{"title":"Grating Filters \u0026 Spectrograph Kits","description":null,"products":[{"product_id":"shelyak-star-analyser-100","title":"Analyseur d'étoiles Shelyak 100","description":"\u003c!-- more --\u003e \u003cp\u003e\u003cspan\u003eLe Star Analyzer 100 est un réseau de diffraction en transmission 100 lignes\/mm à haut rendement, blazé au premier ordre. Il est monté dans une cellule filetée standard de 1,25 pouce de diamètre, pour être compatible avec la plupart des télescopes et accessoires.\u003c\/span\u003e\u003c\/p\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":44968070807837,"sku":"SHK-PF0003","price":265.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/products\/PF0003-Star-Analyser_5__12858.1671742177.1280.1280.png?v=1684348653"},{"product_id":"shelyak-star-analyser-200","title":"Analyseur d'étoiles Shelyak 200","description":"\u003c!-- more --\u003e\u003cp\u003e \u003cspan\u003eL'analyseur 200 est un réseau de diffraction en transmission 200 lignes\/mm à haut rendement, blazé au premier ordre. Il est monté dans une cellule filetée à profil bas standard de 1,25 pouce de diamètre, compatible avec la plupart des télescopes et accessoires ainsi que des roues à filtres minces.\u003c\/span\u003e\u003c\/p\u003e","brand":"Shelyak","offers":[{"title":"Default Title","offer_id":44968070971677,"sku":"SHK-PF0040","price":305.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/products\/pf0040-sa200-f-t210x156_158__03510.1671742470.1280.1280.png?v=1684348655"},{"product_id":"shelyak-op0094","title":"Shelyak Prism 3.8° for the Star Analyser","description":"\u003cul class=\"DAV-feature-list\"\u003e\n\u003cli\u003e3.8° prism angle precisely calculated for the Star Analyser\u003c\/li\u003e\n\u003cli\u003eImproves spectral resolution by approximately 20%\u003c\/li\u003e\n\u003cli\u003eAchieves a resolving power of R~130\u003c\/li\u003e\n\u003cli\u003eCorrects optical coma inherent in converging beam setups\u003c\/li\u003e\n\u003cli\u003eOptimized for advanced applications like nova and supernova characterization\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\u003ePrism 3.8° for the Star Analyser\u003c\/h2\u003e\n\u003cp\u003eThe Shelyak Prism 3.8° for the Star Analyser is an optical enhancement designed to increase its resolving power by approximately 20%. This accessory corrects for coma inherent in the Star Analyser's simple design, pushing its performance to a resolving power of R~130. By adding this 3.8° prism, you can extract more detailed spectral data from your existing 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\u003eCorrect Coma and Boost Resolution by 20% to R~130\u003c\/h3\u003e\n\u003cp\u003eThe Star Analyser's effectiveness comes from its simplicity—placing a diffraction grating directly into a telescope's converging light path. However, this introduces optical coma, which can soften spectral lines. The 3.8° Prism is specifically calculated to counteract this aberration, resulting in a sharper spectrum and an approximate 20% improvement in resolving power, achieving R~130.\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\u003eIs the 3.8° Prism Necessary for Your Spectroscopy?\u003c\/h3\u003e\n\u003cp\u003eThis prism is not a requirement for everyone. If you are using the Star Analyser to explore the basics of spectroscopy, the standard configuration is more than sufficient. However, if your goal is to push the instrument to its analytical limits for scientific contribution—such as characterizing the spectral evolution of novae or supernovae—this 3.8° prism is an essential upgrade.\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 Prism 3.8° for the Star Analyser?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe primary purpose of the 3.8° Prism is to improve the optical quality and resolution of spectra produced by a Star Analyser grating. It specifically corrects for \u003cstrong\u003ecoma\u003c\/strong\u003e, an aberration introduced when the grating is placed in a converging telescope beam, boosting resolution by about \u003cstrong\u003e20% to R~130\u003c\/strong\u003e.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eHow does the 3.8° Prism for the Star Analyser improve resolution?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe prism works by pre-correcting the light path before it reaches the diffraction grating. Its \u003cstrong\u003e3.8° wedge angle\u003c\/strong\u003e is precisely calculated to cancel out the coma that the simple, in-beam placement of the Star Analyser would otherwise create. This results in sharper, better-defined spectral lines and therefore higher effective resolution.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eDo I need this 3.8° Prism if I'm just starting with spectroscopy?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eNo, this prism is generally not necessary for beginners. The standard Star Analyser is an excellent tool for learning and discovering spectroscopy. This 3.8° prism is an upgrade for users who want to push the Star Analyser to its maximum performance for more demanding applications, like pro-am collaborations.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eCan I use the 3.8° Prism to study the spectrum of a bright supernova like SN 2023ixf?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eYes, this is an ideal application. Characterizing novae and supernovae is a key use case for this prism. The increased resolution to \u003cstrong\u003eR~130\u003c\/strong\u003e allows for better identification and monitoring of spectral features as the event evolves, providing more valuable scientific data than the Star Analyser could achieve on its own.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWhat kind of optical aberration does the Prism 3.8° correct in my f\/8 SCT?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe prism is designed to correct for \u003cstrong\u003ecoma\u003c\/strong\u003e that is introduced by the Star Analyser itself, not the telescope. When you place the grating in the converging f\/8 light cone of your SCT, coma is created. The 3.8° Prism is engineered to minimize this specific aberration, leading to a cleaner spectrum regardless of your telescope's native optical quality.\u003c\/p\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion\"\u003e\n\u003ch3 class=\"DAV-accordion-Q\"\u003eWill the 3.8° Prism for the Star Analyser change how I process my spectra?\u003c\/h3\u003e\n\u003c\/div\u003e\n\u003cdiv class=\"DAV-accordion-A\"\u003e\n\u003cp\u003eThe prism does not fundamentally change the data acquisition or processing workflow. You will still capture and calibrate your spectra using the same software (like Demetra). The primary difference will be in the final result: you will start with a sharper raw image, allowing for a more precise and higher-resolution final spectral profile.\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_Star_Analyser_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 Star Analyser 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":52943034614045,"sku":"SHK-OP0094","price":116.0,"currency_code":"CAD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0753\/5280\/1565\/files\/Shelyak-Prism-3-8-for-the-Star-Analyser-1_4033f785-10e6-4816-acc7-23ef1ad0c1cf.jpg?v=1789616029"},{"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":1297.0,"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-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":278.0,"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"}],"url":"https:\/\/davidastro.com\/fr-int\/collections\/grating-filters-and-kits.oembed","provider":"David Astro","version":"1.0","type":"link"}