High angular resolution detection of β Pictoris b at 2.18 μ m

M. Bonnefoy; A. M. Lagrange; A. Boccaletti; G. Chauvin; D. Apai; F. Allard; D. Ehrenreich; J. H.V. Girard; D. Mouillet; D. Rouan; D. Gratadour; M. Kasper

doi:10.1051/0004-6361/201016224

High angular resolution detection of β Pictoris b at 2.18 μ m

M. Bonnefoy, A. M. Lagrange, A. Boccaletti, G. Chauvin, D. Apai, F. Allard, D. Ehrenreich, J. H.V. Girard, D. Mouillet, D. Rouan, D. Gratadour, M. Kasper

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Abstract

Context. A giant planet was recently discovered around the young star β Pictoris. This planet is the closest to its parent star ever imaged. With an estimated mass of about 9 M_Jup and separation of 8-15 AU, it explains most of the peculiarities of β Pictoris and its disk. Aims. Previous detections were made in the L′ band (3.8 μm) and at 4.05 μm. We recorded new K_s-band data (2.18 μm) in order to measure its color and get an additional estimate of its mass and effective temperature Methods. Angular differential K_s-band images of β Pictoris were recorded with NaCo in March and April 2010. Results. The companion is detected at K_s. This independently confirms the physical nature of β Pictoris b inferred from the L′ and NB-4.05 bands. The increase of the projected separation between October-December 2009 and April 2010 observations is consistent within error bars with the expected orbital motion. Using the absolute K_s photometry, "hot start" evolutionary models predict a mass of 7-11 M_Jup in agreement with previous estimates. Moreover, this mass is compatible with T_eff = 1700 ± 300 K derived from the comparison of the K_s - L′ color with those generated using synthetic spectra.

Original language	English (US)
Article number	L15
Journal	Astronomy and astrophysics
Volume	528
DOIs	https://doi.org/10.1051/0004-6361/201016224
State	Published - 2011

Keywords

instrumentation: adaptive optics
planetary systems
stars: early-type
stars: individual βPictoris

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/201016224

Cite this

@article{79fc8a77e53e4de2b0f1528c14763f1b,

title = "High angular resolution detection of β Pictoris b at 2.18 μ m",

abstract = "Context. A giant planet was recently discovered around the young star β Pictoris. This planet is the closest to its parent star ever imaged. With an estimated mass of about 9 MJup and separation of 8-15 AU, it explains most of the peculiarities of β Pictoris and its disk. Aims. Previous detections were made in the L′ band (3.8 μm) and at 4.05 μm. We recorded new Ks-band data (2.18 μm) in order to measure its color and get an additional estimate of its mass and effective temperature Methods. Angular differential Ks-band images of β Pictoris were recorded with NaCo in March and April 2010. Results. The companion is detected at Ks. This independently confirms the physical nature of β Pictoris b inferred from the L′ and NB-4.05 bands. The increase of the projected separation between October-December 2009 and April 2010 observations is consistent within error bars with the expected orbital motion. Using the absolute Ks photometry, {"}hot start{"} evolutionary models predict a mass of 7-11 MJup in agreement with previous estimates. Moreover, this mass is compatible with Teff = 1700 ± 300 K derived from the comparison of the Ks - L′ color with those generated using synthetic spectra.",

keywords = "instrumentation: adaptive optics, planetary systems, stars: early-type, stars: individual βPictoris",

author = "M. Bonnefoy and Lagrange, {A. M.} and A. Boccaletti and G. Chauvin and D. Apai and F. Allard and D. Ehrenreich and Girard, {J. H.V.} and D. Mouillet and D. Rouan and D. Gratadour and M. Kasper",

note = "Funding Information: We are gratefull to our anonymous referee for his very useful review. We would like to thank the ESO staff for his help. We acknowledge financial support from the French Programme National de Plan{\'e}tologie (PNP, INSU).",

year = "2011",

doi = "10.1051/0004-6361/201016224",

language = "English (US)",

volume = "528",

journal = "Astronomy and astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - High angular resolution detection of β Pictoris b at 2.18 μ m

AU - Bonnefoy, M.

AU - Lagrange, A. M.

AU - Boccaletti, A.

AU - Chauvin, G.

AU - Apai, D.

AU - Allard, F.

AU - Ehrenreich, D.

AU - Girard, J. H.V.

AU - Mouillet, D.

AU - Rouan, D.

AU - Gratadour, D.

AU - Kasper, M.

N1 - Funding Information: We are gratefull to our anonymous referee for his very useful review. We would like to thank the ESO staff for his help. We acknowledge financial support from the French Programme National de Planétologie (PNP, INSU).

PY - 2011

Y1 - 2011

N2 - Context. A giant planet was recently discovered around the young star β Pictoris. This planet is the closest to its parent star ever imaged. With an estimated mass of about 9 MJup and separation of 8-15 AU, it explains most of the peculiarities of β Pictoris and its disk. Aims. Previous detections were made in the L′ band (3.8 μm) and at 4.05 μm. We recorded new Ks-band data (2.18 μm) in order to measure its color and get an additional estimate of its mass and effective temperature Methods. Angular differential Ks-band images of β Pictoris were recorded with NaCo in March and April 2010. Results. The companion is detected at Ks. This independently confirms the physical nature of β Pictoris b inferred from the L′ and NB-4.05 bands. The increase of the projected separation between October-December 2009 and April 2010 observations is consistent within error bars with the expected orbital motion. Using the absolute Ks photometry, "hot start" evolutionary models predict a mass of 7-11 MJup in agreement with previous estimates. Moreover, this mass is compatible with Teff = 1700 ± 300 K derived from the comparison of the Ks - L′ color with those generated using synthetic spectra.

AB - Context. A giant planet was recently discovered around the young star β Pictoris. This planet is the closest to its parent star ever imaged. With an estimated mass of about 9 MJup and separation of 8-15 AU, it explains most of the peculiarities of β Pictoris and its disk. Aims. Previous detections were made in the L′ band (3.8 μm) and at 4.05 μm. We recorded new Ks-band data (2.18 μm) in order to measure its color and get an additional estimate of its mass and effective temperature Methods. Angular differential Ks-band images of β Pictoris were recorded with NaCo in March and April 2010. Results. The companion is detected at Ks. This independently confirms the physical nature of β Pictoris b inferred from the L′ and NB-4.05 bands. The increase of the projected separation between October-December 2009 and April 2010 observations is consistent within error bars with the expected orbital motion. Using the absolute Ks photometry, "hot start" evolutionary models predict a mass of 7-11 MJup in agreement with previous estimates. Moreover, this mass is compatible with Teff = 1700 ± 300 K derived from the comparison of the Ks - L′ color with those generated using synthetic spectra.

KW - instrumentation: adaptive optics

KW - planetary systems

KW - stars: early-type

KW - stars: individual βPictoris

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DO - 10.1051/0004-6361/201016224

M3 - Article

SN - 0004-6361

VL - 528

JO - Astronomy and astrophysics

JF - Astronomy and astrophysics

M1 - L15

ER -

High angular resolution detection of β Pictoris b at 2.18 μ m

Abstract

Keywords

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