Precise masses in the WASP-47 system

Andrew Vanderburg; Juliette C. Becker; Lars A. Buchhave; Annelies Mortier; Eric Lopez; Luca Malavolta; Raphaëlle D. Haywood; David W. Latham; David Charbonneau; Mercedes López-Morales; Fred C. Adams; Aldo Stefano Bonomo; François Bouchy; Andrew Collier Cameron; Rosario Cosentino; Luca Di Fabrizio; Xavier Dumusque; Aldo Fiorenzano; Avet Harutyunyan; John Asher Johnson; Vania Lorenzi; Christophe Lovis; Michel Mayor; Giusi Micela; Emilio Molinari; Marco Pedani; Francesco Pepe; Giampaolo Piotto; David Phillips; Ken Rice; Dimitar Sasselov; Damien Ségransan; Alessandro Sozzetti; Stéphane Udry; Chris Watson

doi:10.3847/1538-3881/aa918b

Precise masses in the WASP-47 system

Andrew Vanderburg
, Juliette C. Becker
, Lars A. Buchhave
, Annelies Mortier
, Eric Lopez
, Luca Malavolta
, Raphaëlle D. Haywood
, David W. Latham
, David Charbonneau
, Mercedes López-Morales
, Fred C. Adams
, Aldo Stefano Bonomo
, François Bouchy
, Andrew Collier Cameron
, Rosario Cosentino
, Luca Di Fabrizio
, Xavier Dumusque
, Aldo Fiorenzano
, Avet Harutyunyan
, John Asher Johnson

Vania Lorenzi, Christophe Lovis, Michel Mayor, Giusi Micela, Emilio Molinari, Marco Pedani, Francesco Pepe, Giampaolo Piotto, David Phillips, Ken Rice, Dimitar Sasselov, Damien Ségransan, Alessandro Sozzetti, Stéphane Udry, Chris Watson

Physics and Astronomy

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

34 Citations (Scopus)

Abstract

We present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ∼19 hr orbit, and a Neptune in a ≈9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transit photometry, our mass measurements place strong constraints on the compositions of the two small planets. We find that, unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 M) and a radius (1.810 ± 0.027 R) that are inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10%, more than an order of magnitude larger than the geometric transit probability of 0.6%.

Original language	English
Article number	237
Journal	Astronomical Journal
Volume	154
Issue number	6
DOIs	https://doi.org/10.3847/1538-3881/aa918b
Publication status	Published - 17 Nov 2017

Bibliographical note

Funding Information:
This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant No. ACI-1053575. This research was done using resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science. We have made use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.

Funding Information:
This work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast and University of Edinburgh. This work was supported in part by the NASA Exoplanets Research Program.

Funding Information:
We thank Jason Eastman, Jonathan Irwin, Laura Kreidberg, Willie Torres, Lauren Weiss, and George Zhou for helpful conversations. We thank Josh Winn for helpful comments on the manuscript and the anonymous referee for a thoughtful report. A.V. and J.C.B. are supported by the NSF Graduate Research Fellowship, grant Nos. DGE 1144152 and DGE 1256260, respectively. This work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.W.L. acknowledges partial support from the from the TESS mission through a sub-award from the Massachusetts Institute of Technology to the Smithsonian Astrophysical Observatory. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under Grant Agreement No. 313014 (ETAEARTH). Parts of this work have been supported by NASA under grant Nos. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation.

Funding Information:
This paper includes data collected by the Kepler/K2 mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. Facilities: Kepler/K2, TNG (HARPS-N).

Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.

Keywords

Planets and satellites: Composition
Planets and satellites: Detection
Planets and satellites: Dynamical evolution and stability
Planets and satellites: Fundamental parameters
Planets and satellites: Gaseous planets
Planets and satellites: Interiors

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-3881/aa918b

Cite this

Vanderburg, A., Becker, J. C., Buchhave, L. A., Mortier, A., Lopez, E., Malavolta, L., Haywood, R. D., Latham, D. W., Charbonneau, D., López-Morales, M., Adams, F. C., Bonomo, A. S., Bouchy, F., Cameron, A. C., Cosentino, R., Di Fabrizio, L., Dumusque, X., Fiorenzano, A., Harutyunyan, A., ... Watson, C. (2017). Precise masses in the WASP-47 system. Astronomical Journal, 154(6), Article 237. https://doi.org/10.3847/1538-3881/aa918b

@article{24ec8c4500f842e6bd1f47d7764d3dc4,

title = "Precise masses in the WASP-47 system",

abstract = "We present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ∼19 hr orbit, and a Neptune in a ≈9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transit photometry, our mass measurements place strong constraints on the compositions of the two small planets. We find that, unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 M) and a radius (1.810 ± 0.027 R) that are inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10\%, more than an order of magnitude larger than the geometric transit probability of 0.6\%.",

keywords = "Planets and satellites: Composition, Planets and satellites: Detection, Planets and satellites: Dynamical evolution and stability, Planets and satellites: Fundamental parameters, Planets and satellites: Gaseous planets, Planets and satellites: Interiors",

author = "Andrew Vanderburg and Becker, \{Juliette C.\} and Buchhave, \{Lars A.\} and Annelies Mortier and Eric Lopez and Luca Malavolta and Haywood, \{Rapha{\"e}lle D.\} and Latham, \{David W.\} and David Charbonneau and Mercedes L{\'o}pez-Morales and Adams, \{Fred C.\} and Bonomo, \{Aldo Stefano\} and Fran{\c c}ois Bouchy and Cameron, \{Andrew Collier\} and Rosario Cosentino and \{Di Fabrizio\}, Luca and Xavier Dumusque and Aldo Fiorenzano and Avet Harutyunyan and Johnson, \{John Asher\} and Vania Lorenzi and Christophe Lovis and Michel Mayor and Giusi Micela and Emilio Molinari and Marco Pedani and Francesco Pepe and Giampaolo Piotto and David Phillips and Ken Rice and Dimitar Sasselov and Damien S{\'e}gransan and Alessandro Sozzetti and St{\'e}phane Udry and Chris Watson",

note = "Funding Information: This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant No. ACI-1053575. This research was done using resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy{\textquoteright}s Office of Science. We have made use of NASA{\textquoteright}s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding Information: This work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast and University of Edinburgh. This work was supported in part by the NASA Exoplanets Research Program. Funding Information: We thank Jason Eastman, Jonathan Irwin, Laura Kreidberg, Willie Torres, Lauren Weiss, and George Zhou for helpful conversations. We thank Josh Winn for helpful comments on the manuscript and the anonymous referee for a thoughtful report. A.V. and J.C.B. are supported by the NSF Graduate Research Fellowship, grant Nos. DGE 1144152 and DGE 1256260, respectively. This work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.W.L. acknowledges partial support from the from the TESS mission through a sub-award from the Massachusetts Institute of Technology to the Smithsonian Astrophysical Observatory. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under Grant Agreement No. 313014 (ETAEARTH). Parts of this work have been supported by NASA under grant Nos. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. Funding Information: This paper includes data collected by the Kepler/K2 mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. Facilities: Kepler/K2, TNG (HARPS-N). Publisher Copyright: {\textcopyright} 2017. The American Astronomical Society. All rights reserved.",

year = "2017",

month = nov,

day = "17",

doi = "10.3847/1538-3881/aa918b",

language = "English",

volume = "154",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "6",

}

Vanderburg, A, Becker, JC, Buchhave, LA, Mortier, A, Lopez, E, Malavolta, L, Haywood, RD, Latham, DW, Charbonneau, D, López-Morales, M, Adams, FC, Bonomo, AS, Bouchy, F, Cameron, AC, Cosentino, R, Di Fabrizio, L, Dumusque, X, Fiorenzano, A, Harutyunyan, A, Johnson, JA, Lorenzi, V, Lovis, C, Mayor, M, Micela, G, Molinari, E, Pedani, M, Pepe, F, Piotto, G, Phillips, D, Rice, K, Sasselov, D, Ségransan, D, Sozzetti, A, Udry, S & Watson, C 2017, 'Precise masses in the WASP-47 system', Astronomical Journal, vol. 154, no. 6, 237. https://doi.org/10.3847/1538-3881/aa918b

TY - JOUR

T1 - Precise masses in the WASP-47 system

AU - Vanderburg, Andrew

AU - Becker, Juliette C.

AU - Buchhave, Lars A.

AU - Mortier, Annelies

AU - Lopez, Eric

AU - Malavolta, Luca

AU - Haywood, Raphaëlle D.

AU - Latham, David W.

AU - Charbonneau, David

AU - López-Morales, Mercedes

AU - Adams, Fred C.

AU - Bonomo, Aldo Stefano

AU - Bouchy, François

AU - Cameron, Andrew Collier

AU - Cosentino, Rosario

AU - Di Fabrizio, Luca

AU - Dumusque, Xavier

AU - Fiorenzano, Aldo

AU - Harutyunyan, Avet

AU - Johnson, John Asher

AU - Lorenzi, Vania

AU - Lovis, Christophe

AU - Mayor, Michel

AU - Micela, Giusi

AU - Molinari, Emilio

AU - Pedani, Marco

AU - Pepe, Francesco

AU - Piotto, Giampaolo

AU - Phillips, David

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Ségransan, Damien

AU - Sozzetti, Alessandro

AU - Udry, Stéphane

AU - Watson, Chris

N1 - Funding Information: This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant No. ACI-1053575. This research was done using resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science. We have made use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding Information: This work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queens University Belfast and University of Edinburgh. This work was supported in part by the NASA Exoplanets Research Program. Funding Information: We thank Jason Eastman, Jonathan Irwin, Laura Kreidberg, Willie Torres, Lauren Weiss, and George Zhou for helpful conversations. We thank Josh Winn for helpful comments on the manuscript and the anonymous referee for a thoughtful report. A.V. and J.C.B. are supported by the NSF Graduate Research Fellowship, grant Nos. DGE 1144152 and DGE 1256260, respectively. This work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.W.L. acknowledges partial support from the from the TESS mission through a sub-award from the Massachusetts Institute of Technology to the Smithsonian Astrophysical Observatory. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under Grant Agreement No. 313014 (ETAEARTH). Parts of this work have been supported by NASA under grant Nos. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. Funding Information: This paper includes data collected by the Kepler/K2 mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. Facilities: Kepler/K2, TNG (HARPS-N). Publisher Copyright: © 2017. The American Astronomical Society. All rights reserved.

PY - 2017/11/17

Y1 - 2017/11/17

N2 - We present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ∼19 hr orbit, and a Neptune in a ≈9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transit photometry, our mass measurements place strong constraints on the compositions of the two small planets. We find that, unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 M) and a radius (1.810 ± 0.027 R) that are inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10%, more than an order of magnitude larger than the geometric transit probability of 0.6%.

AB - We present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ∼19 hr orbit, and a Neptune in a ≈9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transit photometry, our mass measurements place strong constraints on the compositions of the two small planets. We find that, unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 M) and a radius (1.810 ± 0.027 R) that are inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10%, more than an order of magnitude larger than the geometric transit probability of 0.6%.

KW - Planets and satellites: Composition

KW - Planets and satellites: Detection

KW - Planets and satellites: Dynamical evolution and stability

KW - Planets and satellites: Fundamental parameters

KW - Planets and satellites: Gaseous planets

KW - Planets and satellites: Interiors

UR - https://www.scopus.com/pages/publications/85038240451

U2 - 10.3847/1538-3881/aa918b

DO - 10.3847/1538-3881/aa918b

M3 - Article

AN - SCOPUS:85038240451

SN - 0004-6256

VL - 154

JO - Astronomical Journal

JF - Astronomical Journal

IS - 6

M1 - 237

ER -

Precise masses in the WASP-47 system

Abstract

Bibliographical note

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