IR Data Reductions

The person in charge of the IR data reductions is Gaston Folatelli,
who is backed up by Nick Suntzeff. His duties involve checking the headers, making stacks,
spreading the images into the CSP database, and doing photometry. For these purposes
the following steps are required:
  • Make a working directory (suggested name, e.g.: 20020914_15) and read the raw data from the DVD into this subdirectory.
  • Get the observing log for the corresponding telescope + instrument here, so you can familiarize yourself with the data taken and the problems reported during the night.
  • Copy "snphot$README_SWO_RC" (or "snphot$README_DUP_WI") into current directory.
      Edit this reduction log file during the data processing.
  • Flat-fielding, sky-subtracting, and making stacks:
    • Load the package "p_reduce" (PANIC, RetroCam) or "w_reduce" (WIRC).
    • Run "p(w)_chk_headers" and check the results.
    • Run "p(w)_fix_headers".
    • Build the "*_pairs" files (i.e., "dflat_pairs", "tflat_pairs", "unc_pairs", "crd_pairs", "std_pairs", "alt_pairs").
    • Run "p(w)_mfid" to mark fiducial and standard stars if it's not been run during the night.
    • Check for the existence of all necessary calibration frames such as darks, flats, etc. If anyone is missing, build a "defaults" file to use calibrations from other nights.
    • Run "p(w)_1go" to process all the images and produce the stacks.
    • Check resulting stacks and mark the SNe using "chk_sn_stks".
  • Type "reset uparm=snphot$uparm_SWO_RC/" (or snphot$uparm_DUP_WI/)
  • Load 'snphot' package by typing 'snphot'.
  • Open DS9 window
  • Inspect the stack headers with the task chkhead.
  • Use the task headers to update the airmass, JD, and UT in the image headers.
  • Use the task spread to spread images in database.
      Note that this task will not copy the images to the database. It will just create a script file called "spread". To make the copy effective you need to type cl < spread Before using the script edit the file and get rid from this file the lines corresponding to dome or sky flats grabbed from other nights.
  • If photometric, you have to obtain the photometric calibration for the night
      and apply it to the photometric sequences (see the instructions here).
  • Record all the raw and reduced data in a DVD. For more information about burning DVDs click here. Label the DVD with the date, telescope, instrument, and the "RAW+PROCESSED" label. Leave the DVD in the CSP office in La Serena.
  • Once you have saved all the data in the DVD, erase all the *fits files from the subdirectory. Do not erase any of the remaining files.
  • Copy the remaining files (without the fits files) into a subdirectory under /csp2/SWO/ (replace "SWO" by "DUP", "BAA", etc., according to the case). The subdirectory for the night should be named as "yyyymmd1_d2". If you are working in csp1, csp2, or csp3 you just need to type, e.g.: cp -r 20040831_01/ /csp2/TEL/ If you are not in any of the csp computers you will have to ftp the subdirectory to /csp2/TEL/.
  • Print the observing log and the reduction log files, put them in a folder, and leave it in the CSP office in La Serena.
  • Log into csp1 as user "cspuser1", and update reduction logs for RetroCam, WIRC or PANIC.
      Carnegie Supernova Program