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Near-infrared spectroscopy of the very low mass companion to the hot DA white dwarf PG 1234+482

Citation

Steele, PR and Burleigh, MR and Dobbie, PD and Barstow, MA, Near-infrared spectroscopy of the very low mass companion to the hot DA white dwarf PG 1234+482, Monthly Notices of the Royal Astronomical Society, 382, (4) pp. 1804-1808. ISSN 0035-8711 (2007) [Refereed Article]

Copyright Statement

Copyright 2007 The Authors. Journal compilation 2007 RAS

DOI: doi:10.1111/j.1365-2966.2007.12481.x

Abstract

We present a near-infrared spectrum of the hot (Teff ≈ 55 000 K) hydrogen atmosphere (DA) white dwarf PG 1234+482. We confirm that a very low mass companion is responsible for the previously recognized infrared photometric excess. We compare spectra of M and L dwarfs, combined with an appropriate white dwarf model, to the data to constrain the spectral type of the secondary. We find that uncertainties in the Two-Micron All-Sky Survey HK photometry of the white dwarf prevent us from distinguishing whether the secondary is stellar or substellar, and assign a spectral type of L0±1 (M9–L1). Therefore, this is the hottest and youngest (≈ 106 yr) DA white dwarf with a possible brown dwarf companion.

Item Details

Item Type:Refereed Article
Keywords:binaries: spectroscopic; stars: low-mass, brown dwarfs; white dwarfs
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Stellar Astronomy and Planetary Systems
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Dobbie, PD (Dr Paul Dobbie)
ID Code:81045
Year Published:2007
Web of Science® Times Cited:7
Deposited By:Mathematics and Physics
Deposited On:2012-11-21
Last Modified:2013-06-27
Downloads:0

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