STIS Near-IR Fringing. II. Basics and Use of Contemporaneous Flats for Spectroscopy of Point Sources (Rev. A)

Details STIS Near-IR Fringing. II. Basics and Use of Contemporaneous Flats for Spectroscopy of Point Sources (Rev. A) STIS Near-IR Fringing. II. Basics and Use of Contemporaneous Flats for Spectroscopy of Point Sources (Rev. A)

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998stis.rept...19g&link_type=abstract

STIS Instrument Science Report 98-19, 18 pages

Computer Science

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

Scientific paper

G750L and G750M spectra of white dwarfs have been analyzed to study the accuracy with which one can correct for long-wavelength fringing on the STIS CCD. Flat-fielding results using pre-flight and in-flight long-slit lamp flats are compared with those using contemporaneous lamp flats (taken during the course of science data collection, in order to keep the same Mode Select Mechanism position as the science spectra). The contemporaneous lamp flats are taken through a short slit to mimic a point source. In the case of G750L spectra, contemporaneous flats are essential if a signal-to-noise above ~30 is required in wavelength regions where the fringing is significant (~700 - 1000 nm). The residuals of the fringes in G750L spectra can be reduced to below the 1% level by division by a wellexposed contemporaneous fringe flat taken through a short slit. The superiority of contemporaneous short-slit flats over long-slit flats is somewhat less critical for G750M spectra, but still quite significant. For the G750M case, contemporaneous fringe flats are essential to reach signal-to-noise ratios above ~50. The effects of on-orbit thermal drifts are evaluated and corrected for by matching the fringe pattern of star and flat along the dispersion direction. The influence of the red "halo" (scattered light) to the tungsten fringe flats is corrected for by scaling the amplitude of the fringes. In this revision we provide an updated recommendation for obtaining fringe flats along with 52x0.2F1 slit spectra (see Table 2).

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