Incidence of planet candidates in open clusters and a planet confirmation

dc.contributor.authorMartins, Bruno Leonardo Canto
dc.contributor.authorLeão, I. C.
dc.contributor.authorAlves, S.
dc.contributor.authorOliveira, G. Pereira de
dc.contributor.authorCortés, C.
dc.contributor.authorBrucalassi, A.
dc.contributor.authorMelo, C. H. F.
dc.contributor.authorFreitas, D. B. de
dc.contributor.authorPasquini, L.
dc.contributor.authorMedeiros, J. R. de
dc.date.accessioned2020-07-02T20:57:54Z
dc.date.available2020-07-02T20:57:54Z
dc.date.issued2018-12-10
dc.description.resumoContext. Detecting exoplanets in clusters of different ages is a powerful tool for understanding a number of open questions, such as how the occurrence rate of planets depends on stellar metallicity, on mass, or on stellar environment. Aims. We present the first results of our HARPS long-term radial velocity (RV) survey which aims to discover exoplanets around intermediate-mass (between ∼2 and 6 M ) evolved stars in open clusters. Methods. We selected 826 bona fide HARPS observations of 114 giants from an initial list of 29 open clusters and computed the halfpeak to peak variability of the HARPS RV measurements, namely ∆RV=2, for each target, to search for the best planet-host candidates. We also performed time series analyses for a few targets for which we have enough observations to search for orbital solutions. Results. Although we attempted to rule out the presence of binaries on the basis of previous surveys, we detected 14 new binary candidates in our sample, most of them identified from a comparison between HARPS and CORAVEL data. We also suggest 11 new planet-host candidates based on a relation between the stellar surface gravity and ∆RV=2. Ten of the candidates are less than 3 M , showing evidence of a low planet occurrence rate for massive stars. One of the planet-host candidates and one of the binary candidates show very clear RV periodic variations, allowing us to confirm the discovery of a new planet and to compute the orbital solution for the binary. The planet is IC 4651 9122b, with a minimum mass of m sin i = 6:3 MJ and a semimajor axis a = 2:0 AU. The binary companion is NGC 5822 201B, with a very low minimum mass of m sin i = 0:11 M and a semimajor axis a = 6:5 AU, which is comparable to the Jupiter distance to the Sun.pt_BR
dc.identifier.citationLEÃO, I. C.; MARTINS, Bruno Leonardo Canto; ALVES, S.; OLIVEIRA, G. Pereira de; CORTÉS, C.; BRUCALASSI, A.; MELO, C. H. F.; FREITAS, D. B. de; PASQUINI, L.; MEDEIROS, J. R. de. Incidence of planet candidates in open clusters and a planet confirmation. Astronomy & Astrophysics, [s.l.], v. 620, p. A139 (15p.), dez. 2018. ISSN 1432-0746 versão online. Disponível em: https://www.aanda.org/articles/aa/abs/2018/12/aa33123-18/aa33123-18.html. Acesso em 02 jul. 2020. http://dx.doi.org/10.1051/0004-6361/201833123. Reproduzido com permissão da Astronomy & Astrophysics, © ESO.pt_BR
dc.identifier.doihttp://dx.doi.org/10.1051/0004-6361/201833123
dc.identifier.issn0004-6361 (print), 1432-0746 (online)
dc.identifier.urihttps://repositorio.ufrn.br/jspui/handle/123456789/29405
dc.languageenpt_BR
dc.publisherEDPSCIENCEpt_BR
dc.subjectPlanetary systemspt_BR
dc.subjectOpen clusters and associations: generalpt_BR
dc.subjectStars: late-typept_BR
dc.subjectBinaries: spectroscopicpt_BR
dc.subjectTechniques: radial velocitiespt_BR
dc.titleIncidence of planet candidates in open clusters and a planet confirmationpt_BR
dc.typearticlept_BR

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