First Spitzer Space Telescope Observations of Magnetic Cataclysmic Variables: Evidence of Excess Emission at 3-8 μm

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Published 2006 July 12 • © 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A.
, , Citation Steve B. Howell et al 2006 ApJ 646 L65 DOI 10.1086/506558

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Author affiliations

1 WIYN Observatory and National Optical Astronomy Observatory (NOAO), 950 North Cherry Avenue, Tucson, AZ 85719

2 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125

3 Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003

4 NASA/NOAO Spitzer Space Telescope Observing Program for Students and Teachers

5 Cranston High School East, 899 Park Avenue, Cranston, RI 02910

6 Environmental Education, Great Falls Public Schools, West Elementary, 1205 First Avenue, NW, Great Falls, MT 59404

7 Allentown High School, 27 High Street, Allentown, NJ 08501

8 Michelson Science Center, California Institute of Technology, Pasadena, CA 91125

9 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195

Dates

  1. Received 2006 January 24
  2. Accepted 2006 June 8
  3. Published
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1538-4357/646/1/L65

Abstract

We present the first observations of magnetic cataclysmic variables using the Spitzer Space Telescope. We used the Infrared Array Camera to obtain photometry of the Polars EF Eri, GG Leo, V347 Pav, and RX J0154.0-5947 at 3.6, 4.5, 5.8, and 8.0 μm, respectively. In all of our targets, we detect excess mid-infrared emission over that expected from the component stars alone. We explore the origin of this IR excess by examining bremsstrahlung, cyclotron emission, circumbinary dust, and L/T brown dwarf secondary stars. Bremsstrahlung and cyclotron emission appear unlikely to be significant contributors to the observed fluxes. At present, the most likely candidate for the excess emission is dust that is probably located in a circumbinary disk with an inner temperature near 800 K. However, a simple dust disk plus any reasonable low-mass or brown dwarf-like secondary star is unable to fully explain the observed flux densities in the 3-8 μm region.

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10.1086/506558