Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

Victoria DiTomasso; Chantanelle Nava; Mercedes López-Morales; Allyson Bieryla; Ryan Cloutier; Luca Malavolta; Annelies Mortier; Lars A. Buchhave; Keivan G. Stassun; Alessandro Sozzetti; Aldo Stefano Bonomo; David Charbonneau; Andrew Collier Cameron; Rosario Cosentino; Mario Damasso; Xavier Dumusque; A. F. Martínez Fiorenzano; Adriano Ghedina; Avet Harutyunyan; R. D. Haywood; David Latham; Emilio Molinari; Francesco A. Pepe; Matteo Pinamonti; Ennio Poretti; Ken Rice; Dimitar Sasselov; Manu Stalport; Stéphane Udry; Christopher Watson; Thomas G. Wilson

doi:10.3847/1538-3881/ac9ccd

Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

Victoria DiTomasso^*, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. HaywoodDavid Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson

^*Corresponding author for this work

School of Physics and Astronomy

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

Abstract

We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of 24.421+0.016−0.017 days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to P=24.422±0.014 days, K=3.19±0.27 m/s, M sin i=10.6±1.2M⊕, and a=0.142±0.005 au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries.

Original language	English
Article number	38
Pages (from-to)	1-22
Number of pages	22
Journal	Astronomical Journal
Volume	165
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/ac9ccd
Publication status	Published - 6 Jan 2023

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astro-ph.EP

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DiTomasso, V., Nava, C., López-Morales, M., Bieryla, A., Cloutier, R., Malavolta, L., Mortier, A., Buchhave, L. A., Stassun, K. G., Sozzetti, A., Bonomo, A. S., Charbonneau, D., Cameron, A. C., Cosentino, R., Damasso, M., Dumusque, X., Fiorenzano, A. F. M., Ghedina, A., Harutyunyan, A., ... Wilson, T. G. (2023). Independent validation of the temperate Super-Earth HD79211 b using HARPS-N. Astronomical Journal, 165(2), 1-22. Article 38. https://doi.org/10.3847/1538-3881/ac9ccd

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title = "Independent validation of the temperate Super-Earth HD79211 b using HARPS-N",

abstract = "We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of 24.421+0.016−0.017 days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to P=24.422±0.014 days, K=3.19±0.27 m/s, M sin i=10.6±1.2M⊕, and a=0.142±0.005 au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries. ",

keywords = "astro-ph.EP",

author = "Victoria DiTomasso and Chantanelle Nava and Mercedes L{\'o}pez-Morales and Allyson Bieryla and Ryan Cloutier and Luca Malavolta and Annelies Mortier and Buchhave, \{Lars A.\} and Stassun, \{Keivan G.\} and Alessandro Sozzetti and Bonomo, \{Aldo Stefano\} and David Charbonneau and Cameron, \{Andrew Collier\} and Rosario Cosentino and Mario Damasso and Xavier Dumusque and Fiorenzano, \{A. F. Mart{\'i}nez\} and Adriano Ghedina and Avet Harutyunyan and Haywood, \{R. D.\} and David Latham and Emilio Molinari and Pepe, \{Francesco A.\} and Matteo Pinamonti and Ennio Poretti and Ken Rice and Dimitar Sasselov and Manu Stalport and St{\'e}phane Udry and Christopher Watson and Wilson, \{Thomas G.\}",

note = "Accepted for publication in AJ, 29 pages, 17 figures Funding Information: This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1745303. 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), the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. Parts of this work have been supported by the National Aeronautics and Space Administration under grant No. NNX17AB59G, issued through the Exoplanets Research Program. Parts of this work have been supported by the Brinson Foundation. R.D.H. is funded by the UK Science and Technology Facilities Council (STFC)'s Ernest Rutherford Fellowship (grant No. ST/V004735/1). T.G.W and A.C.C acknowledge support from STFC consolidated grant Nos. ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. 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, https://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} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = jan,

day = "6",

doi = "10.3847/1538-3881/ac9ccd",

language = "English",

volume = "165",

pages = "1--22",

journal = "Astronomical Journal",

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DiTomasso, V, Nava, C, López-Morales, M, Bieryla, A, Cloutier, R, Malavolta, L, Mortier, A, Buchhave, LA, Stassun, KG, Sozzetti, A, Bonomo, AS, Charbonneau, D, Cameron, AC, Cosentino, R, Damasso, M, Dumusque, X, Fiorenzano, AFM, Ghedina, A, Harutyunyan, A, Haywood, RD, Latham, D, Molinari, E, Pepe, FA, Pinamonti, M, Poretti, E, Rice, K, Sasselov, D, Stalport, M, Udry, S, Watson, C & Wilson, TG 2023, 'Independent validation of the temperate Super-Earth HD79211 b using HARPS-N', Astronomical Journal, vol. 165, no. 2, 38, pp. 1-22. https://doi.org/10.3847/1538-3881/ac9ccd

TY - JOUR

T1 - Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

AU - DiTomasso, Victoria

AU - Nava, Chantanelle

AU - López-Morales, Mercedes

AU - Bieryla, Allyson

AU - Cloutier, Ryan

AU - Malavolta, Luca

AU - Mortier, Annelies

AU - Buchhave, Lars A.

AU - Stassun, Keivan G.

AU - Sozzetti, Alessandro

AU - Bonomo, Aldo Stefano

AU - Charbonneau, David

AU - Cameron, Andrew Collier

AU - Cosentino, Rosario

AU - Damasso, Mario

AU - Dumusque, Xavier

AU - Fiorenzano, A. F. Martínez

AU - Ghedina, Adriano

AU - Harutyunyan, Avet

AU - Haywood, R. D.

AU - Latham, David

AU - Molinari, Emilio

AU - Pepe, Francesco A.

AU - Pinamonti, Matteo

AU - Poretti, Ennio

AU - Rice, Ken

AU - Sasselov, Dimitar

AU - Stalport, Manu

AU - Udry, Stéphane

AU - Watson, Christopher

AU - Wilson, Thomas G.

N1 - Accepted for publication in AJ, 29 pages, 17 figures Funding Information: This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1745303. 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), the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. Parts of this work have been supported by the National Aeronautics and Space Administration under grant No. NNX17AB59G, issued through the Exoplanets Research Program. Parts of this work have been supported by the Brinson Foundation. R.D.H. is funded by the UK Science and Technology Facilities Council (STFC)'s Ernest Rutherford Fellowship (grant No. ST/V004735/1). T.G.W and A.C.C acknowledge support from STFC consolidated grant Nos. ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. 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, https://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: © 2023. The Author(s). Published by the American Astronomical Society.

PY - 2023/1/6

Y1 - 2023/1/6

N2 - We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of 24.421+0.016−0.017 days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to P=24.422±0.014 days, K=3.19±0.27 m/s, M sin i=10.6±1.2M⊕, and a=0.142±0.005 au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries.

AB - We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of 24.421+0.016−0.017 days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to P=24.422±0.014 days, K=3.19±0.27 m/s, M sin i=10.6±1.2M⊕, and a=0.142±0.005 au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries.

KW - astro-ph.EP

U2 - 10.3847/1538-3881/ac9ccd

DO - 10.3847/1538-3881/ac9ccd

M3 - Article

SN - 0004-6256

VL - 165

SP - 1

EP - 22

JO - Astronomical Journal

JF - Astronomical Journal

IS - 2

M1 - 38

ER -

Independent validation of the temperate Super-Earth HD79211 b using HARPS-N

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