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dc.contributor.authorJones, H.R.A.
dc.contributor.authorButler, R.P.
dc.contributor.authorTinney, C.G.
dc.contributor.authorO'Toole, S.
dc.contributor.authorWittenmyer, R.
dc.contributor.authorHenry, G.W.
dc.contributor.authorMeschiari, S.
dc.contributor.authorVogt, S.
dc.contributor.authorRivera, E.
dc.contributor.authorLaughlin, G.
dc.contributor.authorCarter, B.D.
dc.contributor.authorBailey, J.
dc.contributor.authorJenkins, J.S.
dc.date.accessioned2010-10-27T10:04:49Z
dc.date.available2010-10-27T10:04:49Z
dc.date.issued2010
dc.identifier.citationJones , H R A , Butler , R P , Tinney , C G , O'Toole , S , Wittenmyer , R , Henry , G W , Meschiari , S , Vogt , S , Rivera , E , Laughlin , G , Carter , B D , Bailey , J & Jenkins , J S 2010 , ' A long-period planet orbiting a nearby Sun-like star ' , Monthly Notices of the Royal Astronomical Society , vol. 403 , no. 4 , pp. 1703-1713 . https://doi.org/10.1111/j.1365-2966.2009.16232.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 180779
dc.identifier.otherPURE UUID: b918444f-968e-40b1-9652-47ffe5aa52ad
dc.identifier.otherdspace: 2299/4929
dc.identifier.otherScopus: 77953055900
dc.identifier.urihttp://hdl.handle.net/2299/4929
dc.descriptionOriginal article can be found at: http://www3.interscience.wiley.com/ Copyright Royal Astronomical Society
dc.description.abstractThe Doppler wobble induced by the extra-solar planet HD 134987b was first detected by data from the Keck Telescope nearly a decade ago, and was subsequently confirmed by data from the Anglo-Australian Telescope (AAT). However, as more data have been acquired for this star over the years since, the quality of a single Keplerian fit to that data has been getting steadily worse. The best-fitting single Keplerian to the 138 Keck and AAT observations now in hand has an root-mean-square (rms) scatter of 6.6 m s−1. This is significantly in excess of both the instrumental precision achieved by both the Keck and Anglo-Australian Planet Searches for stars of this magnitude, and of the jitter expected for a star with the properties of HD134987. However, a double Keplerian (i.e. dual planet) fit delivers a significantly reduced rms of 3.3 m s−1. The best-fitting double planet solution has minimum planet masses of 1.59 and 0.82 1.59 ± 0.02MJup, orbital periods of 258 and 5000 d, and eccentricities of 0.23 and 0.12, respectively. We find evidence that activity-induced jitter is a significant factor in our fits and do not find evidence for asteroseismological p modes. We also present seven years of photometry at a typical precision of 0.003 mag with the T8 0.8 m automatic photometric telescope at Fairborn observatory. These observations do not detect photometric variability and support the inference that the detected radial-velocity periods are due to planetary mass companions rather than due to photospheric spots and plages.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.titleA long-period planet orbiting a nearby Sun-like staren
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionScience & Technology Research Institute
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=77953055900&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2010
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2009.16232.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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