K2-291b: A Rocky Super-Earth in a 2.2 day Orbit

Molly R. Kosiarek; Sarah Blunt; Mercedes López-Morales; Ian J.M. Crossfield; Evan Sinukoff; Erik A. Petigura; Erica J. Gonzales; Ennio Poretti; Luca Malavolta; Andrew W. Howard; Howard Isaacson; Raphaëlle D. Haywood; David R. Ciardi; Makennah Bristow; Andrew Collier Cameron; David Charbonneau; Courtney D. Dressing; Pedro Figueira; Benjamin J. Fulton; Bronwen J. Hardee; Lea A. Hirsch; David W. Latham; Annelies Mortier; Chantanelle Nava; Joshua E. Schlieder; Andrew Vanderburg; Lauren Weiss; Aldo S. Bonomo; François Bouchy; Lars A. Buchhave; Adrien Coffinet; Mario Damasso; Xavier Dumusque; Christophe Lovis; Michel Mayor; Giusi Micela; Emilio Molinari; Francesco Pepe; David Phillips; Giampaolo Piotto; Ken Rice; Dimitar Sasselov; Damien Ségransan; Alessandro Sozzetti; Stéphane Udry; Chris Watson

doi:10.3847/1538-3881/aafe83

K2-291b: A Rocky Super-Earth in a 2.2 day Orbit

Molly R. Kosiarek, Sarah Blunt, Mercedes López-Morales, Ian J.M. Crossfield, Evan Sinukoff, Erik A. Petigura, Erica J. Gonzales, Ennio Poretti, Luca Malavolta, Andrew W. Howard, Howard Isaacson, Raphaëlle D. Haywood, David R. Ciardi, Makennah Bristow, Andrew Collier Cameron, David Charbonneau, Courtney D. Dressing, Pedro Figueira, Benjamin J. Fulton, Bronwen J. HardeeLea A. Hirsch, David W. Latham, Annelies Mortier, Chantanelle Nava, Joshua E. Schlieder, Andrew Vanderburg, Lauren Weiss, Aldo S. Bonomo, François Bouchy, Lars A. Buchhave, Adrien Coffinet, Mario Damasso, Xavier Dumusque, Christophe Lovis, Michel Mayor, Giusi Micela, Emilio Molinari, Francesco Pepe, David 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

12 Citations (Scopus)

Abstract

K2-291 is a solar-type star with a radius of R _∗ = 0.899 ±0.034 R and mass of M _∗ = 0.934 ±0.038 M . From the K2 C13 data, we found one super-Earth planet (R _p = 1.589 _-0.072 ^+0.095 R _⊕ ) transiting this star on a short period orbit (P = 2.225177 _-6.8e-5 ^+6.6e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M _p = 6.49 ±1.16 M _⊕ . We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84 _-2.03 ^+2.50 g cm ^-3 , the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.

Original language	English
Article number	116
Journal	Astronomical Journal
Volume	157
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aafe83
Publication status	Published - 13 Feb 2019

Bibliographical note

Funding Information:
This material is based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. 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). 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. 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. This research has 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. This research has made use of the corner.py code by Dan Foreman-Mackey at github.com/dfm/corner.py. This publication received support from a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation.

Funding Information:
This research has made use of 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. A.W.H., I.J.M.C., and C.D.D. acknowledge support from the K2 Guest Observer Program. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant and observing support from NASA at Keck Observatory. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute (R.D.H., C.D.D., A.V.). Some of this work has been carried out within the framework of the NCCR PlanetS, supported by the Swiss National Science Foundation. M.R.K is supported by the NSF Graduate Research Fellowhsip, grant No. DGE 1339067. A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. C.A.W. acknowledges support by STFC grant ST/P000312/1. L.M. acknowledges the support by INAF/Frontiera through the Progetti Premiali funding scheme of the Italian Ministry of Education, University, and Research.

Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved..

Keywords

planets and satellites: composition
planets and satellites: detection
techniques: radial velocities

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-3881/aafe83

Cite this

Kosiarek, M. R., Blunt, S., López-Morales, M., Crossfield, I. J. M., Sinukoff, E., Petigura, E. A., Gonzales, E. J., Poretti, E., Malavolta, L., Howard, A. W., Isaacson, H., Haywood, R. D., Ciardi, D. R., Bristow, M., Cameron, A. C., Charbonneau, D., Dressing, C. D., Figueira, P., Fulton, B. J., ... Watson, C. (2019). K2-291b: A Rocky Super-Earth in a 2.2 day Orbit. Astronomical Journal, 157(3), Article 116. https://doi.org/10.3847/1538-3881/aafe83

@article{00f002006d6f411d81eaf7ad870e9ef8,

title = "K2-291b: A Rocky Super-Earth in a 2.2 day Orbit",

abstract = " K2-291 is a solar-type star with a radius of R ∗ = 0.899 ±0.034 R and mass of M ∗ = 0.934 ±0.038 M . From the K2 C13 data, we found one super-Earth planet (R p = 1.589 -0.072 +0.095 R ⊕ ) transiting this star on a short period orbit (P = 2.225177 -6.8e-5 +6.6e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M p = 6.49 ±1.16 M ⊕ . We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84 -2.03 +2.50 g cm -3 , the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.",

keywords = "planets and satellites: composition, planets and satellites: detection, techniques: radial velocities",

author = "Kosiarek, {Molly R.} and Sarah Blunt and Mercedes L{\'o}pez-Morales and Crossfield, {Ian J.M.} and Evan Sinukoff and Petigura, {Erik A.} and Gonzales, {Erica J.} and Ennio Poretti and Luca Malavolta and Howard, {Andrew W.} and Howard Isaacson and Haywood, {Rapha{\"e}lle D.} and Ciardi, {David R.} and Makennah Bristow and Cameron, {Andrew Collier} and David Charbonneau and Dressing, {Courtney D.} and Pedro Figueira and Fulton, {Benjamin J.} and Hardee, {Bronwen J.} and Hirsch, {Lea A.} and Latham, {David W.} and Annelies Mortier and Chantanelle Nava and Schlieder, {Joshua E.} and Andrew Vanderburg and Lauren Weiss and Bonomo, {Aldo S.} and Fran{\c c}ois Bouchy and Buchhave, {Lars A.} and Adrien Coffinet and Mario Damasso and Xavier Dumusque and Christophe Lovis and Michel Mayor and Giusi Micela and Emilio Molinari and Francesco Pepe and David Phillips 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: This material is based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. 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). 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. 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. This research has 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. This research has made use of the corner.py code by Dan Foreman-Mackey at github.com/dfm/corner.py. This publication received support from a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. Funding Information: This research has made use of 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. A.W.H., I.J.M.C., and C.D.D. acknowledge support from the K2 Guest Observer Program. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant and observing support from NASA at Keck Observatory. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute (R.D.H., C.D.D., A.V.). Some of this work has been carried out within the framework of the NCCR PlanetS, supported by the Swiss National Science Foundation. M.R.K is supported by the NSF Graduate Research Fellowhsip, grant No. DGE 1339067. A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. C.A.W. acknowledges support by STFC grant ST/P000312/1. L.M. acknowledges the support by INAF/Frontiera through the Progetti Premiali funding scheme of the Italian Ministry of Education, University, and Research. Publisher Copyright: {\textcopyright} 2019. The American Astronomical Society. All rights reserved..",

year = "2019",

month = feb,

day = "13",

doi = "10.3847/1538-3881/aafe83",

language = "English",

volume = "157",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "3",

}

Kosiarek, MR, Blunt, S, López-Morales, M, Crossfield, IJM, Sinukoff, E, Petigura, EA, Gonzales, EJ, Poretti, E, Malavolta, L, Howard, AW, Isaacson, H, Haywood, RD, Ciardi, DR, Bristow, M, Cameron, AC, Charbonneau, D, Dressing, CD, Figueira, P, Fulton, BJ, Hardee, BJ, Hirsch, LA, Latham, DW, Mortier, A, Nava, C, Schlieder, JE, Vanderburg, A, Weiss, L, Bonomo, AS, Bouchy, F, Buchhave, LA, Coffinet, A, Damasso, M, Dumusque, X, Lovis, C, Mayor, M, Micela, G, Molinari, E, Pepe, F, Phillips, D, Piotto, G, Rice, K, Sasselov, D, Ségransan, D, Sozzetti, A, Udry, S & Watson, C 2019, 'K2-291b: A Rocky Super-Earth in a 2.2 day Orbit', Astronomical Journal, vol. 157, no. 3, 116. https://doi.org/10.3847/1538-3881/aafe83

TY - JOUR

T1 - K2-291b

T2 - A Rocky Super-Earth in a 2.2 day Orbit

AU - Kosiarek, Molly R.

AU - Blunt, Sarah

AU - López-Morales, Mercedes

AU - Crossfield, Ian J.M.

AU - Sinukoff, Evan

AU - Petigura, Erik A.

AU - Gonzales, Erica J.

AU - Poretti, Ennio

AU - Malavolta, Luca

AU - Howard, Andrew W.

AU - Isaacson, Howard

AU - Haywood, Raphaëlle D.

AU - Ciardi, David R.

AU - Bristow, Makennah

AU - Cameron, Andrew Collier

AU - Charbonneau, David

AU - Dressing, Courtney D.

AU - Figueira, Pedro

AU - Fulton, Benjamin J.

AU - Hardee, Bronwen J.

AU - Hirsch, Lea A.

AU - Latham, David W.

AU - Mortier, Annelies

AU - Nava, Chantanelle

AU - Schlieder, Joshua E.

AU - Vanderburg, Andrew

AU - Weiss, Lauren

AU - Bonomo, Aldo S.

AU - Bouchy, François

AU - Buchhave, Lars A.

AU - Coffinet, Adrien

AU - Damasso, Mario

AU - Dumusque, Xavier

AU - Lovis, Christophe

AU - Mayor, Michel

AU - Micela, Giusi

AU - Molinari, Emilio

AU - Pepe, Francesco

AU - Phillips, David

AU - Piotto, Giampaolo

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Ségransan, Damien

AU - Sozzetti, Alessandro

AU - Udry, Stéphane

AU - Watson, Chris

N1 - Funding Information: This material is based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. 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). 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. 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. This research has 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. This research has made use of the corner.py code by Dan Foreman-Mackey at github.com/dfm/corner.py. This publication received support from a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. Funding Information: This research has made use of 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. A.W.H., I.J.M.C., and C.D.D. acknowledge support from the K2 Guest Observer Program. A.W.H. acknowledges support for our K2 team through a NASA Astrophysics Data Analysis Program grant and observing support from NASA at Keck Observatory. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute (R.D.H., C.D.D., A.V.). Some of this work has been carried out within the framework of the NCCR PlanetS, supported by the Swiss National Science Foundation. M.R.K is supported by the NSF Graduate Research Fellowhsip, grant No. DGE 1339067. A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. C.A.W. acknowledges support by STFC grant ST/P000312/1. L.M. acknowledges the support by INAF/Frontiera through the Progetti Premiali funding scheme of the Italian Ministry of Education, University, and Research. Publisher Copyright: © 2019. The American Astronomical Society. All rights reserved..

PY - 2019/2/13

Y1 - 2019/2/13

N2 - K2-291 is a solar-type star with a radius of R ∗ = 0.899 ±0.034 R and mass of M ∗ = 0.934 ±0.038 M . From the K2 C13 data, we found one super-Earth planet (R p = 1.589 -0.072 +0.095 R ⊕ ) transiting this star on a short period orbit (P = 2.225177 -6.8e-5 +6.6e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M p = 6.49 ±1.16 M ⊕ . We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84 -2.03 +2.50 g cm -3 , the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.

AB - K2-291 is a solar-type star with a radius of R ∗ = 0.899 ±0.034 R and mass of M ∗ = 0.934 ±0.038 M . From the K2 C13 data, we found one super-Earth planet (R p = 1.589 -0.072 +0.095 R ⊕ ) transiting this star on a short period orbit (P = 2.225177 -6.8e-5 +6.6e-5 days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M p = 6.49 ±1.16 M ⊕ . We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84 -2.03 +2.50 g cm -3 , the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.

KW - planets and satellites: composition

KW - planets and satellites: detection

KW - techniques: radial velocities

UR - http://www.scopus.com/inward/record.url?scp=85063463878&partnerID=8YFLogxK

U2 - 10.3847/1538-3881/aafe83

DO - 10.3847/1538-3881/aafe83

M3 - Article

AN - SCOPUS:85063463878

SN - 0004-6256

VL - 157

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

M1 - 116

ER -

K2-291b: A Rocky Super-Earth in a 2.2 day Orbit

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Keywords

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