The Hawaii imaging Fabry-Perot interferometer (HIFI)

Details The Hawaii imaging Fabry-Perot interferometer (HIFI) The Hawaii imaging Fabry-Perot interferometer (HIFI)

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98..723b&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, Aug. 1989, p. 723-735. Research supported by Canada-France-Hawaii Telescope Corp

Astronomy and Astrophysics

Astronomy

65

Astronomical Observatories, Fabry-Perot Interferometers, Astronomical Photometry, Calibrating, Charge Coupled Devices, Etalons, Galaxies, Hawaii, Imaging Spectrometers

Scientific paper

At Mauna Kea Observatory, optical studies of bright, nearby galaxies have been conducted using Fabry-Perot systems on both the University of Hawaii 2.2-m and Canada-France-Hawaii 3.6-m telescopes. These instruments provide high kinematic resolution for a field of view as much as 10 arcmin at subarcsecond increments matched to the seeing disk above the site. The present approach differs from that of the highly successful TAURUS systems (Taylor and Atherton 1980) in the use of a large free-spectral-range etalon with high finesse and CCD at the image plane. CCDs afford certain advantages over photon-counting detectors for two-dimensional, kinematic, and spectrophotometric studies. The geometric integrity of the CCD produces a clean Airy surface and bypasses the optoelectronic distortions of image intensifiers. The high quantum efficiency and linearity over a wide dynamic range in intensity proved to be essential in recent studies of extended narrowline regions, the results of which are summarized. A major advantage afforded by photon-counting systems is the ability to scan rapidly in wavelength, while CCDs are presently limited by detector readout noise. As the readout noise of CCDs approaches a few electrons, the readout time will provide the limitation to rapid scanning.

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