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dc.contributor.authorGettel, Sara
dc.contributor.authorCharbonneau, David
dc.contributor.authorDressing, Courtney D.
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorDumusque, Xavier
dc.contributor.authorVanderburg, Andrew
dc.contributor.authorBonomo, Aldo S.
dc.contributor.authorMalavolta, Luca
dc.contributor.authorPepe, Francesco
dc.contributor.authorCameron, Andrew Collier
dc.contributor.authorLatham, David W.
dc.contributor.authorUdry, Stephane
dc.contributor.authorMarcy, Geoffrey W.
dc.contributor.authorIsaacson, Howard
dc.contributor.authorHoward, Andrew W.
dc.contributor.authorDavies, Guy R.
dc.contributor.authorAguirre, Victor Silva
dc.contributor.authorKjeldsen, Hans
dc.contributor.authorBedding, Timothy R.
dc.contributor.authorLopez, Eric
dc.contributor.authorAffer, Laura
dc.contributor.authorCosentino, Rosario
dc.contributor.authorFigueira, Pedro
dc.contributor.authorFiorenzano, Aldo F. M.
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorJohnson, John Asher
dc.contributor.authorLopez-Morales, Mercedes
dc.contributor.authorLovis, Christophe
dc.contributor.authorMayor, Michel
dc.contributor.authorMicela, Giusi
dc.contributor.authorMolinari, Emilio
dc.contributor.authorMotalebi, Fatemeh
dc.contributor.authorPhillips, David F.
dc.contributor.authorPiotto, Giampaolo
dc.contributor.authorQueloz, Didier
dc.contributor.authorRice, Ken
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorSegransan, Damien
dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorWatson, Chris
dc.contributor.authorBasu, Sarbani
dc.contributor.authorCampante, Tiago L.
dc.contributor.authorChristensen-Dalsgaard, Jorgen
dc.contributor.authorKawaler, Steven D.
dc.contributor.authorMetcalfe, Travis S.
dc.contributor.authorHandberg, Rasmus
dc.contributor.authorLund, Mikkel N.
dc.contributor.authorLundkvist, Mia S.
dc.contributor.authorHuber, Daniel
dc.contributor.authorChaplin, William J.
dc.date.accessioned2016-01-30T00:12:00Z
dc.date.available2016-01-30T00:12:00Z
dc.date.issued2016-01-14
dc.identifier.citationGettel , S , Charbonneau , D , Dressing , C D , Buchhave , L A , Dumusque , X , Vanderburg , A , Bonomo , A S , Malavolta , L , Pepe , F , Cameron , A C , Latham , D W , Udry , S , Marcy , G W , Isaacson , H , Howard , A W , Davies , G R , Aguirre , V S , Kjeldsen , H , Bedding , T R , Lopez , E , Affer , L , Cosentino , R , Figueira , P , Fiorenzano , A F M , Harutyunyan , A , Johnson , J A , Lopez-Morales , M , Lovis , C , Mayor , M , Micela , G , Molinari , E , Motalebi , F , Phillips , D F , Piotto , G , Queloz , D , Rice , K , Sasselov , D , Segransan , D , Sozzetti , A , Watson , C , Basu , S , Campante , T L , Christensen-Dalsgaard , J , Kawaler , S D , Metcalfe , T S , Handberg , R , Lund , M N , Lundkvist , M S , Huber , D & Chaplin , W J 2016 , ' The Kepler-454 system : A small, not-rocky inner planet, a Jovian world, and a distant companion ' , Astrophysical Journal , vol. 816 , no. 2 , 95 . https://doi.org/10.3847/0004-637X/816/2/95en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 240605984
dc.identifier.otherPURE UUID: c32a828b-6b08-4029-a6b6-654d0b59c61d
dc.identifier.otherArXiv: http://arxiv.org/abs/1511.09097v1
dc.identifier.otherScopus: 84954537907
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531521
dc.identifier.otherWOS: 000368238500047
dc.identifier.urihttp://hdl.handle.net/10023/8100
dc.description.abstractKepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like starthat hosts a transiting planet candidate in a 10.6 d orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i <2.4 km s-1. We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be 1.028+0:04-0:03 M_Sun, the radius to be 1.066 +/- 0.012 R_Sun and the age to be 5.25+1:41-1:39 Gyr. We estimate the radius of the 10.6 d planet as 2.37 +/- 0.13 R_Earth. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at Keck Observatory, we measure the mass of this planet to be 6.8 +/- 1.4M_Earth. We also detect two additional non-transiting companions, a planet with a minimum mass of 4.46 +/- 0.12 M_J in a nearly circular 524 d orbit and a massive companion with a period >10 years and mass >12.1M_J . The twelve exoplanets with radii <2.7 R_Earth and precise mass measurements appear to fall into two populations, with those <1.6 R_Earth following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 +/- 0.73 g cm-3, Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016. The American Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://dx.doi.org/10.3847/0004-637X/816/2/95en
dc.subjectastro-ph.EPen
dc.subjectastro-ph.SRen
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellitesen
dc.subjectCompositionen
dc.subjectStars: individual (KOI-273 & KIC 3102384)en
dc.subjectAsteroseismologyen
dc.subjectTechniques: radial velocitiesen
dc.subjectQB Astronomyen
dc.subjectDASen
dc.subject.lccQBen
dc.titleThe Kepler-454 system : A small, not-rocky inner planet, a Jovian world, and a distant companionen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/816/2/95
dc.description.statusPeer revieweden


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