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Multiplicity and Optical Excess across the Substellar Boundary in Taurus

Kraus, Adam L. and White, Russel J. and Hillenbrand, Lynne A. (2006) Multiplicity and Optical Excess across the Substellar Boundary in Taurus. Astrophysical Journal, 649 (1). pp. 306-318. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20110602-105415354

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Abstract

We present the results of a high-resolution imaging survey of 22 brown dwarfs and very low mass stars in the nearby (~145 pc) young (~1-2 Myr) low-density star-forming region Taurus-Auriga. We obtained images with the Advanced Camera for Surveys High Resolution Channel on HST through the F555W (V), F775W (i'), and F850LP (z') filters. This survey confirmed the binarity of [BHS98] MHO 8 (hereafter MHO-Tau-8) and discovered a new candidate binary system, [SS94] V410 X-ray 3 (hereafter V410-Xray3), resulting in a binary fraction of 9^(+10)_(-3)% at separations >4 AU. Both binary systems are tight (<10 AU), and they possess mass ratios of 0.75 and 0.46, respectively. The binary frequency and separations are consistent with low-mass binary properties in the field, but the mass ratio of V410-Xray3 is among the lowest known. We find that the binary frequency is higher for very low mass stars and high-mass brown dwarfs than for lower mass brown dwarfs, implying either a decline in frequency or a shift to smaller separations for the lowest mass binaries. Combining these results with multiplicity statistics for higher mass Taurus members suggests a gradual decline in binary frequency and separation toward low masses. The implication is that the distinct binary properties of very low-mass systems are set during formation and that the formation process is similar to the process that creates higher mass stellar binaries, but occurs on a smaller scale. We combine the survey detection limits with models for planetary-mass objects to show that there are no planets or very low-mass brown dwarfs with mass >3M_J at projected separation >40 AU orbiting any of the Taurus members in our sample, implying that planetary-mass companions at wide separations are rare. Finally, based on fits to the optical and near-infrared spectral energy distributions, we identify several BDs with significant (≳1 mag) V-band excesses. The excesses appear to be correlated with signatures of accretion and if attributed to accretion luminosity may imply mass accretion rates several orders of magnitude above those inferred from line profile analyses.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/503665DOIArticle
http://iopscience.iop.org/0004-637X/649/1/306PublisherArticle
ORCID:
AuthorORCID
Kraus, Adam L.0000-0001-9811-568X
White, Russel J.0000-0001-5313-7498
Additional Information:© 2006 American Astronomical Society. Received 2005 November 18; accepted 2006 February 18. We thank the referee for a prompt, thorough, and helpful critique of this paper. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 9853. This work also makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Subject Keywords:binaries: visual; stars: low-mass, brown dwarfs; stars: pre–main-sequence
Issue or Number:1
Record Number:CaltechAUTHORS:20110602-105415354
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110602-105415354
Official Citation:Multiplicity and Optical Excess across the Substellar Boundary in Taurus Adam L. Kraus et al. 2006 ApJ 649 306
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23873
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:03 Jun 2011 20:30
Last Modified:09 Mar 2020 13:19

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