The near-infrared spectral energy distribution of β Pictoris b

M. Bonnefoy, A. Boccaletti, A. M. Lagrange, F. Allard, C. Mordasini, H. Beust, G. Chauvin, J. H V Girard, D. Homeier, Daniel Apai, S. Lacour, D. Rouan

Research output: Contribution to journalArticle

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Abstract

Context. A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ∼12 Myr old star Pictoris. The β Pictoris system offers the rare opportunity of both studying the physical and atmospheric properties of an exoplanet placed on a wide orbit and establishing its formation scenario. Aims. We aim to build the 1-5 μm spectral energy distribution of the planet for the first time. Our goal is to provide secure and accurate constraints on its physical and chemical properties. Methods. We obtained J (1.265 μm), H (1.66 μm), and M0 (4.78 μm) band angular differential imaging of the system between 2011 and 2012.We used Markov chain Monte Carlo simulations of the astrometric data to revise constraints on the orbital parameters of the planet. Photometric measurements were compared to those of ultra-cool dwarfs and young companions. They were combined with existing photometry (2.18, 3.80, and 4.05 μm) and compared to predictions from 7 PHOENIX-based atmospheric models in order to derive the atmospheric parameters (Teff, log g) of β Pictoris b. Predicted properties from ("hot-start", "cold-start", and "warm start") evolutionary models were compared to independent constraints on the mass of β Pictoris b. We used planet-population synthesis models following the core-accretion paradigm to discuss the planet's possible origin. Results. We detect the planetary companion in our four-epoch observations. We estimate J = 14:0 ± 0:3, H = 13:5 ± 0:2, and M0 = 11:0 ± 0:3 mag. Our new astrometry consolidates previous semi-major axis (8-10 AU) and excentricity (e 0:15) estimates of the planet. The location of β Pictoris b in color-magnitude diagrams suggests it has spectroscopic properties similar to L0-L4 dwarfs. This enables one to derive Log10 (L=L ·) =-3.87±0.08 for the companion. The analysis with atmospheric models reveals that the planet has a dusty atmosphere with Teff = 1700 ± 100 K and log q =4.0 ± 0.5. "Hot-start" evolutionary models give a new mass of 10+3 -2 Mjup from Teff and 9+3 -2 Mjup from luminosity. Predictions of "Cold-start" models are still inconsistent with independent constraints on the planet mass. "Warm-start" models constrains the mass to M≥ 6 Mjup and the initial entropies to value (Sinit≥9.3k b/baryon) midway between those considered for cold/hot-start models, but probably closer to those of hot-start models.

Original languageEnglish (US)
Article numberA107
JournalAstronomy and Astrophysics
Volume555
DOIs
StatePublished - 2013

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spectral energy distribution
near infrared
planet
planets
energy
atmospheric models
planetary evolution
physical properties
gas giant planets
astrometry
color-magnitude diagram
Markov chains
extrasolar planets
estimates
predictions
distribution
debris
chemical properties
Markov chain
prediction

Keywords

  • Instrumentation: adaptive optics
  • Planetary systems
  • Planets and satellites: atmospheres
  • Planets and satellites: fundamental parameters
  • Stars: individual:βPic b
  • Techniques: photometric

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Bonnefoy, M., Boccaletti, A., Lagrange, A. M., Allard, F., Mordasini, C., Beust, H., ... Rouan, D. (2013). The near-infrared spectral energy distribution of β Pictoris b. Astronomy and Astrophysics, 555, [A107]. https://doi.org/10.1051/0004-6361/201220838

The near-infrared spectral energy distribution of β Pictoris b. / Bonnefoy, M.; Boccaletti, A.; Lagrange, A. M.; Allard, F.; Mordasini, C.; Beust, H.; Chauvin, G.; Girard, J. H V; Homeier, D.; Apai, Daniel; Lacour, S.; Rouan, D.

In: Astronomy and Astrophysics, Vol. 555, A107, 2013.

Research output: Contribution to journalArticle

Bonnefoy, M, Boccaletti, A, Lagrange, AM, Allard, F, Mordasini, C, Beust, H, Chauvin, G, Girard, JHV, Homeier, D, Apai, D, Lacour, S & Rouan, D 2013, 'The near-infrared spectral energy distribution of β Pictoris b', Astronomy and Astrophysics, vol. 555, A107. https://doi.org/10.1051/0004-6361/201220838
Bonnefoy M, Boccaletti A, Lagrange AM, Allard F, Mordasini C, Beust H et al. The near-infrared spectral energy distribution of β Pictoris b. Astronomy and Astrophysics. 2013;555. A107. https://doi.org/10.1051/0004-6361/201220838
Bonnefoy, M. ; Boccaletti, A. ; Lagrange, A. M. ; Allard, F. ; Mordasini, C. ; Beust, H. ; Chauvin, G. ; Girard, J. H V ; Homeier, D. ; Apai, Daniel ; Lacour, S. ; Rouan, D. / The near-infrared spectral energy distribution of β Pictoris b. In: Astronomy and Astrophysics. 2013 ; Vol. 555.
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abstract = "Context. A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ∼12 Myr old star Pictoris. The β Pictoris system offers the rare opportunity of both studying the physical and atmospheric properties of an exoplanet placed on a wide orbit and establishing its formation scenario. Aims. We aim to build the 1-5 μm spectral energy distribution of the planet for the first time. Our goal is to provide secure and accurate constraints on its physical and chemical properties. Methods. We obtained J (1.265 μm), H (1.66 μm), and M0 (4.78 μm) band angular differential imaging of the system between 2011 and 2012.We used Markov chain Monte Carlo simulations of the astrometric data to revise constraints on the orbital parameters of the planet. Photometric measurements were compared to those of ultra-cool dwarfs and young companions. They were combined with existing photometry (2.18, 3.80, and 4.05 μm) and compared to predictions from 7 PHOENIX-based atmospheric models in order to derive the atmospheric parameters (Teff, log g) of β Pictoris b. Predicted properties from ({"}hot-start{"}, {"}cold-start{"}, and {"}warm start{"}) evolutionary models were compared to independent constraints on the mass of β Pictoris b. We used planet-population synthesis models following the core-accretion paradigm to discuss the planet's possible origin. Results. We detect the planetary companion in our four-epoch observations. We estimate J = 14:0 ± 0:3, H = 13:5 ± 0:2, and M0 = 11:0 ± 0:3 mag. Our new astrometry consolidates previous semi-major axis (8-10 AU) and excentricity (e 0:15) estimates of the planet. The location of β Pictoris b in color-magnitude diagrams suggests it has spectroscopic properties similar to L0-L4 dwarfs. This enables one to derive Log10 (L=L ·) =-3.87±0.08 for the companion. The analysis with atmospheric models reveals that the planet has a dusty atmosphere with Teff = 1700 ± 100 K and log q =4.0 ± 0.5. {"}Hot-start{"} evolutionary models give a new mass of 10+3 -2 Mjup from Teff and 9+3 -2 Mjup from luminosity. Predictions of {"}Cold-start{"} models are still inconsistent with independent constraints on the planet mass. {"}Warm-start{"} models constrains the mass to M≥ 6 Mjup and the initial entropies to value (Sinit≥9.3k b/baryon) midway between those considered for cold/hot-start models, but probably closer to those of hot-start models.",
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T1 - The near-infrared spectral energy distribution of β Pictoris b

AU - Bonnefoy, M.

AU - Boccaletti, A.

AU - Lagrange, A. M.

AU - Allard, F.

AU - Mordasini, C.

AU - Beust, H.

AU - Chauvin, G.

AU - Girard, J. H V

AU - Homeier, D.

AU - Apai, Daniel

AU - Lacour, S.

AU - Rouan, D.

PY - 2013

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N2 - Context. A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ∼12 Myr old star Pictoris. The β Pictoris system offers the rare opportunity of both studying the physical and atmospheric properties of an exoplanet placed on a wide orbit and establishing its formation scenario. Aims. We aim to build the 1-5 μm spectral energy distribution of the planet for the first time. Our goal is to provide secure and accurate constraints on its physical and chemical properties. Methods. We obtained J (1.265 μm), H (1.66 μm), and M0 (4.78 μm) band angular differential imaging of the system between 2011 and 2012.We used Markov chain Monte Carlo simulations of the astrometric data to revise constraints on the orbital parameters of the planet. Photometric measurements were compared to those of ultra-cool dwarfs and young companions. They were combined with existing photometry (2.18, 3.80, and 4.05 μm) and compared to predictions from 7 PHOENIX-based atmospheric models in order to derive the atmospheric parameters (Teff, log g) of β Pictoris b. Predicted properties from ("hot-start", "cold-start", and "warm start") evolutionary models were compared to independent constraints on the mass of β Pictoris b. We used planet-population synthesis models following the core-accretion paradigm to discuss the planet's possible origin. Results. We detect the planetary companion in our four-epoch observations. We estimate J = 14:0 ± 0:3, H = 13:5 ± 0:2, and M0 = 11:0 ± 0:3 mag. Our new astrometry consolidates previous semi-major axis (8-10 AU) and excentricity (e 0:15) estimates of the planet. The location of β Pictoris b in color-magnitude diagrams suggests it has spectroscopic properties similar to L0-L4 dwarfs. This enables one to derive Log10 (L=L ·) =-3.87±0.08 for the companion. The analysis with atmospheric models reveals that the planet has a dusty atmosphere with Teff = 1700 ± 100 K and log q =4.0 ± 0.5. "Hot-start" evolutionary models give a new mass of 10+3 -2 Mjup from Teff and 9+3 -2 Mjup from luminosity. Predictions of "Cold-start" models are still inconsistent with independent constraints on the planet mass. "Warm-start" models constrains the mass to M≥ 6 Mjup and the initial entropies to value (Sinit≥9.3k b/baryon) midway between those considered for cold/hot-start models, but probably closer to those of hot-start models.

AB - Context. A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ∼12 Myr old star Pictoris. The β Pictoris system offers the rare opportunity of both studying the physical and atmospheric properties of an exoplanet placed on a wide orbit and establishing its formation scenario. Aims. We aim to build the 1-5 μm spectral energy distribution of the planet for the first time. Our goal is to provide secure and accurate constraints on its physical and chemical properties. Methods. We obtained J (1.265 μm), H (1.66 μm), and M0 (4.78 μm) band angular differential imaging of the system between 2011 and 2012.We used Markov chain Monte Carlo simulations of the astrometric data to revise constraints on the orbital parameters of the planet. Photometric measurements were compared to those of ultra-cool dwarfs and young companions. They were combined with existing photometry (2.18, 3.80, and 4.05 μm) and compared to predictions from 7 PHOENIX-based atmospheric models in order to derive the atmospheric parameters (Teff, log g) of β Pictoris b. Predicted properties from ("hot-start", "cold-start", and "warm start") evolutionary models were compared to independent constraints on the mass of β Pictoris b. We used planet-population synthesis models following the core-accretion paradigm to discuss the planet's possible origin. Results. We detect the planetary companion in our four-epoch observations. We estimate J = 14:0 ± 0:3, H = 13:5 ± 0:2, and M0 = 11:0 ± 0:3 mag. Our new astrometry consolidates previous semi-major axis (8-10 AU) and excentricity (e 0:15) estimates of the planet. The location of β Pictoris b in color-magnitude diagrams suggests it has spectroscopic properties similar to L0-L4 dwarfs. This enables one to derive Log10 (L=L ·) =-3.87±0.08 for the companion. The analysis with atmospheric models reveals that the planet has a dusty atmosphere with Teff = 1700 ± 100 K and log q =4.0 ± 0.5. "Hot-start" evolutionary models give a new mass of 10+3 -2 Mjup from Teff and 9+3 -2 Mjup from luminosity. Predictions of "Cold-start" models are still inconsistent with independent constraints on the planet mass. "Warm-start" models constrains the mass to M≥ 6 Mjup and the initial entropies to value (Sinit≥9.3k b/baryon) midway between those considered for cold/hot-start models, but probably closer to those of hot-start models.

KW - Instrumentation: adaptive optics

KW - Planetary systems

KW - Planets and satellites: atmospheres

KW - Planets and satellites: fundamental parameters

KW - Stars: individual:βPic b

KW - Techniques: photometric

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