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A proto brown dwarf candidate in Taurus

Barrado, D. and Morales-Calderón, M. and Palau, A. and Bayo, A. and de Gregorio-Monsalvo, I. and Eiroa, C. and Huélamo, N. and Bouy, H. and Morata, Ò and Schmidtobreick, L. (2009) A proto brown dwarf candidate in Taurus. Astronomy and Astrophysics, 508 (2). pp. 859-867. ISSN 0004-6361.

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Aims. We search for brown dwarfs at the Class 0/I evolutionary stage, or proto brown dwarfs. Methods. We present a multi wavelength study, ranging from optical at 0.8 μm to radio wavelengths at 6 cm, of a cool, very faint, and red multiple object, SSTB213 J041757, detected by Spitzer toward the Barnard 213 dark cloud, in Taurus. Results. The SED of SSTB213 J041757 displays a clear excess at long wavelengths resembling that of a Class I object. The mid-IR source has two possible counterparts, A and B, in the near-IR and optical images, and the 350 μm observations detect clear extended emission, presumably from an envelope around the two sources. The position of A & B in the (Ic− J) versus (J − [3.6]) colour-colour diagram is consistent with them being Galactic sources and not extragalactic contaminants. A proper-motion study confirms this result for A, while it is inconclusive for B. The temperature and mass of the two possible central objects, according to COND evolutionary models, range between 1550−1750 K and 3−4 M_(Jupiter), and 950−1300 K and 1−2 M_(Jupiter), for A and B, respectively. The integrated SED provides bolometric temperatures and luminosities of 280 K and 0.0034 L_⊙, assuming that the emission at wavelengths > 5 μm is associated with component A, and 150 K and 0.0033 L_⊙, assuming that the emission at wavelengths > 5 μm is associated with component B, which would imply the SSTB213 J041757 object has a luminosity well below the luminosity of other very low luminosity objects discovered up to date. Conclusions. With these characteristics, SSTB213 J041757 seems to be a promising, and perhaps double, proto brown dwarf candidate.

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Huélamo, N.0000-0002-2711-8143
Additional Information:© ESO 2009. Received 4 April 2009. Accepted 22 September 2009. We deeply thank Calar Alto and IRAM Observatories for allocation of director’s discretionary time to this programme. We are deeply grateful to A. Kovacks, S. Leon, R. Zylka and C. Vlahakis for assistance in the reduction of the CSO and IRAM data. The paper is also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. We do appreciate the discussions with A. Alonso-Herrero, and P. Pérez González, and the contributions from C. Young, and M. Dunham. We are grateful to the anonymous referee for very detailed and useful discussions which have led to the improving the paper. This research has been funded by Spanish grants ESP2007-65475-C02-02, AYA2008-06189-C03, AYA2008-1727, CSD2006-00070 and PRICITS-0505/ESP/0361.
Funding AgencyGrant Number
Ministerio de Ciencia e Innovación (MCINN)ESP2007-65475-C02-02
Ministerio de Ciencia e Innovación (MCINN)AYA2008-06189-C03
Ministerio de Ciencia e Innovación (MCINN)AYA2008-1727
Ministerio de Ciencia e Innovación (MCINN)CSD2006-00070
Ministerio de Ciencia e Innovación (MCINN)PRICITS-0505/ESP/0361
Subject Keywords:circumstellar matter; stars: formation; stars: low-mass, brown dwarfs; stars: pre-main sequence; infrared: stars
Issue or Number:2
Record Number:CaltechAUTHORS:20100127-101344607
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Official Citation:A proto brown dwarf candidate in Taurus D. Barrado, M. Morales-Calderón, A. Palau, A. Bayo, I. de Gregorio-Monsalvo, C. Eiroa, N. Huélamo, H. Bouy, O. Morata and L. Schmidtobreick A&A 508 (2) 859-867 (2009) DOI: 10.1051/0004-6361/200912276
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17317
Deposited By: Tony Diaz
Deposited On:28 Jan 2010 19:28
Last Modified:01 Nov 2019 23:40

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