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Working with OmegaCam flat files from the CASU pipeline

The OSA archives the FITS images and catalogues produced by the CASU pipeline. Metadata from the images and objects from the catalogues are processed and ingested into database tables (also see data overview)

Typically the FITS images have a .fit file extension while the catalogues end _cat.fits. The database entity MULTIFRAME references a FITS image and if applicable a corresponding FITS catlogue. Note only stacked images have catalogues (eg calibration frames and intermediate science frames do not have catalogues.)

Apart from secondary data products (e.g. mosaic images) CASU FITS files have a primary header and FITS extensions with each extension representing one of the detectors. The FITS image files are RICE compressed and some applications will require the file to be uncompressed before use, see notes on compression.

Starlinks's GAIA is able to open the FITS images directly for display.

Converting catalogue fluxes to magnitudes

The FITS catalogues contain un-calibrated fluxes. When ingested in to the database tables (DETECTION and SOURCE tables) objects will have their fluxes converted to calibrated magnitudes. The fluxes contained in the FITS catalogues can be converted to calibrated magnitudes using attributes in the FITS header of the relevant extension. Whereby, the instrumental magnitude, instMag, is

instMag = -2.5 * log10(flux) and

the extinction correction, extCorr, is

extCorr = -extinct * (airmassStart + airmassEnd)/2) -1) and

the exposure correction, texpCorr, is

texpCorr = 2.5 * log10(exptime)

then the calibrated magnitude, calMag, is

calMag = instMag + magZpt + extCorr + texpCorr - aperCor

The values for extinct, airmassStart, airmassEnd, exptime and magZpt can be found in the FITS header of the relevant extension under keywords: EXTINCT, AMSTART, AMEND, EXP_TIME and MAGZPT. The values for flux are read for each object (row) in the catalogue from the required flux attribute eg Aper_flux_3 or Kron_flux. For aperture corrected magnitudes use the corresponding APERCOR value in the FITS extension header eg APCOR3.

By way of an example, the 1st extension of a FITS catlogues has the following header information

AMSTART =                1.083 / Airmass at start of observation                
AMEND   =                1.084 / Airmass at end of observation                  
EXP_TIME=            20.000000 / [s] Integration time per exposure              
APCOR1  =             1.242335 / Stellar aperture correction - 1/2x core flux   
APCOR2  =            0.8231881 / Stellar aperture correction - core/sqrt(2) flux
APCOR3  =            0.4040413 / Stellar aperture correction - core flux        
APCOR4  =            0.1864481 / Stellar aperture correction - sqrt(2)x core flu
APCOR5  =           0.07809448 / Stellar aperture correction - 2x core flux     
APCOR6  =           0.02818298 / Stellar aperture correction - 2sqrt(2)x core fl
APCOR7  =                   0. / Stellar aperture correction - 4x core flux     
MAGZPT  =               22.771 / Photometric ZP (mags) for default extinction   
EXTINCT =                0.05  / Extinction coefficient (mags)                  

So say for a given object the aper_flux_3 is 0.60321E+03 and the kron_flux is 0.10143E+04. Then

extCorr = -0.00418, texpCorr=3.25257 and

aperMag3 =-2.5*log10(0.60321E+03)+22.771-0.00418+3.25257-APERCOR3 = 18.664 and

kronMag =-2.5*log10(0.10143+04)+22.771-0.00418+3.25257 = 18.504