Dynamical Constraints on the HR 8799 Planets with GPI

Jason J. Wang; James R. Graham; Rebekah Dawson; Daniel Fabrycky; Robert J. De Rosa; Laurent Pueyo; Quinn Konopacky; Bruce Macintosh; Christian Marois; Eugene Chiang; S. Mark Ammons; Pauline Arriaga; Vanessa P. Bailey; Travis Barman; Joanna Bulger; Jeffrey Chilcote; Tara Cotten; Rene Doyon; Gaspard Duchêne; Thomas M. Esposito; Michael P. Fitzgerald; Katherine B. Follette; Benjamin L. Gerard; Stephen J. Goodsell; Alexandra Z. Greenbaum; Pascale Hibon; Li Wei Hung; Patrick Ingraham; Paul Kalas; James E. Larkin; Jérôme Maire; Franck Marchis; Mark S. Marley; Stanimir Metchev; Maxwell A. Millar-Blanchaer; Eric L. Nielsen; Rebecca Oppenheimer; David Palmer; Jennifer Patience; Marshall Perrin; Lisa Poyneer; Abhijith Rajan; Julien Rameau; Fredrik T. Rantakyrö; Jean Baptiste Ruffio; Dmitry Savransky; Adam C. Schneider; Anand Sivaramakrishnan; Inseok Song; Remi Soummer; Sandrine Thomas; J. Kent Wallace; Kimberly Ward-Duong; Sloane Wiktorowicz; Schuyler Wolff

doi:10.3847/1538-3881/aae150

Dynamical Constraints on the HR 8799 Planets with GPI

Jason J. Wang, James R. Graham, Rebekah Dawson, Daniel Fabrycky, Robert J. De Rosa, Laurent Pueyo, Quinn Konopacky, Bruce Macintosh, Christian Marois, Eugene Chiang, S. Mark Ammons, Pauline Arriaga, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Jeffrey Chilcote, Tara Cotten, Rene Doyon, Gaspard Duchêne, Thomas M. EspositoMichael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Li Wei Hung, Patrick Ingraham, Paul Kalas, James E. Larkin, Jérôme Maire, Franck Marchis, Mark S. Marley, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Jean Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, Schuyler Wolff

Research output: Contribution to journal › Article › peer-review

86 Scopus citations

Abstract

The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system's dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager, we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through N-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets' orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above 6 M _Jup and 7 M _Jup, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of 42 ± 5 Myr, we found the mass of planet b to be 5.8 ± 0.5 M _Jup, and the masses of planets c, d, and e to be each.

Original language	English (US)
Article number	192
Journal	Astronomical Journal
Volume	156
Issue number	5
DOIs	https://doi.org/10.3847/1538-3881/aae150
State	Published - Nov 2018

Keywords

astrometry
planetdisk interactions
planets and satellites: dynamical evolution and stability
planets and satellites: gaseous planets
stars: individual (HR 8799)
techniques: high angular resolution

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-3881/aae150

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Wang, J. J., Graham, J. R., Dawson, R., Fabrycky, D., De Rosa, R. J., Pueyo, L., Konopacky, Q., Macintosh, B., Marois, C., Chiang, E., Ammons, S. M., Arriaga, P., Bailey, V. P., Barman, T., Bulger, J., Chilcote, J., Cotten, T., Doyon, R., Duchêne, G., ... Wolff, S. (2018). Dynamical Constraints on the HR 8799 Planets with GPI. Astronomical Journal, 156(5), Article 192. https://doi.org/10.3847/1538-3881/aae150

Wang, JJ, Graham, JR, Dawson, R, Fabrycky, D, De Rosa, RJ, Pueyo, L, Konopacky, Q, Macintosh, B, Marois, C, Chiang, E, Ammons, SM, Arriaga, P, Bailey, VP, Barman, T, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Esposito, TM, Fitzgerald, MP, Follette, KB, Gerard, BL, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Larkin, JE, Maire, J, Marchis, F, Marley, MS, Metchev, S, Millar-Blanchaer, MA, Nielsen, EL, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Rajan, A, Rameau, J, Rantakyrö, FT, Ruffio, JB, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S & Wolff, S 2018, 'Dynamical Constraints on the HR 8799 Planets with GPI', Astronomical Journal, vol. 156, no. 5, 192. https://doi.org/10.3847/1538-3881/aae150

@article{01f6a4b8f287448c8cae65251814d81b,

title = "Dynamical Constraints on the HR 8799 Planets with GPI",

abstract = "The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system's dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager, we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through N-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets' orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above 6 M Jup and 7 M Jup, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of 42 ± 5 Myr, we found the mass of planet b to be 5.8 ± 0.5 M Jup, and the masses of planets c, d, and e to be each.",

keywords = "astrometry, planetdisk interactions, planets and satellites: dynamical evolution and stability, planets and satellites: gaseous planets, stars: individual (HR 8799), techniques: high angular resolution",

author = "Wang, {Jason J.} and Graham, {James R.} and Rebekah Dawson and Daniel Fabrycky and {De Rosa}, {Robert J.} and Laurent Pueyo and Quinn Konopacky and Bruce Macintosh and Christian Marois and Eugene Chiang and Ammons, {S. Mark} and Pauline Arriaga and Bailey, {Vanessa P.} and Travis Barman and Joanna Bulger and Jeffrey Chilcote and Tara Cotten and Rene Doyon and Gaspard Duch{\^e}ne and Esposito, {Thomas M.} and Fitzgerald, {Michael P.} and Follette, {Katherine B.} and Gerard, {Benjamin L.} and Goodsell, {Stephen J.} and Greenbaum, {Alexandra Z.} and Pascale Hibon and Hung, {Li Wei} and Patrick Ingraham and Paul Kalas and Larkin, {James E.} and J{\'e}r{\^o}me Maire and Franck Marchis and Marley, {Mark S.} and Stanimir Metchev and Millar-Blanchaer, {Maxwell A.} and Nielsen, {Eric L.} and Rebecca Oppenheimer and David Palmer and Jennifer Patience and Marshall Perrin and Lisa Poyneer and Abhijith Rajan and Julien Rameau and Rantakyr{\"o}, {Fredrik T.} and Ruffio, {Jean Baptiste} and Dmitry Savransky and Schneider, {Adam C.} and Anand Sivaramakrishnan and Inseok Song and Remi Soummer and Sandrine Thomas and Wallace, {J. Kent} and Kimberly Ward-Duong and Sloane Wiktorowicz and Schuyler Wolff",

note = "Funding Information: Simulations in this paper made use of the REBOUND code, which can be downloaded freely at http://github.com/ hannorein/rebound. We thank Dan Tamayo for offering REBOUND tutorials and help with setting up the simulations. We also thank Eve Lee for helpful discussions on dynamics. J.J.W., J.R.G., P.K., and R.J.D.R. were supported in part by NSF AST-1518332, NASA NNX15AC89G, and NNX15AD95G. This work benefited from NASA{\textquoteright}s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA{\textquoteright}s Science Mission Directorate. R.I.D. gratefully acknowledges support from NASA XRP 80NSSC18K0355. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Funding Information: The GPI project has been supported by Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist{\'e}rio da Ci{\'e}ncia, Tecnologia e Inova{\c c}{\~a}o (Brazil), and Ministerio de Ciencia, Tecnolog{\'i}a e Innovaci{\'o}n Productiva (Argentina). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Publisher Copyright: {\textcopyright} 2018. The American Astronomical Society. All rights reserved.",

year = "2018",

month = nov,

doi = "10.3847/1538-3881/aae150",

language = "English (US)",

volume = "156",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "5",

}

TY - JOUR

T1 - Dynamical Constraints on the HR 8799 Planets with GPI

AU - Wang, Jason J.

AU - Graham, James R.

AU - Dawson, Rebekah

AU - Fabrycky, Daniel

AU - De Rosa, Robert J.

AU - Pueyo, Laurent

AU - Konopacky, Quinn

AU - Macintosh, Bruce

AU - Marois, Christian

AU - Chiang, Eugene

AU - Ammons, S. Mark

AU - Arriaga, Pauline

AU - Bailey, Vanessa P.

AU - Barman, Travis

AU - Bulger, Joanna

AU - Chilcote, Jeffrey

AU - Cotten, Tara

AU - Doyon, Rene

AU - Duchêne, Gaspard

AU - Esposito, Thomas M.

AU - Fitzgerald, Michael P.

AU - Follette, Katherine B.

AU - Gerard, Benjamin L.

AU - Goodsell, Stephen J.

AU - Greenbaum, Alexandra Z.

AU - Hibon, Pascale

AU - Hung, Li Wei

AU - Ingraham, Patrick

AU - Kalas, Paul

AU - Larkin, James E.

AU - Maire, Jérôme

AU - Marchis, Franck

AU - Marley, Mark S.

AU - Metchev, Stanimir

AU - Millar-Blanchaer, Maxwell A.

AU - Nielsen, Eric L.

AU - Oppenheimer, Rebecca

AU - Palmer, David

AU - Patience, Jennifer

AU - Perrin, Marshall

AU - Poyneer, Lisa

AU - Rajan, Abhijith

AU - Rameau, Julien

AU - Rantakyrö, Fredrik T.

AU - Ruffio, Jean Baptiste

AU - Savransky, Dmitry

AU - Schneider, Adam C.

AU - Sivaramakrishnan, Anand

AU - Song, Inseok

AU - Soummer, Remi

AU - Thomas, Sandrine

AU - Wallace, J. Kent

AU - Ward-Duong, Kimberly

AU - Wiktorowicz, Sloane

AU - Wolff, Schuyler

N1 - Funding Information: Simulations in this paper made use of the REBOUND code, which can be downloaded freely at http://github.com/ hannorein/rebound. We thank Dan Tamayo for offering REBOUND tutorials and help with setting up the simulations. We also thank Eve Lee for helpful discussions on dynamics. J.J.W., J.R.G., P.K., and R.J.D.R. were supported in part by NSF AST-1518332, NASA NNX15AC89G, and NNX15AD95G. This work benefited from NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate. R.I.D. gratefully acknowledges support from NASA XRP 80NSSC18K0355. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. Funding Information: The GPI project has been supported by Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciéncia, Tecnologia e Inovação (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Publisher Copyright: © 2018. The American Astronomical Society. All rights reserved.

PY - 2018/11

Y1 - 2018/11

N2 - The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system's dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager, we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through N-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets' orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above 6 M Jup and 7 M Jup, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of 42 ± 5 Myr, we found the mass of planet b to be 5.8 ± 0.5 M Jup, and the masses of planets c, d, and e to be each.

AB - The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system's dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager, we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through N-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets' orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above 6 M Jup and 7 M Jup, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of 42 ± 5 Myr, we found the mass of planet b to be 5.8 ± 0.5 M Jup, and the masses of planets c, d, and e to be each.

KW - astrometry

KW - planetdisk interactions

KW - planets and satellites: dynamical evolution and stability

KW - planets and satellites: gaseous planets

KW - stars: individual (HR 8799)

KW - techniques: high angular resolution

UR - http://www.scopus.com/inward/record.url?scp=85056639445&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85056639445&partnerID=8YFLogxK

U2 - 10.3847/1538-3881/aae150

DO - 10.3847/1538-3881/aae150

M3 - Article

AN - SCOPUS:85056639445

SN - 0004-6256

VL - 156

JO - Astronomical Journal

JF - Astronomical Journal

IS - 5

M1 - 192

ER -

Dynamical Constraints on the HR 8799 Planets with GPI

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