Computer Science
Scientific paper
Jul 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8844p&link_type=abstract
HST Proposal ID #8844
Computer Science
Hst Proposal Id #8844
Scientific paper
The primary advantage of STIS with HST in the visible portion of the spectrum is high angular resolution with excellent rejection along the slit. However no data is available that measures the spatial/spectral PSF to the limit of the CCD chip dimensions. We plan to acquire a set of deep spectroscopic images of isolated, point source stars with STIS for the purpose of correcting spectroscopic science observations for dispersed residual scattered light along the slit from the point-like central object. Using limited observations from the archive, we suspect that a dynamic range approaching 10exp7 can be measured from the stellar core to 26" away at the limit of the CCD and aperture edge. This can be measured using first the normal slit on axis, then rotating the two fiducials, F1 and F2 into the chip center. F1 with GXXXM is found to knock the stellar core down by 200x. We wish to measure the rejection of F2, which should be approaching 1000x. Moreover, only 52x0.2F1 is currently supported. Data from this study will provide information on implementing more fiducial settings for GO programs. Measurements of standard stars demonstrate that the Airy rings and scattered light are indeed knocked down by 10x the 52x0.2 aperture when compared to the 52x2 aperture. A sample of the rejection of the 52x0.1, 52x0.1F1 and 52x0.1F2 will also be recorded. Four stars with spectral type ranging across the HR diagram will be observed. We have selected these stars with bias toward previous use as standard stars, being bright enough that 10, 000 electrons would be recorded in the peak pixels for normal 52x0.2 aperture in less than ten seconds, being near CVZ, and being in sparse fields. Two werealready selected for measurement of the rejection of the coronagraphic slots {proposal 8419, Charles Proffitt, PI} for consistency and extension of data applicability. HD141653 is an A2 IV star and HD115617 is a G5 V star. We select an M-star, HD181204 as it has been used for a WFPC2 coronagraphic standard and has low proper motion. Finally BD+75D325 is included as a hot star for PSF measures with G230 and G430 gratings. Some 52x0.2F2 settings are eliminated to fit the program into ten orbits made available. One orbit of coronagraphic observations have been added to the HD18204 visit {see program 8842 visit 03 and program 8419} to improve observational efficiency at the request of Charles Proffitt {05122000}.
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