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dc.contributor.authorBerardo, David
dc.contributor.authorCrossfield, Ian JM
dc.contributor.authorWerner, Michael
dc.contributor.authorPetigura, Erik
dc.contributor.authorChristiansen, Jessie
dc.contributor.authorCiardi, David R
dc.contributor.authorDressing, Courtney
dc.contributor.authorFulton, Benjamin J
dc.contributor.authorGorjian, Varoujan
dc.contributor.authorGreene, Thomas P
dc.contributor.authorHardegree-Ullman, Kevin
dc.contributor.authorKane, Stephen R
dc.contributor.authorLivingston, John
dc.contributor.authorMorales, Farisa
dc.contributor.authorSchlieder, Joshua E
dc.date.accessioned2021-09-20T18:22:15Z
dc.date.available2021-09-20T18:22:15Z
dc.identifier.urihttps://hdl.handle.net/1721.1/132402
dc.description.abstract© 2019. The American Astronomical Society. All rights reserved. We present new observations of the multiplanet system HIP 41378, a bright star (V = 8.9, K s = 7.7) with five known transiting planets. Previous K2 observations showed multiple transits of two Neptune-sized bodies and single transits of three larger planets (R P = 0.33R J, 0.47R J, 0.88R J). K2 recently observed the system again in Campaign 18 (C18). We observe one new transit each of two of the larger planets d/f, giving maximal orbital periods of 1114/1084 days, as well as integer divisions of these values down to a lower limit of about 50 days. We use all available photometry to determine the eccentricity distributions of HIP 41378 d & f, finding that periods ≲300 days require non-zero eccentricity. We check for overlapping orbits of planets d and f to constrain their mutual periods, finding that short periods (P < 300 days) for planet f are disfavored. We also observe transits of planets b and c with Spitzer/Infrared Array Camera (IRAC), which we combine with the K2 observations to search for transit timing variations (TTVs). We find a linear ephemeris for planet b, but see a significant TTV signal for planet c. The ability to recover the two smaller planets with Spitzer shows that this fascinating system will continue to be detectable with Spitzer, CHEOPS, TESS, and other observatories, allowing us to precisely determine the periods of d and f, characterize the TTVs of planet c, recover the transits of planet e, and further enhance our view of this remarkable dynamical laboratory.en_US
dc.language.isoen
dc.publisherAmerican Astronomical Societyen_US
dc.relation.isversionof10.3847/1538-3881/AB100Cen_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.sourceThe American Astronomical Societyen_US
dc.titleRevisiting the HIP 41378 System with K 2 and Spitzeren_US
dc.typeArticleen_US
dc.relation.journalAstronomical 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.updated2020-10-19T17:59:00Z
dspace.orderedauthorsBerardo, D; Crossfield, IJM; Werner, M; Petigura, E; Christiansen, J; Ciardi, DR; Dressing, C; Fulton, BJ; Gorjian, V; Greene, TP; Hardegree-Ullman, K; Kane, SR; Livingston, J; Morales, F; Schlieder, JEen_US
dspace.date.submission2020-10-19T17:59:08Z
mit.journal.volume157en_US
mit.journal.issue5en_US
mit.licensePUBLISHER_POLICY
mit.metadata.statusAuthority Work and Publication Information Needed


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