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dc.contributor.authorBerardo, David
dc.contributor.authorCrossfield, Ian
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.accessioned2020-12-23T19:28:19Z
dc.date.available2020-12-23T19:28:19Z
dc.date.issued2019-04-22
dc.identifier.citationDavid Berardo et al 2019 AJ 157 185en_US
dc.identifier.urihttp://hdl.handle.net/1808/31001
dc.description.abstractWe 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 lesssim300 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.publisherIOP Publishingen_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectPlanetary systemsen_US
dc.subjectPlanets and satellites: detectionen_US
dc.subjectPlanets and satellites: gaseous planetsen_US
dc.titleRevisiting the HIP 41378 System with K2 and Spitzeren_US
dc.typeArticleen_US
kusw.kuauthorCrossfield, Ian
kusw.kudepartmentPhysics and Astronomyen_US
dc.identifier.doi10.3847/1538-3881/ab100cen_US
dc.identifier.orcidhttps://orcid.org/0000-0001-6298-412Xen_US
dc.identifier.orcidhttps://orcid.org/0000-0002-1835-1891en_US
dc.identifier.orcidhttps://orcid.org/0000-0003-0967-2893en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-8035-4778en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-5741-3047en_US
dc.identifier.orcidhttps://orcid.org/0000-0001-8189-0233en_US
dc.identifier.orcidhttps://orcid.org/0000-0003-3504-5316en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-8963-8056en_US
dc.identifier.orcidhttps://orcid.org/0000-0003-3702-0382en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-7084-0529en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-4881-3620en_US
dc.identifier.orcidhttps://orcid.org/0000-0001-9414-3851en_US
dc.identifier.orcidhttps://orcid.org/0000-0001-5347-7062en_US
kusw.oaversionScholarly/refereed, publisher versionen_US
kusw.oapolicyThis item meets KU Open Access policy criteria.en_US
dc.rights.accessrightsopenAccessen_US


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