Hawaii Quasar and T Dwarf Survey. I. Method and Discovery of Faint Field Ultracool Dwarfs

Details Hawaii Quasar and T Dwarf Survey. I. Method and Discovery of Faint Field Ultracool Dwarfs Hawaii Quasar and T Dwarf Survey. I. Method and Discovery of Faint Field Ultracool Dwarfs

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...723..184k&link_type=abstract

The Astrophysical Journal, Volume 723, Issue 1, pp. 184-196 (2010).

Astronomy and Astrophysics

Astronomy

2

Brown Dwarfs, Early Universe, Quasars: General, Stars: Low-Mass, Techniques: Photometric

Scientific paper

The Hawaii Quasar and T dwarf survey (HQT Survey) is a wide-field, red optical survey carried out with the Suprime-Cam mosaic CCD camera on the 8.2 m Subaru telescope. The HQT survey is designed to search for low-luminosity (M AB1450 < -23) quasars at high redshift (z>5.7) as well as T dwarfs, both of which are selected by their very red I - z' colors. We use an optical narrowband filter NB816 to break a well-known I - z' color degeneracy between high-z quasars and foreground M and L dwarfs, which are more numerous than quasars. This paper is the first in a series of papers from the HQT survey and we report on the discovery of six faint (19 <= J <= 20) ultracool dwarfs found over a ~9.3 deg2 area with a limiting magnitude of z'AB <= 23.3. These dwarfs were confirmed by near-IR imaging and/or spectroscopy conducted at various facilities on Mauna Kea. With estimated distances of 60-170 pc, these are among the most distant spectroscopically confirmed field brown dwarfs to date. Limits on the proper motions of these ultracool dwarfs suggest that they are old members of the Galactic disk, though future follow-up observations are necessary to minimize errors. Our finding rate of ultracool dwarfs is within model predictions of Liu et al. However, the large brightening amplitude (~1 mag) previously reported for the L/T transition objects appears to overpredict the numbers. We also examine how the survey field latitude affects the survey sensitivity to the vertical scale height of ultracool dwarfs.
Based in part on data obtained at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.
Based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA and was made possible by the generous financial support of the W. M. Keck Foundation.

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