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An accurate distance to 2M1207Ab

Ducourant, C. and Teixeira, R. and Chauvin, G. and Daigne, G. and Le Campion, J.-F. and Song, I. and Zuckerman, B. (2008) An accurate distance to 2M1207Ab. Astronomy and Astrophysics, 477 (1). L1-L4. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:DUCaanda08

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Abstract

Context. In April 2004, the first image was obtained of a planetary mass companion (now known as 2M1207 b) in orbit around a self-luminous object different from our own Sun (the young brown dwarf 2MASSW J1207334-393254, hereafter 2M1207 A). That 2M1207 b probably formed via fragmentation and gravitational collapse offered proof that such a mechanism can form bodies in the planetary mass regime. However, the predicted mass, luminosity, and radius of 2M1207 b depend on its age, distance, and other observables, such as effective temperature. Aims. To refine our knowledge of the physical properties of 2M1207 b and its nature, we accurately determined the distance to the 2M1207 A and b system by measuring of its trigonometric parallax at the milliarcsec level. Methods. With the ESO NTT/SUSI2 telescope, we began a campaign of photometric and astrometric observations in 2006 to measure the trigonometric parallax of 2M1207 A. Results. An accurate distance (52.4 ± 1.1 pc) to 2M1207A was measured. From distance and proper motions we derived spatial velocities that are fully compatible with TWA membership. Conclusions. With this new distance estimate, we discuss three scenarios regarding the nature of 2M1207 b: (1) a cool (1150 ± 150 K) companion of mass 4 ± 1 MJup, (2) a warmer (1600 ± 100 K) and heavier (8 ± 2 MJup) companion occulted by an edge-on circumsecondary disk, or (3) a hot protoplanet collision afterglow.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361:20078886DOIArticle
http://www.aanda.org/index.php?option=article&access=doi&doi=10.1051/0004-6361:20078886PublisherArticle
ORCID:
AuthorORCID
Ducourant, C.0000-0003-4843-8979
Song, I.0000-0002-5815-7372
Additional Information:© ESO 2007. Received 20 October 2007 / Accepted 6 November 2007. We would like to thank the staff of ESO-VLT and CFHT and Gilles Chabrier, Isabelle Baraffe, and France Allard for providing the latest update of their evolutionary models. We also acknowledge partial financial support from the Programmes Nationaux de Planétologie et de Physique Stellaire (PNP & PNPS) (in France), the Brazilian Organism FAPESP and CAPES, and the French Organism COFECUB.
Funders:
Funding AgencyGrant Number
Programmes Nationaux de Planétologie et de Physique Stellaire (PNP & PNPS)UNSPECIFIED
Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)UNSPECIFIED
French Organism COFECUBUNSPECIFIED
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)UNSPECIFIED
Subject Keywords:stars: distances; stars: low-mass, brown dwarfs; planetary sys
Issue or Number:1
Record Number:CaltechAUTHORS:DUCaanda08
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:DUCaanda08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13853
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Jun 2009 18:37
Last Modified:09 Mar 2020 13:18

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