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Title:
Infrared spectroscopy, imaging, and 10 micron photometry of Giclas 29-38
Authors:
Tokunaga, A. T.; Hodapp, K.-W.; Becklin, E. E.; Cruikshank, D. P.; Rigler, M.; Toomey, D.; Brown, R. H.; Zuckerman, B.
Affiliation:
AA(Hawaii, University, Honolulu), AB(Hawaii, University, Honolulu), AC(Hawaii, University, Honolulu), AD(Hawaii, University, Honolulu), AE(Hawaii, University, Honolulu), AF(Hawaii, University, Honolulu), AG(California Institute of Technology, Jet Propulsion Laboratory, Pasadena)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 332, Sept. 15, 1988, p. L71-L74. (ApJL Homepage)
Publication Date:
09/1988
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Binary Stars, Infrared Imagery, Infrared Spectroscopy, Stellar Spectrophotometry, White Dwarf Stars, Absorption Spectra, Brown Dwarf Stars, M Stars, Signal To Noise Ratios
DOI:
10.1086/185269
Bibliographic Code:
1988ApJ...332L..71T

Abstract

An NIR spectrum and several images of Giclas 29-38, a white dwarf suspected to have a brown dwarf in orbit around it, are presented. There is no absorption feature in the spectrum that is deeper than 5 percent in the wavelength range 1.95-2.45 microns, from which it is inferred that there is no feature deeper than 10 percent at 2.4 microns from any brown dwarf companion. The IR spectrum does not yield any strong constraint on whether or not the thermal emission observed from G29-38 comes from a brown dwarf or dust. The 1.6- and 2.2-micron images of G29-38 appear indistinguishable from a point source with an upper limit of 0.4 arcsec for the separation of the white dwarf and the source of the excess IR emission. This corresponds to a projected linear separation of 5.6 AU. A 2sigma limit at 10 microns of 10 mJy constrains possible alternative models for the IR excess by emission from dust grains. While the present results do not show evidence for the suspected brown dwarf companion around G29-38, the presence of such an object cannot be ruled out.

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