K2-291b: a rocky super-Earth in a 2.2 day orbit

Molly R. Kosiarek; Sarah Blunt; Mercedes Lopez-Morales; Ian J. M. Crossfield; Evan Sinukoff; Erik A. Petigura; Erica J. Gonzales; Ennio Poretti; Luca Malavolta; Andrew W. Howard; Howard Isaacson; Raphaelle D. Haywood; David R. Ciardi; Makennah Bristow; Andrew Collier Cameron; David Charbonneau; Courtney D. Dressing; Pedro Figueird; 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; Francois 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 Segransan; Alessandro Sozzetti; Stephane 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 Lopez-Morales, Ian J. M. Crossfield, Evan Sinukoff, Erik A. Petigura, Erica J. Gonzales, Ennio Poretti, Luca Malavolta, Andrew W. Howard, Howard Isaacson, Raphaelle D. Haywood, David R. Ciardi, Makennah Bristow, Andrew Collier Cameron, David Charbonneau, Courtney D. Dressing, Pedro Figueird, 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, Francois 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 Segransan, Alessandro Sozzetti, Stephane Udry, Chris Watson

^*Corresponding author for this work

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Abstract

K2-291 is a solar-type star with a radius of R-* = 0.899 +/- 0.034 R-circle dot and mass of M-* = 0.934 +/- 0.038 M-circle dot. From the K2 C13 data, we found one super-Earth planet (R-p = 1.589(-0.072)(+0.095)R(circle plus)) 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-circle plus. 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 rho = 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
Number of pages	10
Journal	Astronomical Journal
Volume	157
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/aafe83
Publication status	Published - 13 Feb 2019

Keywords

Planets and satellites: composition
Planets and satellites: detection
Techniques: radial velocities

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Kosiarek_2019_AJ_rockysuper-Earth_FinalPubVersion
Copyright © 2019. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://doi.org/10.3847/1538-3881/aafe83
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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018
Jardine, M. M. (PI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Horne, K. D. (CoI) & Wood, K. (CoI)
Science & Technology Facilities Council
1/04/15 → 31/03/18
Project: Standard
EU FP7 Space ETAEARTH: ETAEARTH
Cameron, A. C. (PI)
European Commission
1/01/13 → 31/12/17
Project: Standard

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Kosiarek, M. R., Blunt, S., Lopez-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., Figueird, 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{5f7382e4a0254399a8d21709c7bccd73,

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-circle dot and mass of M-* = 0.934 +/- 0.038 M-circle dot. From the K2 C13 data, we found one super-Earth planet (R-p = 1.589(-0.072)(+0.095)R(circle plus)) 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-circle plus. 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 rho = 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 Lopez-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, {Raphaelle D.} and Ciardi, {David R.} and Makennah Bristow and Cameron, {Andrew Collier} and David Charbonneau and Dressing, {Courtney D.} and Pedro Figueird 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 Francois 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 Segransan and Alessandro Sozzetti and Stephane Udry and Chris Watson",

note = "A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. 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).",

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, Lopez-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, Figueird, 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, Segransan, 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 - Lopez-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, Raphaelle D.

AU - Ciardi, David R.

AU - Bristow, Makennah

AU - Cameron, Andrew Collier

AU - Charbonneau, David

AU - Dressing, Courtney D.

AU - Figueird, 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, Francois

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 - Segransan, Damien

AU - Sozzetti, Alessandro

AU - Udry, Stephane

AU - Watson, Chris

N1 - A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. 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).

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-circle dot and mass of M-* = 0.934 +/- 0.038 M-circle dot. From the K2 C13 data, we found one super-Earth planet (R-p = 1.589(-0.072)(+0.095)R(circle plus)) 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-circle plus. 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 rho = 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-circle dot and mass of M-* = 0.934 +/- 0.038 M-circle dot. From the K2 C13 data, we found one super-Earth planet (R-p = 1.589(-0.072)(+0.095)R(circle plus)) 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-circle plus. 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 rho = 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

U2 - 10.3847/1538-3881/aafe83

DO - 10.3847/1538-3881/aafe83

M3 - Article

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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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

EU FP7 Space ETAEARTH: ETAEARTH

Cite this