Deep Fabry-Perot Observations of High Velocity Clouds

Details Deep Fabry-Perot Observations of High Velocity Clouds Deep Fabry-Perot Observations of High Velocity Clouds

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.1209b&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #12.09; Bulletin of the American Astronomical Society, Vol. 26, p.1327

Astronomy and Astrophysics

Astronomy

1

Scientific paper

In recent months, we have demonstrated that it is possible to reach Hα emission measures as low as 0.02 cm(-6) pc (4times 10(-20) erg cm(-2) s(-1) arcsec(-2) ) in six hours of dark time observation (3sigma limit) with the TAURUS-2 imaging Fabry-Perot interferometer at the f/8 Cassegrain focus of the AAT 3.9m. This deep limit assumes that the emission-line source is spectrally unresolved and completely fills the field of view (9(') ). The etalon is kept at a fixed spacing in which case the spectrum is dispersed as a series of annular rings over the field. For our preferred choice of etalon and filters, TAURUS-2 provides ~ 50 Angstroms of spectral coverage in a single exposure at a spectral resolution close to 1 Angstroms FWHM. Below emission measures (T_e = 10(4) K) of roughly 0.1 cm(-6) pc, there are systematic effects which can only be removed with extensive calibrations. Our new deep limit brings a number of important experiments into the realm of possibility for the first time. It has long been realized that an emission-line detection (at optical wavelengths) of a high velocity cloud would provide an important constraint on the galactic and/or metagalactic radiation fields. To date, there exists only one high velocity cloud with a possible Hα detection (Kutryev & Reynolds 1989). We shall present early results from a new survey which aims to detect a statistically useful number of clouds in more than one emission line.

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