Imaging With STIS on the Hubble Space Telescope: Astronomy at V=30

Details Imaging With STIS on the Hubble Space Telescope: Astronomy at V=30 Imaging With STIS on the Hubble Space Telescope: Astronomy at V=30

Publishing date

Sep 1997

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasp..109.1062g&link_type=abstract

Journals

Publications of the Astronomical Society of the Pacific, v.109, p.1062-1067

Science

Astronomy and Astrophysics

Field

Astronomy

Additional info 2

12

Additional info 3

Instrumentation: Spectrographs, Telescopes

Type

Scientific paper

Abstract

In February, 1997, the second Space Shuttle servicing mission to the Hubble Observatory installed the Space Telescope Imaging Spectrograph (STIS). This new instrument will greatly enhance the spectroscopic capabilities of the Hubble Space Telescope by providing a longslit format and CCD detector technology. STIS can also be used as an imager, providing an alternative to the Wide Field Planetary Camera 2. The optical filter set of STIS is limited and does not contain standard bandpasses, but we show here that this does not preclude useful two-color broad band photometry. Because the STIS bandpasses reach $\sim 1.5$ magnitudes deeper than WFPC2, the STIS photometric system may be preferable for many applications where a faint limiting magnitude and fine spatial resolution are overriding considerations. The two optical wide-band choices on STIS are a clear aperture and a longpass ($\lambda > 5500$\AA) filter. We define an effective short-pass filter from the difference of these, making two-color photometry possible with STIS. We present preliminary transformations between the STIS system and Cousins BVRI bandpasses, showing that these transformations are very well-behaved over almost all temperatures, luminosities, and abundances for normal stars. In an 8-orbit cycle, STIS will be able to reach signal-to-noise of $\sim 5-10$ at V = 30.0 in its clear and longpass imaging modes, a significant increase in the power of HST to address a number of fundamental issues out of reach of current instrumentation capabilities on the ground or in spac. (SECTION: Astronomical Instrumentation)

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