**************** MMT Blue Channel **************** Overview ======== This file summarizes several instrument specific items for the MMTO's Blue Channel spectrograph. Wavelength Calibration ++++++++++++++++++++++ Templates were created in 2023 that cover the usable range for each of the following gratings: * 300GPM * 500GPM * 800GPM * 832GPM, both 1st and 2nd order * 1200GPM These templates have been tested against a wide range of archived data and have proven to be reliable. If there is an issue for some reason, the :ref:`wvcalib-holygrail` algorithm has also proven to work in many cases, especially with the 300GPM and 800GPM gratings. Observation and Reduction Setup +++++++++++++++++++++++++++++++ A few notes on setting up observations to work optimally with ``pypeit`` and what to watch out for in your :ref:`pypeit_file`: * :ref:`pypeit_setup` will group data by grating angle. Sometimes continuum flats can be shared between different grating angles and this will need to be edited by hand. * If a spectrograph component is in motion while an image is acquired, the position will be reported as ``moving`` in the image header. These images will get included in a :ref:`pypeit_file` with those ``moving`` values set to ``None``. Users will want to inspect those files and either remove them or edit the missing information by hand. * Images that are intended to be used as sky flats should have target set to ``skyflat`` in their headers so ``pypeit`` can identify them automatically. Otherwise they will need to be manually configured. * On-sky images that use the ``5.0x180`` slit are assumed to be standard star observations. Edit the resulting :ref:`pypeit_file` if this is not the case or otherwise define which observations are standard stars. * Images taken as part of spectrograph focus runs are automatically identified and configured as ``tilt`` images, but not ``arc``. This is because their line widths can vary by quite a bit and thus shouldn't be coadded to/averaged with in-focus ``arc`` images.