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1995PASP..107..871H - Publ. Astron. Soc. Pac., 107, 871-887 (1995/September-0)
The Goddard High-Resolution Spectrograph : In-orbit performance.
HEAP S.R., BRANDT J.C., RANDALL C.E., CARPENTER K.G., LECKRONE D.S., MARAN S.P., SMITH A.M., BEAVER E.A., BOGGESS A., EBBETS D.C., GARNER H.W., HUTCHINGS J.B., JURA M., LINSKY J.L., SAVAGE B.D., CARDELLI J.A., TRAFTON L.M., WALTER F.M., WEYMANN R.J., AKE T.B., CRENSHAW D.M., MALUMUTH E.M., ROBINSON R.D., SANDOVAL J.L., SHORE S.N., WAHLGREN G.M., BRUHWEILER F., LINDLER D.J., GILLILAND R.L., HULBERT S.J. and SODERBLOM D.R.
Abstract (from CDS):
Data have been obtained over a wavelength range from below 1100 A to 3300 A, at spectral resolutions as high as R = lambda/delta-lambda = 90,000. The wavelength scale is influenced by spectrograph temperature, outgassing of the optical bench, and interaction of the magnetic field within the detector with the earth's magnetic field. Models of these effects lead to a default wavelength scale with an accuracy better than 1 diode, corresponding to 3 km s^-1 in the echelle mode. With care, the wavelength scale can be determined to an accuracy of 0.2 diodes.
Calibration of the instrument sensitivity functions is tied into the HST flux calibration through observations of spectrophotometric standard stars. The measurements of vignetting and the echelle blaze function provide relative photometric precision to about 5% or better. The effects of fixed-pattern noise have been investigated, and techniques have been devised for recognizing and removing it from the data. The ultimate signal-to-noise ratio achievable with the spectrograph is essentially limited only by counting statistics, and values approaching 1000:1 have been obtained.
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