What is the purpose of the dual slits on the 23/200µm Photometric Slit?
The two slits serve two different scientific goals. The narrow 23µm slit is used to achieve the highest possible spectral resolution for detecting fine absorption or emission lines. The wide 200µm slit 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.
When should I use the 23µm slit with my Alpy 600?
Use 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.
When is the 200µm slit the right choice for the Photometric Slit?
The 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.
Is this Photometric Slit compatible with all Shelyak spectrographs?
No, this slit is specifically designed for use with the Shelyak Alpy 600 and Shelyak UVEX spectroscope models. It is not compatible with other instruments like the Lhires III or LISA.
Do I need other accessories to use the 23/200µm Photometric Slit?
Yes, this photometric slit must be used with the Alpy Guiding Module. The guiding module is required to position the target star accurately on the desired slit and maintain that position during an exposure.
How does the 200µm slit on the Photometric Slit help with poor seeing?
Atmospheric 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.