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Independent validation of the temperate super-Earth HD 79211 b using HARPS-N

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dc.contributor.authorDiTomasso, Victoria
dc.contributor.authorNava, Chantanelle
dc.contributor.authorLópez-Morales, Mercedes
dc.contributor.authorBieryla, Allyson
dc.contributor.authorCloutier, Ryan
dc.contributor.authorMalavolta, Luca
dc.contributor.authorMortier, Annelies
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorStassun, Keivan G.
dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorBonomo, Aldo Stefano
dc.contributor.authorCharbonneau, David
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorCosentino, Rosario
dc.contributor.authorDamasso, Mario
dc.contributor.authorDumusque, Xavier
dc.contributor.authorMartínez Fiorenzano, A. F.
dc.contributor.authorGhedina, Adriano
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorHaywood, R. D.
dc.contributor.authorLatham, David
dc.contributor.authorMolinari, Emilio
dc.contributor.authorPepe, Francesco A.
dc.contributor.authorPinamonti, Matteo
dc.contributor.authorPoretti, Ennio
dc.contributor.authorRice, Ken
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorStalport, Manu
dc.contributor.authorUdry, Stéphane
dc.contributor.authorWatson, Christopher
dc.contributor.authorWilson, Thomas G.
dc.date.accessioned2023-01-20T16:30:07Z
dc.date.available2023-01-20T16:30:07Z
dc.date.issued2023-02-01
dc.identifier283034222
dc.identifierd41bf0d0-bd66-4c43-a4f1-12c0aedc9461
dc.identifier85146175246
dc.identifier000909863600001
dc.identifier.citationDiTomasso , 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 , Collier Cameron , A , Cosentino , R , Damasso , M , Dumusque , X , Martínez Fiorenzano , A F , Ghedina , A , Harutyunyan , A , Haywood , R D , Latham , D , Molinari , E , Pepe , F A , Pinamonti , M , Poretti , E , Rice , K , Sasselov , D , Stalport , M , Udry , S , Watson , C & Wilson , T G 2023 , ' Independent validation of the temperate super-Earth HD 79211 b using HARPS-N ' , Astronomical Journal , vol. 165 , no. 2 , 38 . https://doi.org/10.3847/1538-3881/ac9ccden
dc.identifier.issn0004-6256
dc.identifier.otherJisc: 829753
dc.identifier.otherpublisher-id: ajac9ccd
dc.identifier.othermanuscript: ac9ccd
dc.identifier.otherother: aas39658
dc.identifier.otherORCID: /0000-0002-8863-7828/work/127066041
dc.identifier.otherORCID: /0000-0001-8749-1962/work/127066173
dc.identifier.urihttps://hdl.handle.net/10023/26801
dc.descriptionFunding: 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.en
dc.description.abstractWe present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD 79210 and HD 79211, two M0V members of a gravitationally bound binary system. We detect a planet candidate with a period of 24.421−0.017+0.016 days around HD 79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES, and RVs spanning a total of 25 yr, we further refine the planet candidate parameters to P = 24.422 ± 0.014 days, K = 3.19 ± 0.27 m s−1, 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 HD 79211, nor do we find any planet candidate signals in HD 79210. 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.
dc.format.extent22
dc.format.extent4466927
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.subjectSolar Systemen
dc.subjectAstrobiologyen
dc.subjectExoplanetsen
dc.subjectRadial velocityen
dc.subjectM dwarf starsen
dc.subjectBinary starsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subjectMCCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleIndependent validation of the temperate super-Earth HD 79211 b using HARPS-Nen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doi10.3847/1538-3881/ac9ccd
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/R00824/1en
dc.identifier.grantnumberST/R003203/1en


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