The Distances to Dwarf Novae and the Calibration of the Technique of Infrared Spectroscopic Parallax

Details The Distances to Dwarf Novae and the Calibration of the Technique of Infrared Spectroscopic Parallax The Distances to Dwarf Novae and the Calibration of the Technique of Infrared Spectroscopic Parallax

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop...16h&link_type=abstract

NOAO Proposal ID #1999A-0016

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Scientific paper

The distances to dwarf novae are poorly known. This deficiency severely impacts our ability to quantify the energetics of the various processes taking place in dwarf novae systems. We have a program nearing completion that uses the Fine Guidance Sensors (FGS) on the HST to measure the parallaxes of three of the best known dwarf novae (DN): SS Cyg, U Gem, and SS Aur. Currently, the distances to these DN are only known to within a factor of ~ 2. The precision achievable by the FGS will result in distances good to ~ +/-10%. Such precision will allow us to calibrate the technique of infrared spectroscopic parallax. We request two nights on the 2.1 m with CRSP to obtain medium resolution K-band spectroscopy of SS Cyg as well as several late-type dwarfs for use as spectral templates. Our medium resolution K-band spectra obtained last winter revealed that the spectral types of SS Aur and U Gem are slightly earlier than previously classified. Strangely, the spectrum for U Gem did not show the CO absorption features expected for an M4V. To examine if this occurs in other DN with very late secondaries, we will observe YY Dra and IP Peg.

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