An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Luca Malavolta; Andrew W. Mayo; Tom Louden; Vinesh M. Rajpaul; Aldo S. Bonomo; Lars A. Buchhave; Laura Kreidberg; Martti H. Kristiansen; Mercedes Lopez-Morales; Annelies Mortier; Andrew Vanderburg; Adrien Coffinet; David Ehrenreich; Christophe Lovis; Francois Bouchy; David Charbonneau; David R. Ciardi; Andrew Collier Cameron; Rosario Cosentino; Ian J.M. Crossfield; Mario Damasso; Courtney D. Dressing; Xavier Dumusque; Mark E. Everett; Pedro Figueira; Aldo F.M. Fiorenzano; Erica J. Gonzales; Raphaëlle D. Haywood; Avet Harutyunyan; Lea Hirsch; Steve B. Howell; John Asher Johnson; David W. Latham; Eric Lopez; Michel Mayor; Giusi Micela; Emilio Molinari; Valerio Nascimbeni; Francesco Pepe; David F. Phillips; Giampaolo Piotto; Ken Rice; Dimitar Sasselov; Damien Ségransan; Alessandro Sozzetti; Stéphane Udry; Chris Watson

doi:10.3847/1538-3881/aaa5b5

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Luca Malavolta, Andrew W. Mayo, Tom Louden, Vinesh M. Rajpaul, Aldo S. Bonomo, Lars A. Buchhave, Laura Kreidberg, Martti H. Kristiansen, Mercedes Lopez-Morales, Annelies Mortier, Andrew Vanderburg, Adrien Coffinet, David Ehrenreich, Christophe Lovis, Francois Bouchy, David Charbonneau, David R. Ciardi, Andrew Collier Cameron, Rosario Cosentino, Ian J.M. CrossfieldMario Damasso, Courtney D. Dressing, Xavier Dumusque, Mark E. Everett, Pedro Figueira, Aldo F.M. Fiorenzano, Erica J. Gonzales, Raphaëlle D. Haywood, Avet Harutyunyan, Lea Hirsch, Steve B. Howell, John Asher Johnson, David W. Latham, Eric Lopez, Michel Mayor, Giusi Micela, Emilio Molinari, Valerio Nascimbeni, Francesco Pepe, David F. Phillips, Giampaolo Piotto, Ken Rice, Dimitar Sasselov, Damien Ségransan, Alessandro Sozzetti, Stéphane Udry, Chris Watson

Physics and Astronomy

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

65 Citations (Scopus)

Abstract

Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

Original language	English
Article number	107
Journal	Astronomical Journal
Volume	155
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aaa5b5
Publication status	Published - Mar 2018

Bibliographical note

Funding Information:
V.M.R. acknowledges the Royal Astronomical Society for financial support.

Funding Information:
Parts of this work have been supported by NASA under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program.

Funding Information:
Some of the observations in the paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley.

Funding Information:
The research leading to these results received funding from the European Union Seventh Framework Programme (FP7/ 2007-2013) under grant agreement number 313014 (ETAEARTH).

Funding Information:
P.F. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through Investigador FCT contract of reference IF/01037/2013/CP1191/CT0001, and POPH/FSE (EC) by FEDER funding through the program “Programa Operacional de Factores de Competitividade—COMPETE.” P.F. further acknowledges support from FCT in the form of an exploratory project of reference IF/01037/2013/CP1191/ CT0001.

Funding Information:
This work has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). D.E., C.L., F.B., D.S., F.P., and S.U. acknowledge the financial support of the SNSF. D.E. acknowledges support from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427).

Funding Information:
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, Queen’s University Belfast and University of Edinburgh.

Funding Information:
This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Funding Information:
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.

Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.

Keywords

planetary systems
planets and satellites: composition
planets and satellites: individual (K2-141b, K2-141c)
planets and satellites: interiors
stars: individual (K2-141)
techniques: photometric
techniques: radial velocities

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-3881/aaa5b5

Cite this

Malavolta, L., Mayo, A. W., Louden, T., Rajpaul, V. M., Bonomo, A. S., Buchhave, L. A., Kreidberg, L., Kristiansen, M. H., Lopez-Morales, M., Mortier, A., Vanderburg, A., Coffinet, A., Ehrenreich, D., Lovis, C., Bouchy, F., Charbonneau, D., Ciardi, D. R., Cameron, A. C., Cosentino, R., ... Watson, C. (2018). An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141. Astronomical Journal, 155(3), Article 107. https://doi.org/10.3847/1538-3881/aaa5b5

@article{271420e8ed334057a43bf21cfece78f2,

title = "An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141",

abstract = "Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.",

keywords = "planetary systems, planets and satellites: composition, planets and satellites: individual (K2-141b, K2-141c), planets and satellites: interiors, stars: individual (K2-141), techniques: photometric, techniques: radial velocities",

author = "Luca Malavolta and Mayo, {Andrew W.} and Tom Louden and Rajpaul, {Vinesh M.} and Bonomo, {Aldo S.} and Buchhave, {Lars A.} and Laura Kreidberg and Kristiansen, {Martti H.} and Mercedes Lopez-Morales and Annelies Mortier and Andrew Vanderburg and Adrien Coffinet and David Ehrenreich and Christophe Lovis and Francois Bouchy and David Charbonneau and Ciardi, {David R.} and Cameron, {Andrew Collier} and Rosario Cosentino and Crossfield, {Ian J.M.} and Mario Damasso and Dressing, {Courtney D.} and Xavier Dumusque and Everett, {Mark E.} and Pedro Figueira and Fiorenzano, {Aldo F.M.} and Gonzales, {Erica J.} and Haywood, {Rapha{\"e}lle D.} and Avet Harutyunyan and Lea Hirsch and Howell, {Steve B.} and Johnson, {John Asher} and Latham, {David W.} and Eric Lopez and Michel Mayor and Giusi Micela and Emilio Molinari and Valerio Nascimbeni and Francesco Pepe and Phillips, {David F.} and Giampaolo Piotto 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: V.M.R. acknowledges the Royal Astronomical Society for financial support. Funding Information: Parts of this work have been supported by NASA under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. Funding Information: Some of the observations in the paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Funding Information: The research leading to these results received funding from the European Union Seventh Framework Programme (FP7/ 2007-2013) under grant agreement number 313014 (ETAEARTH). Funding Information: P.F. acknowledges support by Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia (FCT) through Investigador FCT contract of reference IF/01037/2013/CP1191/CT0001, and POPH/FSE (EC) by FEDER funding through the program “Programa Operacional de Factores de Competitividade—COMPETE.” P.F. further acknowledges support from FCT in the form of an exploratory project of reference IF/01037/2013/CP1191/ CT0001. Funding Information: This work has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). D.E., C.L., F.B., D.S., F.P., and S.U. acknowledge the financial support of the SNSF. D.E. acknowledges support from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). Funding Information: 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, Queen{\textquoteright}s University Belfast and University of Edinburgh. Funding Information: This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding Information: 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. Publisher Copyright: {\textcopyright} 2018. The American Astronomical Society. All rights reserved.",

year = "2018",

month = mar,

doi = "10.3847/1538-3881/aaa5b5",

language = "English",

volume = "155",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "3",

}

Malavolta, L, Mayo, AW, Louden, T, Rajpaul, VM, Bonomo, AS, Buchhave, LA, Kreidberg, L, Kristiansen, MH, Lopez-Morales, M, Mortier, A, Vanderburg, A, Coffinet, A, Ehrenreich, D, Lovis, C, Bouchy, F, Charbonneau, D, Ciardi, DR, Cameron, AC, Cosentino, R, Crossfield, IJM, Damasso, M, Dressing, CD, Dumusque, X, Everett, ME, Figueira, P, Fiorenzano, AFM, Gonzales, EJ, Haywood, RD, Harutyunyan, A, Hirsch, L, Howell, SB, Johnson, JA, Latham, DW, Lopez, E, Mayor, M, Micela, G, Molinari, E, Nascimbeni, V, Pepe, F, Phillips, DF, Piotto, G, Rice, K, Sasselov, D, Ségransan, D, Sozzetti, A, Udry, S & Watson, C 2018, 'An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141', Astronomical Journal, vol. 155, no. 3, 107. https://doi.org/10.3847/1538-3881/aaa5b5

TY - JOUR

T1 - An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

AU - Malavolta, Luca

AU - Mayo, Andrew W.

AU - Louden, Tom

AU - Rajpaul, Vinesh M.

AU - Bonomo, Aldo S.

AU - Buchhave, Lars A.

AU - Kreidberg, Laura

AU - Kristiansen, Martti H.

AU - Lopez-Morales, Mercedes

AU - Mortier, Annelies

AU - Vanderburg, Andrew

AU - Coffinet, Adrien

AU - Ehrenreich, David

AU - Lovis, Christophe

AU - Bouchy, Francois

AU - Charbonneau, David

AU - Ciardi, David R.

AU - Cameron, Andrew Collier

AU - Cosentino, Rosario

AU - Crossfield, Ian J.M.

AU - Damasso, Mario

AU - Dressing, Courtney D.

AU - Dumusque, Xavier

AU - Everett, Mark E.

AU - Figueira, Pedro

AU - Fiorenzano, Aldo F.M.

AU - Gonzales, Erica J.

AU - Haywood, Raphaëlle D.

AU - Harutyunyan, Avet

AU - Hirsch, Lea

AU - Howell, Steve B.

AU - Johnson, John Asher

AU - Latham, David W.

AU - Lopez, Eric

AU - Mayor, Michel

AU - Micela, Giusi

AU - Molinari, Emilio

AU - Nascimbeni, Valerio

AU - Pepe, Francesco

AU - Phillips, David F.

AU - Piotto, Giampaolo

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Ségransan, Damien

AU - Sozzetti, Alessandro

AU - Udry, Stéphane

AU - Watson, Chris

N1 - Funding Information: V.M.R. acknowledges the Royal Astronomical Society for financial support. Funding Information: Parts of this work have been supported by NASA under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. Funding Information: Some of the observations in the paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Funding Information: The research leading to these results received funding from the European Union Seventh Framework Programme (FP7/ 2007-2013) under grant agreement number 313014 (ETAEARTH). Funding Information: P.F. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through Investigador FCT contract of reference IF/01037/2013/CP1191/CT0001, and POPH/FSE (EC) by FEDER funding through the program “Programa Operacional de Factores de Competitividade—COMPETE.” P.F. further acknowledges support from FCT in the form of an exploratory project of reference IF/01037/2013/CP1191/ CT0001. Funding Information: This work has been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). D.E., C.L., F.B., D.S., F.P., and S.U. acknowledge the financial support of the SNSF. D.E. acknowledges support from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). Funding Information: 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, Queen’s University Belfast and University of Edinburgh. Funding Information: This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding Information: 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. Publisher Copyright: © 2018. The American Astronomical Society. All rights reserved.

PY - 2018/3

Y1 - 2018/3

N2 - Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

AB - Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

KW - planetary systems

KW - planets and satellites: composition

KW - planets and satellites: individual (K2-141b, K2-141c)

KW - planets and satellites: interiors

KW - stars: individual (K2-141)

KW - techniques: photometric

KW - techniques: radial velocities

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U2 - 10.3847/1538-3881/aaa5b5

DO - 10.3847/1538-3881/aaa5b5

M3 - Article

AN - SCOPUS:85043493669

SN - 0004-6256

VL - 155

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

M1 - 107

ER -

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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