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dc.contributor.authorAlbrecht, Simon
dc.contributor.authorArriagada, Pamela
dc.contributor.authorBieryla, Allyson
dc.contributor.authorButler, R. Paul
dc.contributor.authorCrane, Jeffrey D.
dc.contributor.authorHirano, Teriyaki
dc.contributor.authorJohnson, John Asher
dc.contributor.authorKiilerich, Amanda
dc.contributor.authorLatham, David W.
dc.contributor.authorNarita, Norio
dc.contributor.authorNowak, Grzegorz
dc.contributor.authorPalle, Enric
dc.contributor.authorRibas, Ignasi
dc.contributor.authorRogers, Leslie A.
dc.contributor.authorSanchis-Ojeda, Roberto
dc.contributor.authorShectman, Stephen A.
dc.contributor.authorTeske, Johanna K.
dc.contributor.authorThompson, Ian B.
dc.contributor.authorVanderburg, Andrew
dc.contributor.authorWittenmyer, Robert A.
dc.contributor.authorDai, Fei
dc.contributor.authorVan Eylen, Vincent
dc.contributor.authorYu, Liang
dc.contributor.authorWinn, Joshua Nathan
dc.date.accessioned2018-06-05T15:30:03Z
dc.date.available2018-06-05T15:30:03Z
dc.date.issued2016-05
dc.date.submitted2016-02
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/116096
dc.description.abstractIn an effort to measure the masses of planets discovered by the NASA K2 mission, we have conducted precise Doppler observations of five stars with transiting planets. We present the results of a joint analysis of these new data and previously published Doppler data. The first star, an M dwarf known as K2-3 or EPIC 201367065, has three transiting planets ("b," with radius "c," and "d," ). Our analysis leads to the mass constraints: M[subscript b] = 8.1[superscript =+2.0][subscript -1.9] M[subscript ⊕] And M[subscript c] < 4.2 M[subscript ⊕] (95% confidence). The mass of planet d is poorly constrained because its orbital period is close to the stellar rotation period, making it difficult to disentangle the planetary signal from spurious Doppler shifts due to stellar activity. The second star, a G dwarf known as K2-19 or EPIC 201505350, has two planets ("b," 7.7 R[subscript ⊕]; and "c," 4.9 R[subscript ⊕]) in a 3:2 mean-motion resonance, as well as a shorter-period planet ("d," 1.1 R[subscript ⊕]). We find M[subscript b] = 28.5[superscript +5.4][subscript -5.0]M[subscript ⊕], M[subscript c] = 25.6[superscript +7.1][subscript -7.1] and M[subscript d] < 14.0 M[subscript ⊕] (95% conf.). The third star, a G dwarf known as K2-24 or EPIC 203771098, hosts two transiting planets ("b," 5.7 R[subscript ⊕]; and "c," 7.8 R[subscript ⊕]) with orbital periods in a nearly 2:1 ratio. We find M[subscript b] = 19.8[superscript +4.5][subscript -4.4] and M[subscript c] = 26.0[superscript +5.8][subscript -6.1]. The fourth star, a G dwarf known as EPIC 204129699, hosts a hot Jupiter for which we measured the mass to be 1.857[superscript +0.081][subscript -0.081]M[subscript Jup]. The fifth star, a G dwarf known as EPIC 205071984, contains three transiting planets ("b," 5.4 R[subscript ⊕]; "c," 3.5 R[subscript ⊕]; and "d," 3.8 R[subscript ⊕]), the outer two of which have a nearly 2:1 period ratio. We find M[subscript b] = 21.1[superscript +5.9][subscript -5.9]M[subscript ⊕], M[subscript c] < 8.1 M[subscript ⊕] (95% conf.) and M[subscript d] < 35 M[subscript ⊕] (95% conf.).en_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.isversionofhttp://dx.doi.org/10.3847/0004-637X/823/2/115en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.titleDOPPLER MONITORING OF FIVE K2 TRANSITING PLANETARY SYSTEMSen_US
dc.typeArticleen_US
dc.identifier.citationDai, Fei, et al. “DOPPLER MONITORING OF FIVE K2 TRANSITING PLANETARY SYSTEMS.” The Astrophysical Journal, vol. 823, no. 2, May 2016, p. 115. © 2016. The American Astronomical Society.en_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorDai, Fei
dc.contributor.mitauthorWinn, Joshua N.
dc.contributor.mitauthorVan Eylen, Vincent
dc.contributor.mitauthorYu, Liang
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2018-02-16T14:23:34Z
dspace.orderedauthorsDai, Fei; Winn, Joshua N.; Albrecht, Simon; Arriagada, Pamela; Bieryla, Allyson; Butler, R. Paul; Crane, Jeffrey D.; Hirano, Teriyaki; Johnson, John Asher; Kiilerich, Amanda; Latham, David W.; Narita, Norio; Nowak, Grzegorz; Palle, Enric; Ribas, Ignasi; Rogers, Leslie A.; Sanchis-Ojeda, Roberto; Shectman, Stephen A.; Teske, Johanna K.; Thompson, Ian B.; Eylen, Vincent Van; Vanderburg, Andrew; Wittenmyer, Robert A.; Yu, Liangen_US
dspace.embargo.termsNen_US
dc.identifier.orcidhttps://orcid.org/0000-0002-8958-0683
dc.identifier.orcidhttps://orcid.org/0000-0002-4265-047X
dc.identifier.orcidhttps://orcid.org/0000-0003-1667-5427
mit.licensePUBLISHER_POLICYen_US


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