PDS_VERSION_ID = PDS3 LABEL_REVISION_NOTE = "2003-09-30 Cornell:carcich" RECORD_TYPE = STREAM OBJECT = TEXT PUBLICATION_DATE = 2003-09-30 NOTE = " CSCALFIL_README.TXT file for CONTOUR Archive Volume " END_OBJECT END ####### File _CSCALFIL_README.TXT_ CONTOUR CRISP IR SPECTROMETER CALIBRATION PIPELINE Joseph Harrington and James F. Bell III, Cornell University 9 December 2002 This is the skeleton calibration pipeline for COmet Nucleus TOUR (CONTOUR) Remote Imager Spectrometer InfraRed (CRISP-IR) spectrometer data. The job of the pipeline is to apply the best known calibration to the raw data, correcting instrument effects and converting to physical units. It also decodes some of the encoded raw header keywords, such as array temperature, into SI units. Most of the calibration data were to have come from an in-space calibration routine that would have run for the first time shortly after transfer-orbit injection. Unfortunately, the spacecraft was lost during the transfer-orbit injection burn. The pipeline is thus a skeleton with hooks for routines to apply, e.g., dark signal and flat field corrections. The pipeline takes input two ways: it either reads a named FITS file from the CONTOUR Science Data Center (SDC) or it accepts a FITS data structure. The FITS data structure option allows the SDC to calibrate data as it arrives, immediately following conversion to FITS format, without rereading the file. For more information on FITS format, see http://fits.gsfc.nasa.gov/ or the FITS Standard - NOST 100-2.0 All calibration parameters are recorded in the header by the pipeline and these values can override the default values on subsequent runs. The user may also set variables when calling the pipeline, and these will override those set in the header. The same image may thus be calibrated different ways on successive runs, if the user desires. We do not anticipate that science users will need to use this capability; it is there for the convenience of those implementing the calibration. The pipeline is written in the Interactive Data Language (IDL), from Research Systems, Inc., a Kodak company. Pipeline routines (in idl directory): CSCAL base routine, called by user CSKEYS standardizes header keywords CSREADFITS applies FITS scaling FITSKEYUPD updates/defaults FITS header keywords GENREADIMAGE reads FITS file INT truncates a floating-point value KEYWORD_DEFINED tests whether a variable is defined MASKMEDFILTLEV generates bad pixel mask with median filter N_AXIS determines the number of elementss on a given array axis In addition, the following external routines are used: IDL Astronomy Library (in idl/astron directory): DIST_CIRCLE FXPAR FXPOSIT GETTOK IEEE_TO_HOST IS_IEEE_BIG ISARRAY MRD_HREAD MRD_SKIP MRDFITS SXADDHIST SXADDPAR SXPAR VALID_NUM Maskinterp bad pixel interpolation package (in idl/maskinterp-1.2 directory): COORD DISC MASKINTERP TWOORDFIT The distribution files for these two external packages are in the externdist directory. They are in gzip-compressed tar format. Their internet origins are: ftp://oobleck.astro.cornell.edu/maskinterp-1.2.tar.gz http://idlastro.gsfc.nasa.gov/astron.dir.tar.gz Example: cd cscalpipe idl @init.idl filename = projtop+'/data/355_CSBML_WSM_02_0001.fit' im = cscal(filename) header = im.header data = im.data print, header print, sxpar(header, 'CSF1TEMP') tvscl, data Documentation for the parameters in the pipeline is in the individual routines, as is documentation for the minimal processing applied to the data.