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Revisiting the HIP 41378 System with K2 and Spitzer
Berardo, David Crossfield, Ian Werner, Michael Petigura, Erik Christiansen, Jessie Ciardi, David R. Dressing, Courtney Fulton, Benjamin J. Gorjian, Varoujan Greene, Thomas P.
Berardo, David
Crossfield, Ian
Werner, Michael
Petigura, Erik
Christiansen, Jessie
Ciardi, David R.
Dressing, Courtney
Fulton, Benjamin J.
Gorjian, Varoujan
Greene, Thomas P.
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Abstract
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 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.
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Date
2019-04-22
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IOP Publishing
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Keywords
Planetary systems, Planets and satellites: detection, Planets and satellites: gaseous planets
Citation
David Berardo et al 2019 AJ 157 185