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

School of Physics and Astronomy

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

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 {}\oplus and a mass of 5.08 ± 0.41 M {}\oplus , 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
Pages (from-to)	107
Journal	Astronomical Journal
Volume	155
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aaa5b5
Publication status	Published - 9 Feb 2018

Keywords / Materials (for Non-textual outputs)

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

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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., Collier Cameron, A., 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), 107. https://doi.org/10.3847/1538-3881/aaa5b5

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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 \{\}\textbackslash{}oplus and a mass of 5.08 ± 0.41 M \{\}\textbackslash{}oplus , 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 \{Collier Cameron\}, Andrew 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",

year = "2018",

month = feb,

day = "9",

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

language = "English",

volume = "155",

pages = "107",

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, Collier Cameron, A, 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, pp. 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 - Collier Cameron, Andrew

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

PY - 2018/2/9

Y1 - 2018/2/9

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 {}\oplus and a mass of 5.08 ± 0.41 M {}\oplus , 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 {}\oplus and a mass of 5.08 ± 0.41 M {}\oplus , 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

KW - K2-141c

KW - planets and satellites: interiors

KW - stars: individual: K2-141

KW - techniques: photometric

KW - techniques: radial velocities

U2 - 10.3847/1538-3881/aaa5b5

DO - 10.3847/1538-3881/aaa5b5

M3 - Article

SN - 0004-6256

VL - 155

SP - 107

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

ER -

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

Abstract

Keywords / Materials (for Non-textual outputs)

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