Reducing a single observation with makee.
Reducing an entire observing run (multiple reductions) using esipipe.
Before running makee you must select your four input images: (1) object , (2) trace star , (3) flat field , and (4) arc lamp . The arclamp is optional (you just won't get a wavelength scale.) You can also use two arclamps for ESI (CuAr and HgNe) although only one is required for wavelength calibration. A short dark (or bias image) may be included using the "bias=", but is not required (a default pattern for ESI will be used).
Select your input files by referring to your logsheets and/or a listing of your ESI Exposures (you can use rhh to get a quick listing of your data). Below is an example listing using rhh :
58 esi0058 23Oct00 15:46 Ec:IntF+qtz1 0.75 1x1 6s IntFlat 65 esi0065 24Oct00 04:26 Ec:Obje 0.75 1x1 100s BD+28 4211 76 esi0076 24Oct00 13:28 Ec:Obje 0.75 1x1 3000s SDSSp0324-0457 77 esi0077 24Oct00 14:30 Ec:Obje 0.75 1x1 3000s HS1818+1037 83 esi0083 24Oct00 15:46 Ec:Line+cu1 0.75 1x1 300s CuAr 84 esi0084 24Oct00 15:56 Ec:Line+ne1 0.75 1x1 4s Hg+Xe
This listing shows the observation number, filename (.fits is assumed), the UT date and time, "Ec:" for echellette., observation type, slit width, binning, exposure time, and object name.
In this example, we want to reduce observation #76, a 3000 second exposure of "SDSSp0324-0457". We will use the UV bright standard star BD+28 4211 to define the echelle trace curve.
The MAKEE command for this would be:
makee esi0076 esi0065 esi0058 esi0083 esi0084 log=esi0076.log
Here we used a single quartz flat, although a sum of flats is usually recommended. We also used two arclamps, although only one was required. We have included the option "log=" to send the output to a log file, alternatively we could have had the output sent to screen (default).
First, look at the log file for this reduction, esi0076.log . Look for error and warning messages or excessive cosmic ray rejections (more than 1000 in the object, or 5000 in the sky background).
Next, look at the trace PostScript file, trace-065.ps . The residuals should be less than about 0.5 pixels with larger residuals of a pixel or more at the edges of some orders.
Then look at the profiles PostScript file, profiles-076.ps . The dotted lines show which regions were extracted as object and background. If the automatically selected regions are inadequate, you can manually select the object and background regions (see Controlling the Object Extraction Boundaries ).
Then we look at the wavelength calibration PostScript file, Arc-083-fr.ps . The top plot shows the first iteration correlation shift which usually has residuals of about 0.2 pixels. The bottom plot shows the fit to arcline centroids which usually has residuals of about 0.2 pixels. For more information on how the ESI wavelength calibrations are done see ESI Wavelength Calibrations .
If those plots look ok, we can view the Flux-076.fits and
The program esipipe can be used to create a script of "makee" commands. The following steps may be used:
rhh esi*.fits > rhh.list
ls esi*.fits > raw.list
esipipe raw.list star.list raw=myrawdata
source makee.script &
egrep -i error *.log egrep -i warning *.log