Observations of G29 - 38 at 10 microns

Details Observations of G29 - 38 at 10 microns Observations of G29 - 38 at 10 microns

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...358l..17t&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 358, July 20, 1990, p. L17-L19.

Astronomy and Astrophysics

Astronomy

12

Brown Dwarf Stars, Infrared Astronomy, Interstellar Matter, White Dwarf Stars, Bolometers, Companion Stars, Spectral Energy Distribution

Scientific paper

The white dwarf G29 - 38 was shown by Zuckerman and Becklin (1987) to have an IR excess at 1-5 microns, possibly due to a spatially unresolved brown dwarf companion. Using the NASA-MSFC 20-pixel bolometer array at the IRTF, a 10.8-micron flux density of 9.5 + or - 3.1 mJy is detected from G29 - 38. This value, combined with more recent 10-micron data obtained by others, implies that 10-micron emission from G29 - 38 is at least twice that expected from a brown dwarf having an effective temperature in the range 1100-1500 K, as previously estimated. The possibility that the IR excess is emitted by dust rather than a brown dwarf is therefore strengthened.

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