Gemini planet imager spectroscopy of the HR 8799 planets c and d

Patrick Ingraham, Mark S. Marley, Didier Saumon, Christian Marois, Bruce Macintosh, Travis S Barman, Brian Bauman, Adam Burrows, Jeffrey K. Chilcote, Robert J. De Rosa, Daren Dillon, René Doyon, Jennifer Dunn, Darren Erikson, Michael P. Fitzgerald, Donald Gavel, Stephen J. Goodsell, James R. Graham, Markus Hartung, Pascale HibonPaul G. Kalas, Quinn Konopacky, James A. Larkin, Jérôme Maire, Franck Marchis, James McBride, Max Millar-Blanchaer, Katie M. Morzinski, Andrew Norton, Rebecca Oppenheimer, Dave W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Fredrik Rantakyrö, Naru Sadakuni, Leslie Saddlemyer, Dmitry Savransky, Rémi Soummer, Anand Sivaramakrishnan, Inseok Song, Sandrine Thomas, J. Kent Wallace, Sloane J. Wiktorowicz, Schuyler G. Wolff

Research output: Contribution to journalArticle

36 Citations (Scopus)

Abstract

During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 μm photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.

Original languageEnglish (US)
Article numberL15
JournalAstrophysical Journal Letters
Volume794
Issue number1
DOIs
StatePublished - Oct 10 2014

Fingerprint

planets
planet
spectroscopy
cloud cover
extrasolar planets
spectral energy distribution
extremely high frequencies
opacity
disequilibrium
metallicity
methane
chemistry
wavelength
wavelengths
modeling
energy

Keywords

  • infrared: planetary systems
  • instrumentation: adaptive optics
  • instrumentation: high angular resolution
  • planets and satellites: atmospheres
  • planets and satellites: gaseous planets
  • techniques: imaging spectroscopy

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Ingraham, P., Marley, M. S., Saumon, D., Marois, C., Macintosh, B., Barman, T. S., ... Wolff, S. G. (2014). Gemini planet imager spectroscopy of the HR 8799 planets c and d. Astrophysical Journal Letters, 794(1), [L15]. https://doi.org/10.1088/2041-8205/794/1/L15

Gemini planet imager spectroscopy of the HR 8799 planets c and d. / Ingraham, Patrick; Marley, Mark S.; Saumon, Didier; Marois, Christian; Macintosh, Bruce; Barman, Travis S; Bauman, Brian; Burrows, Adam; Chilcote, Jeffrey K.; De Rosa, Robert J.; Dillon, Daren; Doyon, René; Dunn, Jennifer; Erikson, Darren; Fitzgerald, Michael P.; Gavel, Donald; Goodsell, Stephen J.; Graham, James R.; Hartung, Markus; Hibon, Pascale; Kalas, Paul G.; Konopacky, Quinn; Larkin, James A.; Maire, Jérôme; Marchis, Franck; McBride, James; Millar-Blanchaer, Max; Morzinski, Katie M.; Norton, Andrew; Oppenheimer, Rebecca; Palmer, Dave W.; Patience, Jenny; Perrin, Marshall D.; Poyneer, Lisa A.; Pueyo, Laurent; Rantakyrö, Fredrik; Sadakuni, Naru; Saddlemyer, Leslie; Savransky, Dmitry; Soummer, Rémi; Sivaramakrishnan, Anand; Song, Inseok; Thomas, Sandrine; Kent Wallace, J.; Wiktorowicz, Sloane J.; Wolff, Schuyler G.

In: Astrophysical Journal Letters, Vol. 794, No. 1, L15, 10.10.2014.

Research output: Contribution to journalArticle

Ingraham, P, Marley, MS, Saumon, D, Marois, C, Macintosh, B, Barman, TS, Bauman, B, Burrows, A, Chilcote, JK, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Fitzgerald, MP, Gavel, D, Goodsell, SJ, Graham, JR, Hartung, M, Hibon, P, Kalas, PG, Konopacky, Q, Larkin, JA, Maire, J, Marchis, F, McBride, J, Millar-Blanchaer, M, Morzinski, KM, Norton, A, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Pueyo, L, Rantakyrö, F, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Kent Wallace, J, Wiktorowicz, SJ & Wolff, SG 2014, 'Gemini planet imager spectroscopy of the HR 8799 planets c and d', Astrophysical Journal Letters, vol. 794, no. 1, L15. https://doi.org/10.1088/2041-8205/794/1/L15
Ingraham, Patrick ; Marley, Mark S. ; Saumon, Didier ; Marois, Christian ; Macintosh, Bruce ; Barman, Travis S ; Bauman, Brian ; Burrows, Adam ; Chilcote, Jeffrey K. ; De Rosa, Robert J. ; Dillon, Daren ; Doyon, René ; Dunn, Jennifer ; Erikson, Darren ; Fitzgerald, Michael P. ; Gavel, Donald ; Goodsell, Stephen J. ; Graham, James R. ; Hartung, Markus ; Hibon, Pascale ; Kalas, Paul G. ; Konopacky, Quinn ; Larkin, James A. ; Maire, Jérôme ; Marchis, Franck ; McBride, James ; Millar-Blanchaer, Max ; Morzinski, Katie M. ; Norton, Andrew ; Oppenheimer, Rebecca ; Palmer, Dave W. ; Patience, Jenny ; Perrin, Marshall D. ; Poyneer, Lisa A. ; Pueyo, Laurent ; Rantakyrö, Fredrik ; Sadakuni, Naru ; Saddlemyer, Leslie ; Savransky, Dmitry ; Soummer, Rémi ; Sivaramakrishnan, Anand ; Song, Inseok ; Thomas, Sandrine ; Kent Wallace, J. ; Wiktorowicz, Sloane J. ; Wolff, Schuyler G. / Gemini planet imager spectroscopy of the HR 8799 planets c and d. In: Astrophysical Journal Letters. 2014 ; Vol. 794, No. 1.
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abstract = "During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 μm photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.",
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AU - Marley, Mark S.

AU - Saumon, Didier

AU - Marois, Christian

AU - Macintosh, Bruce

AU - Barman, Travis S

AU - Bauman, Brian

AU - Burrows, Adam

AU - Chilcote, Jeffrey K.

AU - De Rosa, Robert J.

AU - Dillon, Daren

AU - Doyon, René

AU - Dunn, Jennifer

AU - Erikson, Darren

AU - Fitzgerald, Michael P.

AU - Gavel, Donald

AU - Goodsell, Stephen J.

AU - Graham, James R.

AU - Hartung, Markus

AU - Hibon, Pascale

AU - Kalas, Paul G.

AU - Konopacky, Quinn

AU - Larkin, James A.

AU - Maire, Jérôme

AU - Marchis, Franck

AU - McBride, James

AU - Millar-Blanchaer, Max

AU - Morzinski, Katie M.

AU - Norton, Andrew

AU - Oppenheimer, Rebecca

AU - Palmer, Dave W.

AU - Patience, Jenny

AU - Perrin, Marshall D.

AU - Poyneer, Lisa A.

AU - Pueyo, Laurent

AU - Rantakyrö, Fredrik

AU - Sadakuni, Naru

AU - Saddlemyer, Leslie

AU - Savransky, Dmitry

AU - Soummer, Rémi

AU - Sivaramakrishnan, Anand

AU - Song, Inseok

AU - Thomas, Sandrine

AU - Kent Wallace, J.

AU - Wiktorowicz, Sloane J.

AU - Wolff, Schuyler G.

PY - 2014/10/10

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N2 - During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 μm photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.

AB - During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 μm photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.

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KW - instrumentation: adaptive optics

KW - instrumentation: high angular resolution

KW - planets and satellites: atmospheres

KW - planets and satellites: gaseous planets

KW - techniques: imaging spectroscopy

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