J/A+A/666/A187ivo://CDS.VizieR/J/A+A/666/A187doi:10.26093/cds/vizier.36660187CDSDamasso M.Perger M.Almenara J.M.Nardiello D.Perez-Torres M.,Sozzetti A.Hara N.C.Quirrenbach A.Bonfils X.Zapatero Osorio M.R.,Astudillo-Defru N.Gonzalez Hernandez J.I.Suarez Mascareno A.,Amado P.J.Forveille T.Lillo-Box J.Alibert Y.Caballero J.A.,Cifuentes C.Delfosse X.Figueira P.Galadi-Enriquez D.Hatzes A.P.,Henning T.Kaminski A.Mayor M.Murgas F.Montes D.Pinamonti M.,Reiners A.Ribas I.Bejar V.J.S.Schweitzer A.Zechmeister M.2023-03-02T10:59:48Z2022-10-28T09:22:10ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsexoplanetsradial-velocityphotometryvisible-astronomyStatistical analyses based on Kepler data show that most of the early-type M dwarfs host multi-planet systems consisting of Earth to sub-Neptune sized planets with orbital periods up to ~250 days, and that at least one such planet is likely located within the habitable zone. M dwarfs are therefore primary targets to search for potentially habitable planets in the solar neighbourhood. We investigated the presence of planetary companions around the nearby (7.6pc) and bright (V=9mag) early-type M dwarf Gl 514, analysing 540 radial velocities collected over nearly 25 years with the HIRES, HARPS, and CARMENES spectrographs. The data are affected by time-correlated signals at the level of 2-3m/s due to stellar activity, that we filtered out testing three different models based on Gaussian process regression. As a sanity cross-check, we repeated the analyses using HARPS radial velocities extracted with three different algorithms. We used HIRES radial velocities and Hipparcos-Gaia astrometry to put constraints on the presence of long-period companions, and we analysed TESS photometric data. We found strong evidence that Gl~514 hosts a super-Earth on a likely eccentric orbit, residing in the conservative habitable zone for nearly 34% of its orbital period. The planet Gl 514 b has minimum mass m_b_sini_b_=5.2+/-0.9M_{sun}_, orbital period P_b_=140.43+/-0.41 days, and eccentricity e_b_=0.45^+0.15^_-0.14_. No evidence for transits is found in the TESS light curve. There is no evidence for a longer period companion in the radial velocities and, based on astrometry, we can rule out a ~0.2M_{Jup}_ planet at a distance of ~3-10au, and massive giant planets/brown dwarfs out to several tens of au. We discuss the possible presence of a second low-mass companion at a shorter distance from the host than Gl 514 b. Gl 514 b represents an interesting science case to study the habitability of planets on eccentric orbits. We advocate for additional spectroscopic follow-up to get more accurate and precise planetary parameters. Further follow-up is also needed to investigate sub m/s and shorter period signals.2022A&A...666A.187Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/666/A187CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/636/A74 : HARPS radial velocity database (Trifonov+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/666/A187https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/666/A187http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/666/A187https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/666/A187https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/666/A187http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/666/A187GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/666/A187/tablea1HARPS RVs extracted with TERRArecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEpochs of the observations (BJD-2450000)dtime.epochdoubleRVRelative radial velocitym/sphys.veloc;pos.heliocentricfloate_RVRadial velocity uncertaintym/sstat.errorfloatJ/A+A/666/A187/tablea2HARPS RVs extracted with NAIRArecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEpochs of the observations (BJD-2450000)dtime.epochdoubleRVRadial velocitym/sphys.veloc;pos.heliocentricdoublee_RVRadial velocity uncertaintym/sstat.errorfloatJ/A+A/666/A187/tablea3Activity diagnostics from HARPS spectraH-alphaH-alpha activity indexphot.color;em.opt.V;em.line.HalphadoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEpochs of the observations (BJD-2450000)dtime.epochdoubleFWHMCCF FWHMkm/sspect.line.widthfloate_FWHMCCF FWHM uncertaintieskm/sstat.error;phys.angSizefloate_H-alphaH-alpha activity index errorsstat.error;spect.linedoubleCaIIHKCaIIHK activity indexspect.indexfloate_CaIIHKCaIIHK activity index errorsstat.errorfloatNaINaI activity indexmeta.code;spect.indexdoublee_NaINaI activity index errorsstat.errordoubleJ/A+A/666/A187/tablea4CARMENES-VIS RVsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEpochs of the observations (BJD-2450000)dtime.epochdoubleRVRelative radial velocitym/sphys.veloc;pos.heliocentricfloate_RVRadial velocity uncertaintym/sstat.errorfloatJ/A+A/666/A187/tablea5Activity diagnostics from CARMENES spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEpochs of the observations (BJD-2450000)dtime.epochdoubleCa-IRTCalcium infrared triplet indexspect.indexdoublee_Ca-IRTCalcium infrared triplet index errorstat.errordoubleNaDSodium doublet indexmeta.code;spect.indexdoublee_NaDSodium doublet index errorstat.errordoubledLWDifferential line widthspect.line.widthfloate_dLWDifferential line width errorstat.errorfloatCRXChromatic indexspect.indexfloate_CRXChromatic index errorstat.errorfloat