The Deep Coronagraphic STIS Point Spread Function

Details The Deep Coronagraphic STIS Point Spread Function The Deep Coronagraphic STIS Point Spread Function

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9224w&link_type=abstract

HST Proposal ID #9224

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #9224 Star Formation

Scientific paper

The last 5 years have seen the study of young planetary systems move beyond theory and into the realm of fore-front observational astronomy. HST imaging campaigns have been a key component of these multiwavelength studies by capitalizing on the stable point spread function {PSF} of the telescope and the availability of coronagraphs to image circumstellar nebulosity within a few arcseconds of the target stars. In cycle 10, the only coronagraph available onboard HST is STIS. This instrument relies on the use of the unfiltered CCD in tandem with coronagraphic wedges; the resulting images have large PSF color effects, which can compromise the ability to successfully separate the residual PSF from circumstellar nebulosity. While this separation is straightforward for systems with detached nebulosity {e.g. debris disks} where the star can be approximated by a color-matched main sequence star, this process is more complicated for actively accreting systems which are either intrinsically and unpredictably variable in color as well as magnitude, or those systems which turn out to be close binary systems. For such stars, a library of stellar PSFs is needed. We propose a calibration study to assemble such a library, documenting optimal observing and data reduction strategies, and disseminating this information {via the STIS handbook} so that the full astronomical community can take advantage of HST's coronagraphic capability.

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