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--- kosmos [2023/07/04 16:56] – [Aligning the mask and observing] jnb
+++ kosmos [2026/01/30 05:13] (current) – external edit 127.0.0.1
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+===== KOSMOS =====
 The Kitt Peak Ohio State Multi-Object Spectrograph (KOSMOS) was loaned to ARC by NOAO for use on the 3.5m telescope.  Because the KOSMOS instrument was modified from its original state in order to be installed on the ARC 3.5m telescope at APO, we now refer to this instrument as KOSMOS II.
-A quick-look fact sheet from September, 2019, about KOSMOS II is available attached below.
+A quick-look fact sheet about KOSMOS II from September 2019 is available {{:wiki:kosmos:kosmos_quick_look_rev1_.pdf|here}}. A
+[[https://docs.google.com/document/d/1aVzRTs3c2Qw2ouDpa6S4oDPSPi5ijx5LKGN9aSaHe-4/edit?usp=sharing|Google doc]]
+contains the latest edits.
-The google doc containing the latest edits is located at https://docs.google.com/document/d/1aVzRTs3c2Qw2ouDpa6S4oDPSPi5ijx5LKGN9aSaHe-4/edit?usp=sharing
+KOSMOS can be used in longslit mode, but also with custom slitmasks, as described in more detail below.
-{{medialist>wiki:kosmos:*}}
+[[https://www.apo.nmsu.edu/mainpage/kosmos/kosmosguide/|KOSMOS instrument manual on APO website]] (does not include slitmask information).
-At the Users Committee meeting on 8/2/2022, someone asked whether any KOSMOS users have posted or shared recommendations for KOSMOS flat fielding given the bright rows in the flats attributed to the zeroth order. The issue is described here: [[https://www.apo.nmsu.edu/arc35m/Instruments/KOSMOS/userguide.html#4p3]] ; the question was how are people are handling this in the data reduction? Jon Holtzman replies that he got some reasonable results just by fitting and subtracting a Gaussian with a linear background at the Littrow ghost location from flats (specifically, using a running median across columns). If people continue to have issues with this, please contact your Users Committee rep so this can be discussed at a future meeting.
+==== Features / issues ====
+* There is significant pattern noise on the detector that varies from frame to frame, likely providing a larger noise floor than expected from the readout noise alone
+* There is a Littrow ghost that can appear. Note that this can be seen in flat fields, leading to issues in flat-fielded images if it is not removed from the flat!
+* KOSMOS has internal calibration lamps, but the external truss lamps can also be used. There is some flexure in the instrument at different rotator angles. It should be
+possible to correct for these using more frequent internal lamp images, but it is also likely that sky lines can be used to achieve this if exposures are sufficiently
+long enough to see sky lines, and if you are working in a region where there are sky lines!
+==== Data reduction ====
+* IRAF-based alternatives
+  * standard IRAF routines (onedspec and twodspec) can be used
+* Python alternatives
+  * [[https://github.com/jradavenport/pykosmos|PyKosmos]] : package developed by Jim Davenport for reduction of long slit data
+  * [[https://pyvista.readthedocs.io|pyvista]] : a general basic, pedagogical, reduction package that has configuration files for KOSMOS and a notebook demonstrating basic reduction. This has the capability to hand both longslit and slitmask data
+    * Abdullah Korra at the College of Idaho wrote a [[https://github.com/mwbest/CofI_2025|meta package]] to handle slitmask data that uses pyvista under an additional layer of abstraction that allows users to select files to process graphically
+  * [[https://PypeIt.readthedocs.io|PypeIt]] : a general package for optimal extraction of spectrograph data, including echelle data. Work is in progress on a configuration for KOSMOS
+==== KOSMOS multi-object slit masks ====
-====== KOSMOS multi-object slit masks ======
 In Summer and Fall 2022, Joe Burchett, Jon Holtzman, and Bill Ketzeback commissioned the multi-object mode of KOSMOS.  To use this mode, one must design a slitmask and have it fabricated and shipped it to the mountain.  The masks are fabricated by a company in Tempe, AZ.  Therefore, we recommend starting the mask design process well in advance of any run where user intend observe with them.  Note that Burchett has a grant account at NMSU to pay for the mask fabrication and shipping, so mask orders should go through him (jnb at nmsu.edu).  Please have mask designs ready by three weeks before the run.
 Note that the mask wheel for KOSMOS only holds 6 masks and one should be left open for imaging. It may be desirable to have another of the slots left for a long slit. So 4-5 slit masks per night of observations may be ambitious. Making masks for a large number of fields should be avoided for beginning users.
-===== Mask design =====
+=== Mask design ===
 Bill has set up a virtual machine at APO with the KOSMOS mask design software, KMS.  To access the machine, you'll first need VPN access, a VPN client, and a VNC viewer.  OpenVPN and RealVNC are popular choices for these last two.  For VPN access, contact Shane Thomas (shane at apo.nmsu.edu).
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   * Once you've output the design (it makes two files), notify Bill (bketzeba at apo.nmsu.edu), and he and Joe will inspect them and initiate the fabrication order.
-===== Aligning the mask and observing =====
+=== Aligning the mask and observing ===
-The following is a mask alignment and observing procedure kindly provided by Amanda Townsend.  Holtzman and Burchett are currently developing software to help automate several steps of the mask alignment process, but we advise that observers fully understand the steps involved!
-- Observer should take slit mask alignment map images (initial can be
+The following is a mask alignment and observing procedure kindly provided by Amanda Townsend.  Holtzman and Burchett have developed software to help automate several steps of the mask alignment process, but we advise that observers fully understand the steps involved!
-done at start of night with cals) = dim truss qtz OR internal qtz (or arc)
-with ND5 filter. Match up alignment map to finder chart with slits, figure
+  - Observer should take slit mask alignment map images (initial can be done at start of night with cals) = dim truss qtz OR internal qtz (or arc) with ND5 filter. Match up alignment map to finder chart with slits, figure out which are which ahead of time to save time later!
-out which are which ahead of time to save time later!
+  - Obs spec should set instrument to kimage to keep focal plane same as image. Corollary: do NOT invert images in ds9! This will make offsets very confusing. Rather, invert your finder chart.
-- Obs spec should set instrument to kimage to keep focal plane same as
+  - Slew to field with rot +90 object.
-image. Corollary: do NOT invert images in ds9! This will make offsets very
+  - Take image exposure with disperser = EMPTY and slit = EMPTY to see field.
-confusing. Rather, invert your finder chart.
+  - Match up image to finder chart. Invert finder chart to match if necessary, but again, do NOT invert kosmos images.
-- Slew to field with rot +90 object.
+  - For each of the (probably 4-5) alignment/register stars, which are the square slits on the mask, determine the (x,y) coords in the alignment map exposure as well as the (x,y) coords of the star in the image you just took.
-- Take image exposure with disperser = EMPTY and slit = EMPTY to see field.
+  - Measure x and y offsets for each alignment star: (star-slit)*(plate scale=.258) = offset in arc seconds, find average x and average y offsets for all alignment stars.
-- Match up image to finder chart. Invert finder chart to match if
+  - Make offsets in TUI Offset window. Select "object arc xy" from the dropdown, and enter x and y offsets. To move star to left = move telescope right = +x offset; to move star down = move telescope up = +y offset. You can also use the nudger (nudger pushes star/pulls telescope).
-necessary, but again, do NOT invert kosmos images.
+  - Start NA2 guider!
-- For each of the (probably 4-5) alignment/register stars, which are the
+  - Take another field exposure, blink between this image and your alignment map in ds9 to check alignment (and/or check pixel positions or copy regions from one frame to the other).
-square slits on the mask, determine the (x,y) coords in the alignment map
+  - If they are still far enough off, iterate; otherwise put in your slit mask but NOT the disperser and take another exposure. Look to see where the stars and targets fall in their slits.
-exposure as well as the (x,y) coords of the star in the image you just
+  - Center up the register stars in the squares. Science targets will be off-center in slits for sky measurements.
-took.
+  - Put in disperser now. Optional: short exposure to check?
-- Measure x and y offsets for each alignment star: (star-slit)*(plate
+  - Science exposures!
-scale=.258) = offset in arc seconds, find average x and average y offsets
-for all alignment stars.
+=== Reducing the data ===
-- Make offsets in TUI Offset window. Select "object arc xy" from the
-dropdown, and enter x and y offsets. To move star to left = move telescope
-right = +x offset; to move star down = move telescope up = +y offset. You
-can also use the nudger (nudger pushes star/pulls telescope).
-- Start NA2 guider!
-- Take another field exposure, blink between this image and your
-alignment map in ds9 to check alignment (and/or check pixel positions or
-copy regions from one frame to the other).
-- If they are still far enough off, iterate; otherwise put in your slit
-mask but NOT the disperser and take another exposure. Look to see where
-the stars and targets fall in their slits.
-- Center up the register stars in the squares. Science targets will be
-off-center in slits for sky measurements.
-- Put in disperser now. Optional: short exposure to check?
-- Science exposures!
-===== Reducing the data =====