Automatic and GO Wavecals, for CCD and MAMA Spectroscopic Observations

Details Automatic and GO Wavecals, for CCD and MAMA Spectroscopic Observations Automatic and GO Wavecals, for CCD and MAMA Spectroscopic Observations

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997stis.rept....1b&link_type=abstract

Instrument Science Report STIS 97-01, 5 pages

Physics

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

Scientific paper

In this report we describe the implementation of automatic and GO wavecals for CCD and MAMA spectroscopic science. Each time the Mode Select Mechanism (grating wheel) is moved to select a new optical element or tilt a grating, the resultant spectrum is projected onto the detector with an error (lack of repeatability) of ~2-6 pixels. In addition, thermal changes in STIS may cause flexure in the optical bench which may cause the projection of the spectrum onto the detector to slowly drift over the course of time. To correct for the spectral zeropoint uncertainty and drift, the ground system will automatically insert short wavecal (line lamp) observations into a series of external observations using a dispersive optical element. The calstis pipeline will process the wavecals along with the science data in order to correct for zeropoint shifts. In addition GOs can insert additional wavecal exposures into their observations if they require particularly high wavelength accuracy.

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