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dc.contributor.authorDubber, Sophie C.
dc.contributor.authorMortier, Annelies
dc.contributor.authorRice, Ken
dc.contributor.authorNava, Chantanelle
dc.contributor.authorMalavolta, Luca
dc.contributor.authorGiles, Helen
dc.contributor.authorCoffinet, Adrien
dc.contributor.authorCharbonneau, David
dc.contributor.authorVanderburg, Andrew
dc.contributor.authorBonomo, Aldo S.
dc.contributor.authorBoschin, Walter
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorCameron, Andrew Collier
dc.contributor.authorCosentino, Rosario
dc.contributor.authorDumusque, Xavier
dc.contributor.authorGhedina, Adriano
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorHaywood, Raphaelle D.
dc.contributor.authorLatham, David
dc.contributor.authorLópez-Morales, Mercedes
dc.contributor.authorMicela, Giusi
dc.contributor.authorMolinari, Emilio
dc.contributor.authorPepe, Francesco A.
dc.contributor.authorPhillips, David
dc.contributor.authorPiotto, Giampaolo
dc.contributor.authorPoretti, Ennio
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorUdry, Stéphane
dc.date.accessioned2019-12-20T11:30:02Z
dc.date.available2019-12-20T11:30:02Z
dc.date.issued2019-12
dc.identifier.citationDubber , S C , Mortier , A , Rice , K , Nava , C , Malavolta , L , Giles , H , Coffinet , A , Charbonneau , D , Vanderburg , A , Bonomo , A S , Boschin , W , Buchhave , L A , Cameron , A C , Cosentino , R , Dumusque , X , Ghedina , A , Harutyunyan , A , Haywood , R D , Latham , D , López-Morales , M , Micela , G , Molinari , E , Pepe , F A , Phillips , D , Piotto , G , Poretti , E , Sasselov , D , Sozzetti , A & Udry , S 2019 , ' Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems ' , Monthly Notices of the Royal Astronomical Society , vol. 490 , no. 4 , pp. 5103–5121 . https://doi.org/10.1093/mnras/stz2856en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 264574534
dc.identifier.otherPURE UUID: dfdb2751-dc3a-4611-9425-1eeec4ae7cf4
dc.identifier.otherArXiv: http://arxiv.org/abs/1910.03518v1
dc.identifier.otherORCID: /0000-0002-8863-7828/work/66398286
dc.identifier.otherScopus: 85079628965
dc.identifier.otherWOS: 000504000300048
dc.identifier.urihttp://hdl.handle.net/10023/19175
dc.descriptionFunding: Senior Kavli Institute Fellowships at the University of Cambridge (AM); UK Science & Technology Facilities Council (STFC) consolidated grant number ST/R000824/1 (ACC).en
dc.description.abstractWe present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely populated category of exoplanets. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass. For PH-2b we recover a 3.5σ mass estimate of Mp=109+30−32 M⊕ and a radius of Rp = 9.49 ± 0.16 R⊕. This means that PH-2b has a Saturn-like bulk density and is the only planet of this type with an orbital period P > 200 d that orbits a single star. We find that Kepler-103b has a mass of Mp,b=11.7+4.31−4.72 M⊕ and Kepler-103c has a mass of Mp,c=58.5+11.2−11.4 M⊕. These are 2.5σ and 5σ results, respectively. With radii of Rp,b=3.49+0.06−0.05 R⊕ and Rp,c=5.45+0.18−0.17 R⊕, these results suggest that Kepler-103b has a Neptune-like density, while Kepler-103c is one of the highest density planets with a period P > 100 d. By providing high-precision estimates for the masses of the long-period, intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of long-period planets with known masses and radii, which will improve our understanding of the mass–radius relation across the full range of exoplanet masses and radii.
dc.format.extent19
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2019 the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz2856en
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectTechniques: spectroscopicen
dc.subjectPlanets and satellites; compositionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleUsing HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systemsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
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.doihttps://doi.org/10.1093/mnras/stz2856
dc.description.statusPeer revieweden


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