Hogerheijde, Michiel R. and van Langevelde, Huib Jan and Mundy, Lee G. and Blake, Geoffrey A. and van Dishoeck, Ewine F. (1997) Subarcsecond Imaging at 267 GHz of a Young Binary System: Detection of a Dust Disk of Radius Less than 70 AU around T Tauri N. Astrophysical Journal Letters, 490 (1). L99-L102. ISSN 2041-8205. http://resolver.caltech.edu/CaltechAUTHORS:20120913-105202243
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The young binary system T Tauri was observed with the Owens Valley Millimeter Array in the 267 GHz continuum and HCO^+ J = 3-2 emission at 0".8 resolution, with the single-baseline interferometer of the James Clerk Maxwell Telescope-Caltech Submillimeter Observatory in the 357 GHz continuum and with the W. M. Keck Telescope at λ = 4 μm. The 267 GHz emission is unresolved, with a flux of 397±35 mJy, located close to the position of the optical star T Tau N. An upper limit of 100 mJy is obtained toward the infrared companion T Tau S. The 357 GHz continuum emission is unresolved, with a flux of 1.35±0.68 Jy. HCO^+ J = 3-2 was detected from a 2" diameter core surrounding T Tau N and S. Both stars are detected at 4 μm, but there is no evidence of the radio source T Tau R. We propose a model in which T Tau S is intrinsically similar to T Tau N but is obscured by the outer parts of T Tau N's disk. A fit to the spectral energy distribution (SED) between 21 cm and 1.22 μm is constructed on this basis. Adopting an r^(−1) surface density distribution and an exponentially truncated edge, disk masses of 0.04±0.01 and 6×10^(−5) to 3×10^(−3) M_☉ are inferred for T Tau N and T Tau S, respectively. A 0.005-0.03 M_☉ circumbinary envelope is also required to fit the millimeter to mid-infrared SED.
|Additional Information:||© 1997 American Astronomical Society. Received 1997 August 13; accepted 1997 September 24; published 1997 October 20. The authors wish to thank O. Lay for a critical reading of the manuscript and him and J. Carlstrom for assistance in the observation and reduction of the SBI data. The telescope staffs are thanked for support during the observations. E. v. D. acknowledges support by NWO/NFRA, G. A. B. by NASA (NAGW-2297, NAGW-1955), L. G. M. by NASA (NAG 5- 4429), and H. J. v. L. by the European Union (CHGECT920011). The OVRO Millimeter Array and the CSO are operated by the Caltech under funding from the NSF (AST96-13717, AST93-13929). The JCMT is operated by the Joint Astronomy Centre on behalf of PPARC UK, NWO Netherlands, and NRC Canada. The W. M. Keck Observatory is operated as a scientific partnership between Caltech, University of California, and NASA. It was made possible by the generous financial support of the W. M. Keck Foundation.|
|Subject Keywords:||binaries: close; ISM: molecules; stars: formation; stars: low-mass, brown dwarfs; stars: pre-main sequence|
|Official Citation:||Subarcsecond Imaging at 267 GHz of a Young Binary System: Detection of a Dust Disk of Radius Less than 70 AU around T Tauri N Michiel R. Hogerheijde et al. 1997 ApJ 490 L99|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||13 Sep 2012 18:07|
|Last Modified:||29 Aug 2014 14:47|
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