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The Classification of T Dwarfs

Published online by Cambridge University Press:  26 May 2016

Adam J. Burgasser ,
Thomas R. Geballe ,
David A. Golimowski ,
Sandy K. Leggett ,
J. Davy Kirkpatrick ,
Gillian R. Knapp  and
Xiaohui Fan
Adam J. Burgasser
Affiliation:
Hubble Fellow; UCLA Dept. Physics & Astronomy, 8965 Math Sciences Bldg., Los Angeles, CA 90095–1562; [email protected]
Thomas R. Geballe
Affiliation:
Gemini Observatory, 670 North A'ohoku Place, Hilo, HI 96720
David A. Golimowski
Affiliation:
Dept. Physics & Astronomy, Johns Hopkins University, 3701 San Martin Drive, Baltimore, MD 21218
Sandy K. Leggett
Affiliation:
Joint Astronomy Centre, 660 North A'ohoku Place, Hilo, HI 96720
J. Davy Kirkpatrick
Affiliation:
Infrared Processing and Analysis Center, M/S 100–22, California Institute of Technology, Pasadena, CA 91125
Gillian R. Knapp
Affiliation:
Princeton University Observatory, Peyton Hall, Princeton, NJ 08544–1001
Xiaohui Fan
Affiliation:
Institute for Advanced Study, Olden Lane, Princeton, NJ 08540–0631

Abstract

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The discovery of many cool brown dwarfs similar to Gliese 229B has led to the definition of a new spectral class, the T dwarfs, whose 1–2.5 μm spectra exhibit signatures of CH4 absorption. Two classification schemes have been proposed for these objects by Burgasser et al. and Geballe et al. We discuss and compare these schemes, and describe a joint classification scheme currently in development that closely follows the guidelines of the MK process. We also address future work toward establishing gravity classes, classifying at other wavelengths, and identifying those features that may signify the end of the T spectral class.

Type
Part 7. Atmospheres and Internal Structure
Information
Symposium - International Astronomical Union , Volume 211: Brown Dwarfs , 2003 , pp. 377 - 384
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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