Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

A. S. Bonomo; A. Sozzetti; C. Lovis; L. Malavolta; K. Rice; L. A. Buchhave; D. Sasselov; A. C. Cameron; D. W. Latham; E. Molinari; F. Pepe; S. Udry; L. Affer; D. Charbonneau; R. Cosentino; C. D. Dressing; X. Dumusque; P. Figueira; A. F. M. Fiorenzano; S. Gettel; A. Harutyunyan; R. D. Haywood; K. Horne; M. Lopez-Morales; M. Mayor; G. Micela; F. Motalebi; V. Nascimbeni; D. F. Phillips; G. Piotto; D. Pollacco; D. Queloz; D. Ségransan; A. Szentgyorgyi; C. Watson

doi:10.1051/0004-6361/201424617

Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

A. S. Bonomo, A. Sozzetti, C. Lovis, L. Malavolta, K. Rice, L. A. Buchhave, D. Sasselov, A. C. Cameron, D. W. Latham, E. Molinari, F. Pepe, S. Udry, L. Affer, D. Charbonneau, R. Cosentino, C. D. Dressing, X. Dumusque, P. Figueira, A. F. M. Fiorenzano, S. GettelA. Harutyunyan, R. D. Haywood, K. Horne, M. Lopez-Morales, M. Mayor, G. Micela, F. Motalebi, V. Nascimbeni, D. F. Phillips, G. Piotto, D. Pollacco, D. Queloz, D. Ségransan, A. Szentgyorgyi, C. Watson

School of Physics and Astronomy

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

Abstract

We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp<3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 - containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance - is certainly of interest for scenarios of planet formation and evolution. This system does not follow thepreviously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación 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.Table 2 is available in electronic form at http://www.aanda.org

Original language	English
Journal	Astronomy & Astrophysics
Volume	572
DOIs	https://doi.org/10.1051/0004-6361/201424617
Publication status	Published - 1 Dec 2014

Keywords

planetary systems
stars: fundamental parameters
techniques: photometric
techniques: radial velocities
techniques: spectroscopic

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10.1051/0004-6361/201424617

aa24617-14Final published version, 5.37 MBLicence: Creative Commons: Attribution-NonCommercial-ShareAlike (CC BY-NC-SA)

Ken Rice
- wkmrroe.acuk
- School of Physics and Astronomy - Personal Chair in Computational Astrophysics
Person: Academic: Research Active

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Bonomo, A. S., Sozzetti, A., Lovis, C., Malavolta, L., Rice, K., Buchhave, L. A., Sasselov, D., Cameron, A. C., Latham, D. W., Molinari, E., Pepe, F., Udry, S., Affer, L., Charbonneau, D., Cosentino, R., Dressing, C. D., Dumusque, X., Figueira, P., Fiorenzano, A. F. M., ... Watson, C. (2014). Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion. Astronomy & Astrophysics, 572. https://doi.org/10.1051/0004-6361/201424617

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title = "Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion",

abstract = "We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp<3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 - containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance - is certainly of interest for scenarios of planet formation and evolution. This system does not follow thepreviously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundaci{\'o}n 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.Table 2 is available in electronic form at http://www.aanda.org",

keywords = "planetary systems, stars: fundamental parameters, techniques: photometric, techniques: radial velocities, techniques: spectroscopic",

author = "Bonomo, {A. S.} and A. Sozzetti and C. Lovis and L. Malavolta and K. Rice and Buchhave, {L. A.} and D. Sasselov and Cameron, {A. C.} and Latham, {D. W.} and E. Molinari and F. Pepe and S. Udry and L. Affer and D. Charbonneau and R. Cosentino and Dressing, {C. D.} and X. Dumusque and P. Figueira and Fiorenzano, {A. F. M.} and S. Gettel and A. Harutyunyan and Haywood, {R. D.} and K. Horne and M. Lopez-Morales and M. Mayor and G. Micela and F. Motalebi and V. Nascimbeni and Phillips, {D. F.} and G. Piotto and D. Pollacco and D. Queloz and D. S{\'e}gransan and A. Szentgyorgyi and C. Watson",

year = "2014",

month = dec,

day = "1",

doi = "10.1051/0004-6361/201424617",

language = "English",

volume = "572",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Bonomo, AS, Sozzetti, A, Lovis, C, Malavolta, L, Rice, K, Buchhave, LA, Sasselov, D, Cameron, AC, Latham, DW, Molinari, E, Pepe, F, Udry, S, Affer, L, Charbonneau, D, Cosentino, R, Dressing, CD, Dumusque, X, Figueira, P, Fiorenzano, AFM, Gettel, S, Harutyunyan, A, Haywood, RD, Horne, K, Lopez-Morales, M, Mayor, M, Micela, G, Motalebi, F, Nascimbeni, V, Phillips, DF, Piotto, G, Pollacco, D, Queloz, D, Ségransan, D, Szentgyorgyi, A & Watson, C 2014, 'Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion', Astronomy & Astrophysics, vol. 572. https://doi.org/10.1051/0004-6361/201424617

TY - JOUR

T1 - Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

AU - Bonomo, A. S.

AU - Sozzetti, A.

AU - Lovis, C.

AU - Malavolta, L.

AU - Rice, K.

AU - Buchhave, L. A.

AU - Sasselov, D.

AU - Cameron, A. C.

AU - Latham, D. W.

AU - Molinari, E.

AU - Pepe, F.

AU - Udry, S.

AU - Affer, L.

AU - Charbonneau, D.

AU - Cosentino, R.

AU - Dressing, C. D.

AU - Dumusque, X.

AU - Figueira, P.

AU - Fiorenzano, A. F. M.

AU - Gettel, S.

AU - Harutyunyan, A.

AU - Haywood, R. D.

AU - Horne, K.

AU - Lopez-Morales, M.

AU - Mayor, M.

AU - Micela, G.

AU - Motalebi, F.

AU - Nascimbeni, V.

AU - Phillips, D. F.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ségransan, D.

AU - Szentgyorgyi, A.

AU - Watson, C.

PY - 2014/12/1

Y1 - 2014/12/1

N2 - We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp<3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 - containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance - is certainly of interest for scenarios of planet formation and evolution. This system does not follow thepreviously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación 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.Table 2 is available in electronic form at http://www.aanda.org

AB - We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp<3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 - containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance - is certainly of interest for scenarios of planet formation and evolution. This system does not follow thepreviously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación 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.Table 2 is available in electronic form at http://www.aanda.org

KW - planetary systems

KW - stars: fundamental parameters

KW - techniques: photometric

KW - techniques: radial velocities

KW - techniques: spectroscopic

U2 - 10.1051/0004-6361/201424617

DO - 10.1051/0004-6361/201424617

M3 - Article

VL - 572

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

ER -

Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

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