SETI public: First Brown Dwarf Science from Laser Guide Star Adaptive Optics

From: LARRY KLAES (ljk4_at_msn.com)
Date: Mon Aug 08 2005 - 19:39:59 UTC

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    Paper: astro-ph/0508082
    Date: Tue, 2 Aug 2005 22:52:23 GMT (128kb)

    Title: Kelu-1 is a Binary L Dwarf: First Brown Dwarf Science from Laser
    Guide
    Star Adaptive Optics

    Authors: Michael C. Liu (IfA/Hawaii), Sandy K. Leggett (UKIRT/JAC)

    Comments: Astrophysical Journal, in press. 24 pages. (Note that Figure 1 of
    the
    PDF version is degraded by arxiv.org. The Postscript version is fine.)
    \\
    (Abridged) We present near-IR imaging of the nearby L dwarf Kelu-1 obtained
    with the Keck sodium laser guide star adaptive optics (LGS AO) system as
    part
    of a high angular resolution survey for substellar binaries. Kelu-1 was one
    of
    the first free-floating L dwarfs identified, and the origin of its
    overluminosity compared to other similar objects has been a long-standing
    question. Our images clearly resolve Kelu-1 into a 0.29'' (5.4 AU) binary,
    and
    a previous non-detection by HST demonstrates that the system is a true
    physical
    pair. Binarity explains the properties of Kelu-1 that were previously noted
    to
    be anomalous compared to other early-L dwarfs. We estimate spectral types of
    L1.5-L3 and L3-L4.5 for the two components, giving model-derived masses of
    0.05-0.07 Msun and 0.045-0.065 Msun for an estimated age of 0.3-0.8 Gyr.
    More
    distant companions are not detected to a limit of 5-9 Mjup. The presence of
    lithium absorption indicates that both components are substellar, but the
    weakness of this feature relative to other L dwarfs may arise from the fact
    that only Kelu-1B is Li-bearing. Determining if both or if only one of the
    components possesses lithium could constrain the age of Kelu-1 (and other
    Li-bearing L binaries) with higher precision than is possible for most
    ultracool field objects. These results are the first LGS AO observations of
    brown dwarfs and demonstrate the potential of this new instrumental
    capability
    for substellar astronomy.

    \\ ( http://arXiv.org/abs/astro-ph/0508082 , 128kb)


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