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On the circum(sub)stellar environment of brown dwarfs in Taurus

Guieu, S. and Pinte, C. and Monin, J.-L. and Ménard, F. and Fukagawa, M. and Padgett, D. L. and Noriega-Crespo, A. and Carey, S. J. and Rebull, L. M. and Huard, T. and Guedel, M. (2007) On the circum(sub)stellar environment of brown dwarfs in Taurus. Astronomy and Astrophysics, 465 (3). pp. 855-864. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20100223-131013626

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Abstract

Aims. We want to investigate whether brown dwarfs (BDs) form like stars or are ejected embryos. We study the presence of disks around BDs in the Taurus cloud, and discuss implications for substellar formation models. Methods. We use photometric measurements from the visible to the far infrared to determine the spectral energy distributions (SEDs) of Taurus BDs. Results. We use Spitzer color indices, Hα as an accretion indicator, and models fit to the SEDs in order to estimate physical parameters of the disks around these BDs. We study the spatial distribution of BDs with and without disks across the Taurus aggregates, and we find that BDs with and without disks are not distributed regularly across the Taurus cloud. Conclusions. We find that 48%±14% of Taurus BDs have a circumstellar disk signature, a ratio similar to recent results from previous authors in other regions. We fit the SEDs and find that none of the disks around BDs in Taurus can be fitted convincingly with a flaring index β = 0, indicating that heating by the central object is efficient and that the disks we observe retain a significant amount of gas. We find that BDs with disks are proportionally more numerous in the northern Taurus filament, possibly the youngest filament. We do not find such a clear segregation for classical T Tauri stars (CTTS) and weak-lined T Tauri stars (WTTS), suggesting that, in addition to the effects of evolution, any segregation effects could be related to the mass of the object. A by-product of our study is to propose a recalibration of the Barrado y Navascués & Martín (2003) accretion limit in the substellar domain. The global shape of the limit fits our data points if it is raised by a factor 1.25–1.30.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361:20066140DOIArticle
ORCID:
AuthorORCID
Pinte, C.0000-0001-5907-5179
Padgett, D. L.0000-0001-5334-5107
Noriega-Crespo, A.0000-0002-6296-8960
Carey, S. J.0000-0002-0221-6871
Rebull, L. M.0000-0001-6381-515X
Additional Information:© ESO 2007. Received 28 July 2006. Accepted 18 December 2006. We thank Cathie Clarke and Anthony Whitworth for enlightening discussions about BD formation models, and an anonymous referee for a detailed report that helped clarify many points in our paper. This research has made use of the CDS database. F.M. thanks the “Center for long Wavelength Astrophysics” for supporting a visit at JPL. We thank the Programme National de Physique Stellaire (PNPS, CNRS/INSU, France) for financial support.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Programme National de Physique Stellaire (PNPS)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Subject Keywords:stars: formation -- stars: low mass, brown dwarfs -- stars: pre-main sequence -- stars: planetary systems: protoplanetary disks -- stars: circumstellar matter
Issue or Number:3
Record Number:CaltechAUTHORS:20100223-131013626
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20100223-131013626
Official Citation:On the circum(sub)stellar environment of brown dwarfs in Taurus S. Guieu, C. Pinte, J.-L. Monin, F. Ménard, M. Fukagawa, D. L. Padgett, A. Noriega-Crespo, S. J. Carey, L. M. Rebull, T. Huard and M. Guedel A&A 465 (3) 855-864 (2007) DOI: 10.1051/0004-6361:20066140
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17565
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:02 Mar 2010 17:14
Last Modified:01 Nov 2019 17:10

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