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Properties of the young gas giant planet β Pictoris b

Published online by Cambridge University Press:  06 January 2014

Mickaël Bonnefoy
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany email: bonnefoy@mpia-hd.mpg.de
Anthony Boccaletti
Affiliation:
LESIA, Observatoire de Paris, CNRS, University Pierre et Marie Curie Paris 6 and University Denis Diderot Paris 7, 5 place Jules Janssen, 92195 Meudon, France
Anne-Marie Lagrange
Affiliation:
UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
France Allard
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 Allée d'Italie, F-69364 Lyon Cedex 07, France
Christoph Mordasini
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany email: bonnefoy@mpia-hd.mpg.de
Hervé Beust
Affiliation:
UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
Gaël Chauvin
Affiliation:
UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
Julien H. V. Girard
Affiliation:
European Southern Observatory, Casilla 19001, Santiago 19, Chile
Derek Homeier
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 Allée d'Italie, F-69364 Lyon Cedex 07, France
Daniel Apai
Affiliation:
Department of Astronomy, 933 N. Cherrt Avenue, Tuscon, AZ 85721, USA Department of Planetary Sciences, The University of Arizona, 1929 E. University Blvd., Tuscon, AZ 85721, USA
Sylvestre Lacour
Affiliation:
LESIA, Observatoire de Paris, CNRS, University Pierre et Marie Curie Paris 6 and University Denis Diderot Paris 7, 5 place Jules Janssen, 92195 Meudon, France
Daniel Rouan
Affiliation:
LESIA, Observatoire de Paris, CNRS, University Pierre et Marie Curie Paris 6 and University Denis Diderot Paris 7, 5 place Jules Janssen, 92195 Meudon, France
Julien Rameau
Affiliation:
UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
Hubert Klahr
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany email: bonnefoy@mpia-hd.mpg.de
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Abstract

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The young (12+8−4 Myr) and nearby (19.44±0.05 pc) star β Pictoris is considered one of the best laboratories for the study of early phases of planetary systems formation since the identification of an extended debris disk surrounding the star in 1984. In 2009, we imaged at 3.8 μm with NaCo at VLT a gas giant planet around β Pictoris, roughly along the disk mid-plane, with a semi-major axis between 8 and 14 AU. We present here the first images of the planet in the J (1.265 μm), H (1.66 μm), and M' (4.78 μm) bands obtained between 2011 and 2012. We used these data to build the 1-5 μm spectral energy distribution (SED) of the companion, and to consolidate previous semi-major axis (8-10 AU) estimates. We compared the SED to seven atmospheric models to derive Teff = 1700 ± 100 K. We used the temperature and the luminosity of β Pictoris b to estimate new masses for the companion. We compared these masses to independent constraints set by the orbital parameters and the radial velocities and use them to discuss the formation history of the object.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

References

Smith, B. A., & Terrile, R. J. 1984, Science, 226, 1421CrossRefGoogle ScholarPubMed
Lagrange, A.-M., Bonnefoy, M.et al. 2010, Science, 329, 57CrossRefGoogle Scholar
Chabrier, G., Baraffe, I., Allard, F., & Hauschildt, P. 2000, ApJ, 542, 464CrossRefGoogle Scholar
Baraffe, I., Chabrier, G., Barman, T. S., Allard, F., & Hauschildt, P. H. 2003, ApJ, 402, 701Google Scholar
Marois, C., Lafrenière, D., Macintosh, B., & Doyon, R. 2006, ApJ, 647, 612CrossRefGoogle Scholar
Lafrenière, D., Marois, C., Doyon, R., Nadeau, D., & Artigau, E. 2007, ApJ, 660, 770CrossRefGoogle Scholar
Soummer, R., Pueyo, L., & Larkin, J. 2012, ApJ, 755, 28CrossRefGoogle Scholar
Chauvin, G., Lagrange, A.-M., Beust, H., Bonnefoy, M., et al. 2012, A&A, 542, 41Google Scholar
Bonnefoy, M., Boccaletti, A., Lagrange, A.-M., et al. 2013, A&A, 555, 107Google Scholar
Lagrange, A.-M., De Bondt, K., Meunier, N., Sterzik, M., et al. 2012, A&A, 542, 18Google Scholar
Bonnefoy, M., Lagrange, A.-M., Boccaletti, A., Chauvin, G., et al. 2011, A&A, 528, 15Google Scholar
Todorov, K., Luhman, K. L., & McLeod, K. K. 2010, ApJ, 714, 84CrossRefGoogle Scholar
Faherty, J. K., Rice, E. L., & Cruz, K. L. 2013, AJ, 145, 2CrossRefGoogle Scholar
Lagrange, A.-M., Gratadour, D., Chauvin, , et al. 2009, A&A, 493, 21Google Scholar
Quanz, S. P., Meyer, M. R., Kenworthy, M. A., et al. 2010, ApJ, 722, 49CrossRefGoogle Scholar
Marley, M. S., Fortney, J. J., Hubickyj, O., et al. 2007, ApJ, 655, 541CrossRefGoogle Scholar
Spiegel, D. S. & Burrows, A. 2012, ApJ, 745, 174CrossRefGoogle Scholar
Marleau, G.-D., & Cumming, A. 2013, MNRAS, Submitted. astro-ph: 1302.1517Google Scholar
Rameau, J., Chauvin, G., Lagrange, A.-M., & Klahr, H. 2013, A&A, 553, 60Google Scholar
Mordasini, C., Alibert, Y., Klahr, H., & Henning, T. 2012, A&A, 547, 111Google Scholar
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Properties of the young gas giant planet β Pictoris b
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