Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems

Sophie C. Dubber; Annelies Mortier; Ken Rice; Chantanelle Nava; Luca Malavolta; Helen Giles; Adrien Coffinet; David Charbonneau; Andrew Vanderburg; Aldo S. Bonomo; Walter Boschin; Lars A. Buchhave; Andrew Collier Cameron; Rosario Cosentino; Xavier Dumusque; Adriano Ghedina; Avet Harutyunyan; Raphaëlle D. Haywood; David Latham; Mercedes López-Morales; Giusi Micela; Emilio Molinari; Francesco A. Pepe; David Phillips; Giampaolo Piotto; Ennio Poretti; Dimitar Sasselov; Alessandro Sozzetti; Stéphane Udry

doi:10.1093/mnras/stz2856

Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems

Sophie C. Dubber, Annelies Mortier, Ken Rice, Chantanelle Nava, Luca Malavolta, Helen Giles, Adrien Coffinet, David Charbonneau, Andrew Vanderburg, Aldo S. Bonomo, Walter Boschin, Lars A. Buchhave, Andrew Collier Cameron, Rosario Cosentino, Xavier Dumusque, Adriano Ghedina, Avet Harutyunyan, Raphaëlle D. Haywood, David Latham, Mercedes López-MoralesGiusi Micela, Emilio Molinari, Francesco A. Pepe, David Phillips, Giampaolo Piotto, Ennio Poretti, Dimitar Sasselov, Alessandro Sozzetti, Stéphane Udry

Physics and Astronomy

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

7 Citations (Scopus)

Abstract

We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5σ mass estimate of M_p = 109⁺₋³⁰₃₂ M⊕ and a radius of R_p = 9.49 ± 0.16 R⊕. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period P > 200 d that orbits a single star. We find that Kepler-103b has a mass of M_p,b = 11.7⁺₋⁴₄³¹₇₂ Mv and Kepler-103c has a mass of M_p,c = 58.5⁺₋¹¹₁₁²₄ M⊕. These are 2.5σ and 5σ results, respectively. With radii of R_p,b = 3.49⁺₋⁰₀⁰⁶₀₅ R⊕ and R_p,c = 5.45⁺₋⁰₀¹⁸₁₇ R⊕, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period P > 100 d. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii.

Original language	English
Pages (from-to)	5103-5121
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	490
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stz2856
Publication status	Published - 1 Dec 2019

Bibliographical note

Funding Information:
AM acknowledges support from Senior Kavli Institute Fellowships at the University of Cambridge. ACC acknowledges support from the Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. AV’s and RDH’s work was performed 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. LM acknowledges support from PLATO ASI-INAF agreement n.2015-019-R.1-2018. 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. This material is partly based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets

Funding Information:
This paper includes data collected by the Kepler 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.

Funding Information:
The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins 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), the University of St Andrews, Queen’s University Belfast, and the University of Edinburgh.

Funding Information:
This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, ht tps://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Keywords

Planets
Satellites: composition
Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1093/mnras/stz2856

Cite this

Dubber, S. C., Mortier, A., Rice, K., Nava, C., Malavolta, L., Giles, H., Coffinet, A., Charbonneau, D., Vanderburg, A., Bonomo, A. S., Boschin, W., Buchhave, L. A., Cameron, A. C., Cosentino, R., Dumusque, X., Ghedina, A., Harutyunyan, A., Haywood, R. D., Latham, D., ... Udry, S. (2019). Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems. Monthly Notices of the Royal Astronomical Society, 490(4), 5103-5121. https://doi.org/10.1093/mnras/stz2856

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title = "Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems",

abstract = "We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5σ mass estimate of Mp = 109+−3032 M⊕ and a radius of Rp = 9.49 ± 0.16 R⊕. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period P > 200 d that orbits a single star. We find that Kepler-103b has a mass of Mp,b = 11.7+−443172 Mv and Kepler-103c has a mass of Mp,c = 58.5+−111124 M⊕. These are 2.5σ and 5σ results, respectively. With radii of Rp,b = 3.49+−000605 R⊕ and Rp,c = 5.45+−001817 R⊕, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period P > 100 d. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii.",

keywords = "Planets, Satellites: composition, Techniques: photometric, Techniques: radial velocities, Techniques: spectroscopic",

author = "Dubber, {Sophie C.} and Annelies Mortier and Ken Rice and Chantanelle Nava and Luca Malavolta and Helen Giles and Adrien Coffinet and David Charbonneau and Andrew Vanderburg and Bonomo, {Aldo S.} and Walter Boschin and Buchhave, {Lars A.} and Cameron, {Andrew Collier} and Rosario Cosentino and Xavier Dumusque and Adriano Ghedina and Avet Harutyunyan and Haywood, {Rapha{\"e}lle D.} and David Latham and Mercedes L{\'o}pez-Morales and Giusi Micela and Emilio Molinari and Pepe, {Francesco A.} and David Phillips and Giampaolo Piotto and Ennio Poretti and Dimitar Sasselov and Alessandro Sozzetti and St{\'e}phane Udry",

note = "Funding Information: AM acknowledges support from Senior Kavli Institute Fellowships at the University of Cambridge. ACC acknowledges support from the Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. AV{\textquoteright}s and RDH{\textquoteright}s work was performed 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. LM acknowledges support from PLATO ASI-INAF agreement n.2015-019-R.1-2018. 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. This material is partly based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Funding Information: This paper includes data collected by the Kepler 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. Funding Information: The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins 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), the University of St Andrews, Queen{\textquoteright}s University Belfast, and the University of Edinburgh. Funding Information: This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, ht tps://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society",

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month = dec,

day = "1",

doi = "10.1093/mnras/stz2856",

language = "English",

volume = "490",

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Dubber, SC, Mortier, A, Rice, K, Nava, C, Malavolta, L, Giles, H, Coffinet, A, Charbonneau, D, Vanderburg, A, Bonomo, AS, Boschin, W, Buchhave, LA, Cameron, AC, Cosentino, R, Dumusque, X, Ghedina, A, Harutyunyan, A, Haywood, RD, Latham, D, López-Morales, M, Micela, G, Molinari, E, Pepe, FA, Phillips, D, Piotto, G, Poretti, E, Sasselov, D, Sozzetti, A & Udry, S 2019, 'Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems', Monthly Notices of the Royal Astronomical Society, vol. 490, no. 4, pp. 5103-5121. https://doi.org/10.1093/mnras/stz2856

TY - JOUR

T1 - Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems

AU - Dubber, Sophie C.

AU - Mortier, Annelies

AU - Rice, Ken

AU - Nava, Chantanelle

AU - Malavolta, Luca

AU - Giles, Helen

AU - Coffinet, Adrien

AU - Charbonneau, David

AU - Vanderburg, Andrew

AU - Bonomo, Aldo S.

AU - Boschin, Walter

AU - Buchhave, Lars A.

AU - Cameron, Andrew Collier

AU - Cosentino, Rosario

AU - Dumusque, Xavier

AU - Ghedina, Adriano

AU - Harutyunyan, Avet

AU - Haywood, Raphaëlle D.

AU - Latham, David

AU - López-Morales, Mercedes

AU - Micela, Giusi

AU - Molinari, Emilio

AU - Pepe, Francesco A.

AU - Phillips, David

AU - Piotto, Giampaolo

AU - Poretti, Ennio

AU - Sasselov, Dimitar

AU - Sozzetti, Alessandro

AU - Udry, Stéphane

N1 - Funding Information: AM acknowledges support from Senior Kavli Institute Fellowships at the University of Cambridge. ACC acknowledges support from the Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1. AV’s and RDH’s work was performed 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. LM acknowledges support from PLATO ASI-INAF agreement n.2015-019-R.1-2018. 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. This material is partly based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Funding Information: This paper includes data collected by the Kepler 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. Funding Information: The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins 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), the University of St Andrews, Queen’s University Belfast, and the University of Edinburgh. Funding Information: This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, ht tps://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

PY - 2019/12/1

Y1 - 2019/12/1

N2 - We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5σ mass estimate of Mp = 109+−3032 M⊕ and a radius of Rp = 9.49 ± 0.16 R⊕. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period P > 200 d that orbits a single star. We find that Kepler-103b has a mass of Mp,b = 11.7+−443172 Mv and Kepler-103c has a mass of Mp,c = 58.5+−111124 M⊕. These are 2.5σ and 5σ results, respectively. With radii of Rp,b = 3.49+−000605 R⊕ and Rp,c = 5.45+−001817 R⊕, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period P > 100 d. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii.

AB - We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5σ mass estimate of Mp = 109+−3032 M⊕ and a radius of Rp = 9.49 ± 0.16 R⊕. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period P > 200 d that orbits a single star. We find that Kepler-103b has a mass of Mp,b = 11.7+−443172 Mv and Kepler-103c has a mass of Mp,c = 58.5+−111124 M⊕. These are 2.5σ and 5σ results, respectively. With radii of Rp,b = 3.49+−000605 R⊕ and Rp,c = 5.45+−001817 R⊕, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period P > 100 d. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass-radius relation across the full range of exoplanet masses and radii.

KW - Planets

KW - Satellites: composition

KW - Techniques: photometric

KW - Techniques: radial velocities

KW - Techniques: spectroscopic

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U2 - 10.1093/mnras/stz2856

DO - 10.1093/mnras/stz2856

M3 - Article

AN - SCOPUS:85079628965

SN - 0035-8711

VL - 490

SP - 5103

EP - 5121

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems

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Keywords

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