stars or supernovae, and studying objects with very broad spectral features. For faint targets, concentrating the light over a smaller sensor area can also improve the signal-to-noise ratio for the overall spectrum, making it a valuable tool for capturing data on challenging objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eChoosing Your Grating: 300 l\/mm vs. the 600 l\/mm Standard\u003c\/h3\u003e\n\u003cp\u003eWhile the UVEX's standard 600 l\/mm grating provides an excellent general-purpose balance for many projects, the 300 l\/mm module serves a specific and complementary role. You would choose the 300 l\/mm grating when your scientific goal prioritizes wavelength coverage over fine detail.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003e300 l\/mm Grating:\u003c\/strong\u003e Best for wide-field spectroscopy. Use it to capture the full spectrum of a nova from the hydrogen-alpha to hydrogen-beta lines in one frame, or for classifying multiple stars in a cluster simultaneously.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003e600 l\/mm Grating (Standard):\u003c\/strong\u003e The versatile workhorse. Ideal for resolving the double-peaked emission lines in Be stars or studying the detailed structure of planetary nebulae spectra.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eHigher Density Gratings (1200\/1800 l\/mm):\u003c\/strong\u003e These are reserved for high-resolution studies of single, narrow spectral lines, such as measuring the radial velocity of a star via Doppler shift.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary use for the Shelyak UVEX 300 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe 300 l\/mm grating is designed for low-resolution spectroscopy where capturing a wide range of wavelengths in a single image is more important than resolving fine details. It is ideal for survey projects, classifying unknown objects, and studying targets with broad spectral features like supernovae or novae.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 300 l\/mm grating compare to the standard 600 l\/mm grating included with the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe 300 l\/mm grating provides half the spectral resolution of the standard 600 l\/mm grating. In exchange, it covers a much wider spectral range on the same sensor. The 600 l\/mm is a general-purpose tool for detailed analysis, while the 300 l\/mm is a specialized tool for wide-field spectroscopic surveys.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen would I choose the 300 l\/mm grating for observing a nova like Nova Persei (GK Persei)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor a nova, especially in its early, rapidly evolving stages, the 300 l\/mm grating is an excellent choice. It allows you to capture the entire visible spectrum, including the broad P Cygni profiles and multiple emission lines (like the Balmer series), in a single exposure to monitor its overall evolution. A higher-resolution grating might require multiple exposures and mosaicking to cover the same range.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill the 300 l\/mm grating fit my Shelyak UVEX spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. This grating is specifically designed as an interchangeable module for the Shelyak UVEX spectroscope, allowing you to easily swap it with the standard 600 l\/mm grating or other optional gratings in the series.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 300 l\/mm grating better for faint objects than the 1200 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, for capturing a detectable spectrum. The 300 l\/mm grating concentrates the faint light over a smaller area on the sensor, improving the signal-to-noise ratio of the overall spectrum. The 1200 l\/mm grating spreads that same faint light out much further, which can make the resulting high-resolution spectrum too dim to be useful without very long exposures.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 300 l\/mm grating to measure the redshift of a quasar like 3C 273?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an excellent application for the 300 l\/mm grating. The broad emission lines of a quasar like 3C 273 are easily visible at this resolution, and the wide spectral coverage helps you identify multiple lines to confirm the redshift. The goal is to identify the pattern of shifted lines, not to resolve their internal structure, making low resolution ideal.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eProduct\u003c\/td\u003e\n\u003ctd\u003eGrating Module\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eInstrument\u003c\/td\u003e\n\u003ctd\u003eShelyak UVEX Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Density\u003c\/td\u003e\n\u003ctd\u003e300 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eGrating Module for UVEX (300 l\/mm)\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943052275997,"sku":"SHK-SE0243","price":992.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-UVEX-150-l-mm-1_b112a085-7d93-4f03-a91a-1d652c44b9a9.jpg?v=1789616467"},{"product_id":"shelyak-se0245","title":"Shelyak Grating module for the UVEX - 1200 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e1200 lines\/mm Grating Density\u003c\/li\u003e\n\u003cli\u003eDesigned for the Shelyak UVEX Spectroscope\u003c\/li\u003e\n\u003cli\u003eEnables High-Resolution Spectroscopy\u003c\/li\u003e\n\u003cli\u003eUser-Interchangeable Module\u003c\/li\u003e\n\u003cli\u003eDoubles Resolution of Standard Grating\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the UVEX - 1200 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThis optional 1200 lines\/mm grating module for the Shelyak UVEX spectroscope is engineered specifically for high-resolution applications. It directly replaces the standard 600 l\/mm grating supplied with the UVEX, effectively doubling the instrument's native spectral resolving power for detailed scientific analysis.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eHigh-Resolution Spectroscopy with the 1200 l\/mm Grating\u003c\/h3\u003e\n\u003cp\u003eIncreasing a spectroscope's line density from 600 l\/mm to 1200 l\/mm allows you to resolve finer details within a star's spectrum. This is critical for advanced projects such as monitoring the emission line profile changes in Be stars, measuring small Doppler shifts in spectroscopic binaries, or separating closely spaced absorption lines in stellar atmospheres.\u003c\/p\u003e\n\u003cp\u003eBy spreading the light over a greater angle, the 1200 l\/mm grating makes these subtle spectral features large enough for your camera sensor to detect. This module transforms the UVEX into an instrument capable of contributing to pro-am research campaigns that require higher resolving power than the stock configuration can provide.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eChoosing Your Grating: 1200 l\/mm vs. the 600 l\/mm Standard\u003c\/h3\u003e\n\u003cp\u003eThe primary trade-off for higher resolution is a reduction in the spectral range captured in a single exposure. While the standard 600 l\/mm grating provides a balanced view of a wide wavelength range, the 1200 l\/mm grating focuses on a smaller segment of the spectrum with significantly greater detail.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003e1200 l\/mm Grating:\u003c\/strong\u003e Choose this for targeted studies of specific spectral lines (like H-alpha or Sodium D-lines) where maximum detail is the goal.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003e600 l\/mm Grating (Standard):\u003c\/strong\u003e Ideal for general stellar classification and capturing broad spectral features across a wide range of wavelengths in one shot.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eLower Density Gratings (e.g., 300 l\/mm):\u003c\/strong\u003e Best for low-resolution survey work, classifying faint objects like supernovae, or capturing the entire visible spectrum of a star at once.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the main advantage of the Shelyak 1200 l\/mm grating over the standard 600 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary advantage is \u003cstrong\u003edoubled spectral resolution\u003c\/strong\u003e. The 1200 l\/mm grating spreads light out more, allowing you to see finer details and separate spectral lines that would appear blended together with the standard 600 l\/mm grating. This is essential for detailed scientific analysis of specific spectral features.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen should I use a lower resolution grating instead of this 1200 l\/mm module for the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eUse a lower-density grating (like the optional 300 l\/mm or 150 l\/mm) when your priority is capturing the widest possible wavelength range in a single image, or when observing very faint objects. Lower resolution concentrates the light, improving the signal-to-noise ratio for targets like quasars, comets, or faint supernovae where detailed line profiles are less critical than initial classification.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 1200 l\/mm UVEX grating to study the H-alpha line of Be stars?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an ideal application. The high resolution of the 1200 l\/mm grating is perfectly suited for resolving the complex and variable emission profiles of the H-alpha line in Be stars. This allows you to track changes in the star's circumstellar disk, which is a key area of pro-am collaborative research.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 1200 l\/mm grating affect the wavelength range I can capture with the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe 1200 l\/mm grating significantly \u003cstrong\u003enarrows the spectral range\u003c\/strong\u003e that fits onto your camera's sensor in a single exposure compared to the 600 l\/mm grating. You will be capturing a smaller slice of the spectrum, but with much greater detail within that slice. You may need to take multiple exposures, rotating the grating slightly between each, to cover a wider region of interest.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eIs installing the 1200 l\/mm grating module in the UVEX spectroscope difficult?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the UVEX is designed for interchangeable gratings. The modules are made to be easily swappable by the user, allowing you to change the resolution of the spectroscope in the field to match your observing target and scientific goals for the night.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of telescope is best for high-resolution spectroscopy with the UVEX and the 1200 l\/mm grating?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eHigh-resolution spectroscopy requires a strong signal. Therefore, telescopes with larger apertures (typically 8\" or greater) are recommended to gather enough light, especially for fainter stars. Schmidt-Cassegrains (SCTs) and Ritchey-Chrétiens (RCs) are common choices due to their large apertures and comfortable back focus, which easily accommodates the spectroscope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eGrating Density\u003c\/td\u003e\n\u003ctd\u003e1200 lines\/mm\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eCompatibility\u003c\/td\u003e\n\u003ctd\u003eShelyak UVEX Spectroscope\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943052538141,"sku":"SHK-SE0245","price":992.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-UVEX-150-l-mm-1_bdc204a7-8ffd-43bd-b3b3-805d4a5ab9ff.jpg?v=1789616475"},{"product_id":"shelyak-se0246","title":"Shelyak Grating module for the UVEX - 1800 l\/mm","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eGrating Density: 1800 lines\/mm\u003c\/li\u003e\n\u003cli\u003eInstrument Compatibility: Shelyak UVEX Spectroscope\u003c\/li\u003e\n\u003cli\u003ePrimary Application: High-resolution spectroscopy\u003c\/li\u003e\n\u003cli\u003eModular Design: Interchangeable with other UVEX gratings\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eGrating module for the UVEX - 1800 l\/mm\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Grating Module for the UVEX elevates your spectroscope's capabilities with a line density of 1800 lines per millimeter (l\/mm). This module offers three times the line count of the standard 600 l\/mm grating included with the UVEX, delivering the highest possible spectral dispersion and resolution available for the instrument.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e1800 l\/mm: The Highest Resolution for UVEX Spectroscopy\u003c\/h3\u003e\n\u003cp\u003eThis grating is a specialized tool designed for maximum detail. The high 1800 l\/mm density spreads starlight across a greater number of pixels, allowing you to resolve extremely fine spectral features that are invisible with lower-dispersion gratings. It is the ideal choice for advanced projects like measuring the Doppler shift in binary star systems, analyzing the detailed atmospheric lines of bright stars, or separating close emission lines in planetary nebulae.\u003c\/p\u003e\n\u003cp\u003eThe trade-off for this high resolution is a reduction in brightness and a narrower spectral range captured in a single exposure. This makes the 1800 l\/mm grating best suited for brighter targets where photon signal is abundant and fine detail is the primary scientific goal.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eThe 5-Grating UVEX Modular System\u003c\/h3\u003e\n\u003cp\u003eThe UVEX spectroscope is engineered around a modular, user-interchangeable grating system. This allows you to adapt the instrument's resolution to match your specific target and observing conditions. The 1800 l\/mm grating represents the pinnacle of this system for high-resolution work.\u003c\/p\u003e\n\u003cp\u003eYou can easily swap it with the standard 600 l\/mm grating or other optional modules, including the 150, 300, and 1200 l\/mm versions. This flexibility transforms the UVEX from a single instrument into a versatile analytical platform, capable of everything from low-resolution surveys of faint objects to high-precision analysis of bright stars.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003e1800 l\/mm vs. 600 l\/mm: Choosing the Right Dispersion\u003c\/h3\u003e\n\u003cp\u003eSelecting the correct grating is critical for successful spectroscopy. The choice between the optional 1800 l\/mm module and the standard 600 l\/mm grating depends entirely on your target.\u003c\/p\u003e\n\u003cul\u003e\n\u003cli\u003e\n\u003cstrong\u003eStandard 600 l\/mm Grating:\u003c\/strong\u003e This is the workhorse for general spectroscopy. It produces brighter spectra and captures a wider range of wavelengths in one shot, making it ideal for classifying stars, observing fainter objects like supernovae, or conducting initial survey work.\u003c\/li\u003e\n\u003cli\u003e\n\u003cstrong\u003eOptional 1800 l\/mm Grating:\u003c\/strong\u003e This is a specialist's tool. Use it when you have a bright target and a specific scientific question that requires resolving very fine details. It prioritizes resolution over all other factors.\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary advantage of the 1800 l\/mm grating for the UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary advantage is its \u003cstrong\u003ehigh spectral resolution\u003c\/strong\u003e. With 1800 lines per millimeter, it spreads light out more than any other UVEX grating, allowing you to resolve very fine, closely spaced details in a spectrum that would be blurred together at lower dispersions.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhen would I use the 1800 l\/mm grating to observe a star like Vega (Alpha Lyrae)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eFor a bright A-type star like Vega, the 1800 l\/mm grating would be excellent for studying the detailed profile of its prominent hydrogen absorption lines (the Balmer series). The high resolution would allow you to detect subtle asymmetries or Doppler shifts caused by stellar rotation or other atmospheric phenomena.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes using the 1800 l\/mm grating have any disadvantages compared to the standard 600 l\/mm?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. Because the light is spread out more, the resulting spectrum is \u003cstrong\u003edimmer\u003c\/strong\u003e and covers a \u003cstrong\u003enarrower wavelength range\u003c\/strong\u003e in a single image. This means it requires longer exposure times or brighter targets and may require taking multiple images to cover the same spectral range as the 600 l\/mm grating.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow difficult is it to install the 1800 l\/mm grating module in the UVEX spectroscope?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe UVEX is designed for user-swappable gratings. The process is straightforward and involves removing the access panel and carefully exchanging the modules. For detailed instructions, please refer to the main Shelyak UVEX instrument manual.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the UVEX 1800 l\/mm grating to study a faint galaxy like the Whirlpool Galaxy (M51)?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eIt is not recommended. The high dispersion of the 1800 l\/mm grating would spread the very faint light from M51 too thinly, resulting in an unusable spectrum with a very low signal-to-noise ratio. A low-dispersion grating, like the standard 600 l\/mm or optional 150 l\/mm, is required for such faint, extended objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat other gratings are available for the Shelyak UVEX?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe UVEX modular system includes a family of gratings to suit different scientific goals. In addition to the standard 600 l\/mm and this 1800 l\/mm module, Shelyak offers optional gratings of \u003cstrong\u003e150 l\/mm\u003c\/strong\u003e, \u003cstrong\u003e300 l\/mm\u003c\/strong\u003e, and \u003cstrong\u003e1200 l\/mm\u003c\/strong\u003e.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943052800285,"sku":"SHK-SE0246","price":992.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Grating-module-for-the-UVEX-150-l-mm-1_3dc2d9fa-d61e-4483-9460-b6cf48cfa251.jpg?v=1789616483"},{"product_id":"shelyak-se0248","title":"Shelyak 530 nm UVEX order filter kit","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eDesigned for the Shelyak Instruments UVEX Spectrograph\u003c\/li\u003e\n\u003cli\u003eSuppresses 2nd Order Near-Infrared (IR) Spectral Contamination\u003c\/li\u003e\n\u003cli\u003eEnsures Cleaner, More Accurate Spectroscopic Data\u003c\/li\u003e\n\u003cli\u003eMounts directly to the rear of the UVEX slot support\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section-center\"\u003e\n      \u003ch2\u003e530 nm UVEX order filter kit\u003c\/h2\u003e\n      \u003cp\u003eThe 530 nm UVEX order filter kit is a critical accessory for the Shelyak UVEX spectrograph, engineered to solve the specific problem of second-order spectral contamination. When observing targets with significant near-infrared (IR) emissions, this filter prevents false signals from appearing in your visible spectrum, ensuring the data you collect is clean. By suppressing this unwanted second-order light, the 530 nm filter allows for unambiguous identification of spectral features.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n  \u003cdiv class=\"DAV-bg-light\"\u003e\n    \u003cdiv class=\"DAV-section\"\u003e\n      \u003ch3\u003eEliminate Spectral Contamination: The 530nm UVEX Order Filter\u003c\/h3\u003e\n      \u003cp\u003eIn spectroscopy, a diffraction grating can produce multiple spectra, or \"orders.\" The second order of a near-IR wavelength can overlap with the first-order spectrum of a visible wavelength, creating an artifact that corrupts your data. This 530 nm order filter is designed to block this specific type of contamination, making it essential for achieving scientific-grade results with your UVEX.\u003c\/p\u003e\n      \u003cp\u003eThe filter is designed for straightforward integration, screwing directly onto the rear of the UVEX's slot support. This placement ensures it effectively filters the light path without complicating your imaging train, resulting in cleaner spectra and more reliable measurements of stellar classifications, emission lines, and other astrophysical phenomena.\u003c\/p\u003e\n    \u003c\/div\u003e\n  \u003c\/div\u003e\n\n\u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary purpose of the 530 nm UVEX order filter kit?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe primary purpose of the 530 nm UVEX order filter is to \u003cstrong\u003esuppress the second order of the near-infrared (IR) spectrum\u003c\/strong\u003e. This prevents false spectral lines from IR sources from contaminating your visible-light spectrum, leading to cleaner and more accurate scientific data.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWhen observing a Be star with my UVEX, do I need the 530 nm order filter?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eYes, observing a Be star is an excellent use case for this filter. Be stars often have strong hydrogen-alpha emission in the red part of the spectrum and can have significant IR emission. Using the 530 nm filter ensures that the second-order light from this IR emission does not create artifacts in the blue-green portion of your spectrum, allowing for accurate characterization of the star's properties.\u003c\/p\u003e\n  \u003c\/div\u003e\n    \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIf I'm observing the H-alpha line at 656nm with my UVEX, is this filter necessary?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eWhen your primary target is a red-end wavelength like H-alpha (656nm), which is above the filter's likely cutoff, this filter is generally not needed and would block the light you intend to measure. This filter is most useful when you are observing targets in the blue and green parts of the spectrum (below 530 nm) and want to eliminate contamination from IR sources.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eHow is the 530 nm UVEX order filter installed?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eThe filter is designed to be screwed directly onto the \u003cstrong\u003erear of the UVEX slot support\u003c\/strong\u003e. This simple and secure mounting method integrates the filter seamlessly into the spectrograph's optical path.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eWill the 530 nm UVEX filter impact the brightness or focus of my spectrum?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eLike any filter, it will cause a minor reduction in light throughput, but this is a necessary trade-off for eliminating significant spectral contamination. The impact on focus should be negligible, as it is a thin, high-quality optical component designed specifically for the UVEX system.\u003c\/p\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion\"\u003e\n    \u003ch3 class=\"DAV-accordion-Q\"\u003eIs the 530 nm order filter required for all observations with the Shelyak UVEX?\u003c\/h3\u003e\n  \u003c\/div\u003e\n  \u003cdiv class=\"DAV-accordion-A\"\u003e\n    \u003cp\u003eNo, it is not required for all observations. It is specifically needed when you are concerned about second-order contamination from near-IR sources. If you are observing targets with little to no IR emission, or if your scientific goals are not impacted by potential low-level contamination, you may not need to use it.\u003c\/p\u003e\n  \u003c\/div\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_UVEX_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak UVEX Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943053488413,"sku":"SHK-SE0248","price":258.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-530-nm-UVEX-order-filter-kit-1_c63b0dd0-657d-4ba4-88f8-6be4e6469bc9.jpg?v=1789616501"},{"product_id":"shelyak-se0275","title":"Shelyak Alpy 200 Optical Core Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConverts an Alpy 600 into an Alpy 200 Spectrograph\u003c\/li\u003e\n\u003cli\u003eResolving Power of R~130 with a 23µm slit\u003c\/li\u003e\n\u003cli\u003eFast F\/4 Aperture for high light throughput\u003c\/li\u003e\n\u003cli\u003eOptimized for spectroscopy of faint targets\u003c\/li\u003e\n\u003cli\u003eRequires existing Alpy 600 mechanical parts and slit\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAlpy 200 Optical Core Module\u003c\/h2\u003e\n\u003cp\u003eThe Alpy 200 optical core module transforms your existing Alpy 600 into a fast F\/4 spectrograph, delivering a resolving power of R~130 for analyzing the faintest targets. This module requires you to reuse the mechanical housing and a 23µm slit from your Alpy 600, providing a low-cost path to low-resolution spectroscopy.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eConvert Your Alpy 600 to an R~130 Spectrograph\u003c\/h3\u003e\n\u003cp\u003eThis module is designed specifically for astronomers who already own a Shelyak Alpy 600 spectrograph. By swapping the internal optics, you can repurpose your instrument for a different class of scientific work without purchasing an entirely new device. This is the optical heart of the Alpy 200, allowing you to achieve a resolving power of R~130.\u003c\/p\u003e\n\u003cp\u003ePlease note this is not a complete spectrograph. It is an upgrade component that relies on the mechanical chassis and the slit from your Alpy 600, which are not included with this module. The conversion allows you to switch between high-resolution and high-sensitivity setups as your observing targets change.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAlpy 200 vs. Alpy 600: The F\/4 Advantage for Faint Targets\u003c\/h3\u003e\n\u003cp\u003eThe fundamental trade-off in spectroscopy is between resolution and sensitivity. While the Alpy 600 provides higher resolution for detailed analysis of brighter stars, the Alpy 200's fast F\/4 optical design is engineered to maximize photon collection on faint, extended objects. You sacrifice resolving power to gain critical signal-to-noise on challenging targets.\u003c\/p\u003e\n\u003cp\u003eThis makes the Alpy 200 configuration ideal for classifying supernovae, observing the spectral features of faint comets, or capturing data from low-surface-brightness nebulae. When every photon counts more than fine spectral detail, the R~130, F\/4 setup of the Alpy 200 is the superior choice.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat is the primary purpose of the Alpy 200 optical core module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Alpy 200 optical core module is an upgrade component that converts an existing Shelyak Alpy 600 spectrograph into a low-resolution, high-sensitivity Alpy 200. Its fast \u003cstrong\u003eF\/4\u003c\/strong\u003e design and \u003cstrong\u003eR~130\u003c\/strong\u003e resolving power are optimized for capturing spectra from very faint astronomical objects.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need to own an Alpy 600 to use the Alpy 200 core module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes. This product is \u003cstrong\u003enot a standalone spectrograph\u003c\/strong\u003e. It is designed exclusively for owners of the Alpy 600, as it requires the reuse of the Alpy 600's mechanical body and slit assembly.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat parts from my Alpy 600 are required for the Alpy 200 conversion?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYou will need to use the complete mechanical housing of your Alpy 600 as well as the slit. The slit is a critical component that is not supplied with the Alpy 200 core module. The resolving power of R~130 is specified with a 23µm slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow would the Alpy 200 module perform when observing a faint supernova in a distant galaxy?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThis is precisely the scenario where the Alpy 200 excels. For a faint supernova, collecting enough photons to get a usable signal is the main challenge. The fast \u003cstrong\u003eF\/4\u003c\/strong\u003e optics gather light efficiently, allowing you to obtain a low-resolution (\u003cstrong\u003eR~130\u003c\/strong\u003e) spectrum to classify the supernova type (e.g., Type Ia, Type II) and monitor its evolution, which would be difficult or impossible with a slower, higher-resolution spectrograph on the same telescope.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I choose the Alpy 200 module's R~130 resolution over the Alpy 600's for a faint comet?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eA faint comet's spectrum is characterized by broad emission bands from molecules like C2 and CN. High resolution is not needed to identify these features. The Alpy 200's low resolution and high throughput ensure you can capture a strong signal from the faint coma, making it a much more effective tool for cometary science than the higher-resolution Alpy 600 in this case.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat does the F\/4 aperture of the Alpy 200 module mean for my observations?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eAn \u003cstrong\u003eF\/4\u003c\/strong\u003e aperture signifies a very \"fast\" optical system, meaning it concentrates light onto the sensor more intensely than a \"slower\" system (like an F\/8 or F\/10). This drastically reduces exposure times needed to achieve a good signal-to-noise ratio, which is essential for faint, diffuse targets that require every available photon.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolving Power\u003c\/td\u003e\n\u003ctd\u003eR ~130 with 23µm slit\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eAperture\u003c\/td\u003e\n\u003ctd\u003eF\/4\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eAlpy 200 Optical Core Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_200_Core_Module_Assembly_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 200 Core Module Assembly Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Backfocus_Diagram.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Backfocus Diagram\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943054700829,"sku":"SHK-SE0275","price":466.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Alpy-200-optical-core-module-1_a104d942-b8b9-405d-ab01-8e5a166f2d2e.jpg?v=1789616531"},{"product_id":"shelyak-se0276","title":"Shelyak Alpy 200 Switch Module","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003eConverts an Alpy 600 system for low-resolution spectroscopy\u003c\/li\u003e\n\u003cli\u003eResolving Power: R ~130 with a 23µm slit\u003c\/li\u003e\n\u003cli\u003eOptimized for F\/4 telescope systems\u003c\/li\u003e\n\u003cli\u003eTool-free installation with 6 knurled screws\u003c\/li\u003e\n\u003cli\u003eEnables spectral acquisition of very faint targets\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c!-- more --\u003e\n\u003cul class=\"tabs\"\u003e\n\u003cli class=\"active\"\u003eDescription\u003c\/li\u003e\n\u003cli\u003eFAQ\u003c\/li\u003e\n\u003cli\u003eSpecifications\u003c\/li\u003e\n\u003cli\u003eIn the Box\u003c\/li\u003e\n\u003cli\u003eDownloads\u003c\/li\u003e\n\u003cli\u003eWarranty\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cul class=\"tabs-content\"\u003e\n\u003cli class=\"active\"\u003e\n\u003cdiv\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section-center\"\u003e\n\u003ch2\u003eAlpy 200 Switch Module\u003c\/h2\u003e\n\u003cp\u003eThe Alpy 200 Switch Module lets you convert your existing Alpy 600 setup for low-resolution spectroscopy, achieving a resolving power of R ~130 with a 23µm slit. Designed for telescopes working at an F\/4 aperture, this module enables a rapid, tool-free swap to capture spectra from faint targets that are inaccessible to higher-resolution systems.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eFrom R~600 to R~130: A 2-Minute Spectrograph Swap\u003c\/h3\u003e\n\u003cp\u003eThis module is engineered for observers who already own the Alpy 600 guiding and spectrograph assembly. It allows you to quickly adapt your instrumentation to the target at hand, swapping from high to low resolution in a matter of minutes. The exchange is purely mechanical; simply undo the 6 knurled screws by hand, lift out the Alpy 600 module, and drop the Alpy 200 in its place.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eAlpy 200 vs. Alpy 600: Prioritizing Signal for Faint Targets\u003c\/h3\u003e\n\u003cp\u003eThe choice between the Alpy 600 and Alpy 200 is a direct trade-off between detail and depth. While the Alpy 600 provides higher resolution for detailed analysis of bright stars, the Alpy 200's R ~130 resolving power spreads the target's light over far fewer pixels. This concentration of photons is essential for successfully recording a signal from extremely faint objects like supernovae, distant quasars, and faint comets.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-bg-light\"\u003e\n\u003cdiv class=\"DAV-section\"\u003e\n\u003ch3\u003eCritical Workflow: Slit Selection and Recalibration for the F\/4 System\u003c\/h3\u003e\n\u003cp\u003eTo maintain data integrity, it's crucial to take new reference frames—specifically flats and calibration lamp spectra—after swapping modules. Note that this is the Alpy 200 module body only and is sold without a slit. You must order the appropriate slit for your telescope and camera configuration separately to complete the spectrograph.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhy would I use the Alpy 200 switch module instead of just my Alpy 600?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe Alpy 200 module is for capturing spectra of very faint targets. Its low resolving power (R ~130) concentrates starlight, allowing you to get a usable signal on objects that would be too dim for the higher-resolution Alpy 600. It turns your existing system into a dual-purpose instrument.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDoes the Alpy 200 switch module come with a slit?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, the Alpy 200 switch module is sold as the module body only. You must purchase a slit separately that matches your telescope and camera setup. This allows you to customize the instrument for your specific needs.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow long does it take to swap the Alpy 200 module into my Alpy 600 setup?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe swap is designed to be very fast, typically taking only a few minutes. The module is secured by 6 knurled screws that can be loosened and tightened by hand, requiring no tools for the exchange.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eI want to capture the spectrum of a faint supernova with my C11 at F\/10. Is the Alpy 200 module the right choice?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, absolutely. A faint supernova is a perfect target for the Alpy 200 module. Its low resolving power is specifically designed to maximize the signal-to-noise ratio on such faint point sources, where simply detecting and classifying the spectrum is the primary goal.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the Alpy 200 switch module on a fast F\/4 Newtonian to study cometary spectra?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, the Alpy 200 is optimized for an F\/4 aperture, making it an excellent match for fast Newtonian astrographs. This combination is ideal for studying the faint, diffuse spectra of comets, allowing you to capture the entire coma within the slit.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need a separate camera for the Alpy 200 switch module?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eA separate camera is not required, as you can move your existing acquisition camera from the Alpy 600 to the Alpy 200 module. However, having a dedicated camera for each module makes the switch even faster and simpler, as you would not need to refocus the camera each time.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ctable class=\"DAV-specifications\"\u003e\n\u003ctbody\u003e\n\u003ctr\u003e\n\u003ctd\u003eResolving Power\u003c\/td\u003e\n\u003ctd\u003eR ~130 (with 23µm slit)\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003ctr\u003e\n\u003ctd\u003eNative Aperture\u003c\/td\u003e\n\u003ctd\u003eF\/4\u003c\/td\u003e\n\u003c\/tr\u003e\n\u003c\/tbody\u003e\n\u003c\/table\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eAlpy 200 Switch Module\u003c\/p\u003e\n\u003cp class=\"DAV-item-subtitle\"\u003e× 1\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003cul class=\"DAV-grid\"\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_200_Core_Module_Assembly_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 200 Core Module Assembly Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_600_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy 600 Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Alpy_Backfocus_Diagram.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Alpy Backfocus Diagram\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003cli class=\"DAV-grid-item\"\u003e\u003ca href=\"https:\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak_Demetra_Software_Manual.pdf\" target=\"_blank\"\u003e\u003csvg class=\"DAV-img-box\" viewbox=\"0 0 512 512\" xmlns=\"http:\/\/www.w3.org\/2000\/svg\"\u003e\u003cpath d=\"M0 64C0 28.7 28.7 0 64 0L224 0l0 128c0 17.7 14.3 32 32 32l128 0 0 144-208 0c-35.3 0-64 28.7-64 64l0 144-48 0c-35.3 0-64-28.7-64-64L0 64zm384 64l-128 0L256 0 384 128zM176 352l32 0c30.9 0 56 25.1 56 56s-25.1 56-56 56l-16 0 0 32c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-48 0-80c0-8.8 7.2-16 16-16zm32 80c13.3 0 24-10.7 24-24s-10.7-24-24-24l-16 0 0 48 16 0zm96-80l32 0c26.5 0 48 21.5 48 48l0 64c0 26.5-21.5 48-48 48l-32 0c-8.8 0-16-7.2-16-16l0-128c0-8.8 7.2-16 16-16zm32 128c8.8 0 16-7.2 16-16l0-64c0-8.8-7.2-16-16-16l-16 0 0 96 16 0zm80-112c0-8.8 7.2-16 16-16l48 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 32 32 0c8.8 0 16 7.2 16 16s-7.2 16-16 16l-32 0 0 48c0 8.8-7.2 16-16 16s-16-7.2-16-16l0-64 0-64z\" fill=\"#0047a7\"\u003e\u003c\/path\u003e\u003c\/svg\u003e\n\u003cdiv\u003e\n\u003cp class=\"DAV-item-title\"\u003eShelyak Demetra Software Manual\u003c\/p\u003e\n\u003c\/div\u003e\n\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003c\/li\u003e\n\u003cli\u003e\n\u003ca href=\"https:\/\/davidastro.com\/pages\/shelyak-warranty-policy\" rel=\"noopener\" target=\"_blank\"\u003eShelyak 1-Year Warranty\u003c\/a\u003e\n\u003c\/li\u003e\n\u003c\/ul\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":52943054897437,"sku":"SHK-SE0276","price":940.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Alpy-200-swich-module-1_cb9e328a-3b39-4e79-a4cf-6469cdbc84aa.jpg?v=1789616539"}],"url":"https:\/\/davidastro.com\/en-us\/collections\/shelyak-spectroscopes.oembed","provider":"David Astro","version":"1.0","type":"link"}