The Awe photometric pipeline Software implementation

Photometric pipeline : class model Cal563/Cal564 Cal569 Cal565 Cal562

Photometric pipeline : equation to solve

Photometric pipeline : source catalogs PhotSrcCatalog : association between standard star catalog and Sextractor catalog photsrccat.refcat = PhotRefCatalog() photsrccat.frame = ScienceFrame() photsrccat.transform = PhotTransformation() photsrccat.make() rawzero = photsrccat.photsourcelist[3].get_raw_zeropoint() rawzero_list = photsrccat.get_list_of_raw_zeropoints()

Photometric pipeline : color terms Color terms are dealt with in photsrccatalog.make() photsrccatalog.transform = PhotTransformation() transf.get_dict_of_transformed_magnitudes(mag_id, refcat)  the mag_id is the primary key through which the system identifies the photometric band Examples : JohnsonV, CousinsR, SloanU, SloanG

Photometric pipeline : extinction Atmospheric extinction is treated as a pluggable algorithm  three different algorithms implemented at present atmospheric_extinction = AtmosphericExtinctionFrames() atmospheric_extinction.polar = photsrccat_list_1 atmospheric_extinction.equat = photsrccat_list_2 atmospheric_extinction.extcurve = PhotExtinctionCurve() atmospheric_extinction.make()  system easily extended with new ways to derive the atmospheric extinction

Photometric pipeline : zeropoints photometricparameters.photcat = photsrccatalog photometricparameters.extinct = atmospheric_extinction photometricparameters.make() The zeropoints are derived by and contained within a PhotometricParameters object.  a PhotometricParameters object represents the Calfile that is used in the image pipeline

Photometric pipeline : illumination correction software has to be implemented current scheme is to apply the correction on frame level in the image pipeline the input frames for the photometric pipeline are, therefore, already corrected for this effect

Photometric pipeline : a general recipe photsrccatalog.refcat = PhotRefCatalog() photsrccatalog.frame = ScienceFrame() photsrccatalog.transform = PhotTransformation() photsrccatalog.make() atmospheric_extinction = BaseAtmosphericExtinction() atmospheric_extinction.make() photometricparameters.extinct = atmospheric_extinction photometricparameters.photcat = photsrccatalog photometricparameters.make()

Photometric pipeline : a use case (1) Available resources for (rough) photometric calibration : during the night, for every filter only ONE observation was made of a standard field standard stars are present on only ONE of the chips of the N-chip camera a standard extinction curve has to be used no illumination correction is known, nor can it be derived Conclusion : the prospects are bleak

Photometric pipeline : a use case (2) the_photsrccatalog.refcat = PhotRefCatalog() the_photsrccatalog.frame = ScienceFrame() the_photsrccatalog.transform = PhotTransformation() the_photsrccatalog.make() photsrccatalog.frame = ScienceFrame() photsrccatalog.set_sky_background() 

Photometric pipeline : a use case (3) atmos_extinction = AtmosphericExtinctionCurve() atmos_extinction.filter = scienceframe.filter atmos_extinction.extcurve = PhotExtinctionCurve() atmos_extinction.report = PhotometricExtinctionReport() atmos_extinction.make()  Note the dependency on a Filter object  Note the dependency on a PhotometricExtinctionReport object

Photometric pipeline : a use case (4) the_photometricparameters = PhotometricParameters() the_photometricparameters.photcat = the_photsrccatalog the_photometricparameters.extinct = atmos_extinction the_photometricparameters.make() photometricparameters.photcat = photsrccatalog photometricparameters.extinct = atmos_extinction photometricparameters.set_zeropoint(zp, zp_err) 

Photometric pipeline : resources /cvsroot/catalog/ /cvsroot/opipe/Toolbox/photometry /cvsroot/opipe/docs /cvsroot/opipe/astro/main Yours truly