FOS Cycle 6: Location of Spectra and Wavelength Calibration - Blue Detector

Details FOS Cycle 6: Location of Spectra and Wavelength Calibration - Blue Detector FOS Cycle 6: Location of Spectra and Wavelength Calibration - Blue Detector

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6913d&link_type=abstract

HST Proposal ID #6913

Physics

Hst Proposal Id #6913

Scientific paper

This proposal monitors the stability of the FOS wavelength scale andlocation of spectra. For the wavelength calibration, all standardgratings are used with the 0.3"circle and either the 0.1" or 0.25"paired apertures. The WAVECAL lamp has a fairly constant output, sothat these data are a secondary monitor of any changes in the FOSinternal sensitivity. For the y-base calibration we will obtainaperture maps to determine the location of spectra and the coarseaperture location for the 0.3" aperture for all grating settings. Wewill then measure the location of spectra for all the remainingscience apertures using only the G190H or G400H gratings. Since weknow that the FOS mechanisms are reasonably well aligned, the smallnumber of observations should suffice and the difference in thelocation of the spectra should be solely due to the single versusthe paired apertures. The program can be scheduled as an interleaverobservation and should be repeated every month for a total of 12 times.It is necessary to conduct this test many times during the cycle sincewe know from previous cycles that the location of the spectra haschanged with time. Total spacecraft time is 1 orbit of prime time and96 orbits of NON-PRIME time.VISIT REQUIREMENT DISCUSSED WITH PC WHO WILL VERIFY TIMING LINKS.

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