TY - GEN
T1 - Properties of the young gas giant planet β Pictoris b
AU - Bonnefoy, Mickaël
AU - Boccaletti, Anthony
AU - Lagrange, Anne Marie
AU - Allard, France
AU - Mordasini, Christoph
AU - Beust, Hervé
AU - Chauvin, Gaël
AU - Girard, Julien H.V.
AU - Homeier, Derek
AU - Apai, Daniel
AU - Lacour, Sylvestre
AU - Rouan, Daniel
AU - Rameau, Julien
AU - Klahr, Hubert
PY - 2013/6
Y1 - 2013/6
N2 - 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.
AB - 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.
KW - Atmosphere
KW - Evolution
KW - Exoplanets: formation
KW - High angular resolution
KW - Instrumentation: adaptive optics
KW - Stars: β Pictoris
UR - http://www.scopus.com/inward/record.url?scp=84891886109&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84891886109&partnerID=8YFLogxK
U2 - 10.1017/S174392131300848X
DO - 10.1017/S174392131300848X
M3 - Conference contribution
AN - SCOPUS:84891886109
SN - 9781107045200
T3 - Proceedings of the International Astronomical Union
SP - 241
EP - 246
BT - Exploring the Formation and Evolution of Planetary Systems
PB - Cambridge University Press
ER -