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Removing the Fringes from Space Telescope Imaging Spectrograph Slitless Spectra

Eliot M. Malumuth, Robert S. Hill, Ted Gull, Bruce E. Woodgate, Charles W. Bowers, Randy A. Kimble, Don Lindler, Phil Plait and Morley Blouke
Publications of the Astronomical Society of the Pacific
Vol. 115, No. 804 (February 2003), pp. 218-234
DOI: 10.1086/345913
Stable URL: http://www.jstor.org/stable/10.1086/345913
Page Count: 17
Subjects: Astronomy
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Removing the Fringes from Space Telescope Imaging Spectrograph Slitless Spectra
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Abstract

ABSTRACT Using what is known about the physical and chemical structure of the CCD detector on the Space Telescope Imaging Spectrograph (STIS) and over 50 calibration images taken with different wavelength mappings onto the detector, we have devised a model function that allows us to predict the fringing of any spectral image taken with the STIS CCD. This function is especially useful for spectra taken without a slit with the G750L grating. The STIS parallel observing program uses this “slitless spectroscopy” mode extensively. The arbitrary mapping of wavelength versus position that results from each source's chance position in the field renders direct calibration of the fringe amplitudes in this mode impossible. However, we find that correcting observed data using our semiempirical fringing model produces a substantial reduction in the fringe amplitudes. Tests using the flux calibration white dwarf standard G191‐B2B show that we can reduce the fringe amplitude in the 9000–10000 Å region from about 20% peak to peak (10% rms) to about 4% peak to peak (2% rms) using the model, while a standard calibration using a “fringe flat” reduces the fringe amplitudes to 3.3% peak to peak (1.7% rms). The same technique is applicable to other astronomical CCDs.

Notes and References

This item contains 9 references.

REFERENCES
  • ['Born, M., & Wolf, E. 1999, Principles of Optics (7th ed.; Cambridge: Cambridge Univ. Press)']
  • ['Gardner, J. P., et al. 1998, ApJ, 492, L99']
  • ['Janesick, J. R. 2001, Scientific Charge‐Coupled Devices (Bellingham: SPIE Press)']
  • ['Kimble, R. A., et al. 1994, Proc. SPIE, 2282, 169']
  • ['———. 1998, ApJ, 492, L83']
  • ['Palik, E. D. 1998, Handbook of Optical Constants of Solids III (Sydney: Academic Press)']
  • ['Pickles, A. J. 1998, PASP, 110, 863']
  • ['Silva, D. R., & Cornell, M. E. 1992, ApJS, 81, 865']
  • ['Windt, D. L. 1998, Comput. Phys., 12, 360']