Spectroscopic Data Reductions





The person in charge of the spectroscopic data reductions is Nidia Morrell,
who is backed up by Mark Phillips. Her/His duties are the following: 
  • Make a subdirectory in the /csp1/DUP/ (or /csp1/BAA/ or /csp1/CLA/) directory following the CSP naming convention, i.e., 20020914_15 (e.g.), and FTP all the data to this subdirectory. You can work in your own computer instead of /csp1, but this will require that you copy some files to /csp1 at the end of the data reductions.
  • Get the observing log from here, so you can familiarize yourself with the data taken and the problems reported during the night.
  • Copy "snphot$README_DUP_WF", "snphot$README_DUP_MS", "snphot$README_CLA_LD", "snphot$README_CLA_BC", or "snphot$README_NTT_EM" into current directory. Edit this reduction log file during the data processing.
  • Type one of the following: reset uparm=snphot$uparm_DUP_WF/ reset uparm=snphot$uparm_DUP_MS/ reset uparm=snphot$uparm_CLA_LD_C1_BLUE/ reset uparm=snphot$uparm_CLA_LD_C2_BLUE/ reset uparm=snphot$uparm_CLA_LD_C1_RED/ reset uparm=snphot$uparm_CLA_LD_C2_RED/ reset uparm=snphot$uparm_CLA_LD_ALL/ reset uparm=snphot$uparm_NTT_EM_BLUE/ reset uparm=snphot$uparm_NTT_EM_GREEN/ reset uparm=snphot$uparm_NTT_EM_RED/ reset uparm=snphot$uparm_BAA_IM2_NOR_200_C2/ reset uparm=snphot$uparm_BAA_IM2_NOR_200_C5/
  • Note added on April 25, 2008: Different setups have been used lately both in LDSS3 and in IMCACS. You can find more info in the 'Observing procedures' pages for boths instruments. It will be possible, from now on, to use VPH_ALL in LDSS3, and IMACS/f2/Normal_Orientation for IMACS. To get more precise detalis on data reduction (including parameter settings for the reduction tasks) for each particular setup, you can refer to /csp11/csp1/camp07_08/BAA or /csp11/csp1/camp07_08/CLA and look into the README file for one night where that specific setup was used.
  • Load 'snphot' package by typing 'snphot'.
  • Open DS9 window
  • For EMMI data, run the task "emmi" to convert BLMD*fits and REMD* files into ccd*fits files.
  • For LDDS3 data, run the task "ldss3" to standarize the headers. You also need to separate the data into two subdirectories, one with quadrant 1 and the other with quadrant 2.
  • The task "ldss3" will work also for IMACS data headers.
  • Use the task "bnc" for Boller & Chivens data.
  • Inspect the image headers with the task chkhead.
  • Use the task headers to update the airmass, JD, and UT in the image headers.
  • Make image listing with "hselect ccd*fits $I,exptime,wairmass,aperture,grism,filter,title yes > list"; or "hselect ccd*fits $I,exptime,wairmass,slit,grating,filter,title yes > list" (for EMMI data) or "ccd*1.fits $I,exptime,wairmass,slitmask,dispersr,filter,title yes > list" (for IMACS data, to save space, we only list one of the chips) or "ccd*c1.fits $I,exptime,wairmass,aperture,grism,filter,title yes > list" (for LDSS3 data).
  • Type "ccdlist *fits" to check that imagetyp is properly set in headers.
  • Use the task specred to process the data through [OTZF]. Do not forget to open a DS9 before running this task.
  • Use the task wavecal to derive a general wavelength calibration for the night.
  • Use the task tell to extract and wavelength calibrate the spectrum of the telluric standard. Then do an splot of the resulting 1-D spectrum of the telluric standard and manually remove any non-telluric features present in it.
  • Use the task fluxcal to derive the flux calibration for the night.
  • Use the task getspec to extract, calibrate 1D spectra, and copy the calibrated spectrum to CSP account in csp1.
  • Update the observing logs in the web site.
  • Use the task ccd40 to process direct images through [OTZF].
  • 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.
  • Update the observing logs in the web site
  • 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.
  • All this subdirectory with the remaining files (without the fits files) should be copied into /csp1/DUP/ (or /csp1/BAA/, or /csp1/CLA). If you are working in csp1, csp2, or csp3 you just need to type: cp -r 20040831_01/ /csp1/DUP/ If you are not in any of the csp computers you will have to ftp the subdirectory to /csp1/DUP/.
  • Print the observing log, the reduction log files, and the file "list", and put them in a folder, and leave it in the CSP office in La Serena.
  • If the SN hasn't been typed, provide a spectroscopic classification, age, and expansion velocity from the spectrum, and submit the conclusions to the IAUC. Also, update the web page with the SN list with your classification.
    
    
    
    
    
     
      Carnegie Supernova Program