Flat Fields for the CCD Spectral Modes

Details Flat Fields for the CCD Spectral Modes Flat Fields for the CCD Spectral Modes

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999stis.rept....6b&link_type=abstract

STIS Instrument Science Report 99-06, 19 pages

Computer Science

Hubble Space Telescope, Hst, Space Telescope Science Institute, Stis, Space Telescope Imaging Spectrograph

Scientific paper

Except for fringing effects at the longer wavelengths, the pixel-to-pixel flat field for the spectral modes is independent of wavelength but does change with time. An average flat with one to four million electrons/px is applicable to all CCD first order modes, except G750M, after the dust mote regions are inserted from separate low or medium dispersion flats. Application of this flat to spectra of standard stars produces a rms residual noise level as good as ~0.3%, which is comparable to the residual noise achievable with no flat. Since the intrinsic rms structure in the CCD flat field is 0.8%, those five current pipeline CCD flats that have less than 0.8% statistical significance produce spectra that are always noisier than with no flat. Since the time constant for changes in the CCD flat is some days, a contemporaneous flat with about a million electrons/px could enable observations with a S/N approaching 1000 for bright sources. For a stellar spectrum with Poisson S/N=1100, an actual S/N of 400 is demonstrated with the new flat.

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