Investigating the physical properties of transiting hot Jupiters with the 1.5-m Kuiper Telescope
AuthorTurner, Jake D.
Leiter, Robin M.
Biddle, Lauren I.
Pearson, Kyle A.
Hardegree-Ullman, Kevin K.
Thompson, Robert M.
Teske, Johanna K.
Cates, Ian T.
Cook, Kendall L.
Berube, Michael P.
Nieberding, Megan N.
Jones, Christen K.
Watson, Zachary T.
Johnson, Robert E.
AffiliationUniv Arizona, Steward Observ
Univ Arizona, Lunar & Planetary Lab
planets and satellites: atmospheres
planets and satellites: gaseous planets
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationInvestigating the physical properties of transiting hot Jupiters with the 1.5-m Kuiper Telescope 2017, 472 (4):3871 Monthly Notices of the Royal Astronomical Society
Rights© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe present new photometric data of 11 hot Jupiter transiting exoplanets (CoRoT-12b, HATP-5b, HAT-P-12b, HAT-P-33b, HAT-P-37b, WASP-2b, WASP-24b, WASP-60b, WASP-80b, WASP-103b and XO-3b) in order to update their planetary parameters and to constrain information about their atmospheres. These observations of CoRoT-12b, HAT-P-37b and WASP-60b are the first follow-up data since their discovery. Additionally, the first near-UV transits of WASP-80b and WASP-103b are presented. We compare the results of our analysis with previous work to search for transit timing variations (TTVs) and a wavelength dependence in the transit depth. TTVs may be evidence of a third body in the system, and variations in planetary radius with wavelength can help constrain the properties of the exoplanet's atmosphere. For WASP-103b and XO-3b, we find a possible variation in the transit depths which may be evidence of scattering in their atmospheres. The B-band transit depth of HAT-P-37b is found to be smaller than its near-IR transit depth and such a variation may indicate TiO/VO absorption. These variations are detected from 2-4.6s, so follow-up observations are needed to confirm these results. Additionally, a flat spectrum across optical wavelengths is found for five of the planets (HAT-P-5b, HAT-P-12b, WASP-2b, WASP-24b and WASP-80b), suggestive that clouds may be present in their atmospheres. We calculate a refined orbital period and ephemeris for all the targets, which will help with future observations. No TTVs are seen in our analysis with the exception of WASP-80b and follow-up observations are needed to confirm this possible detection.
VersionFinal published version
SponsorsNASA's Planetary Atmospheres programme; Double Hoo Research Grant; National Science Foundation Graduate Research Fellowship [DGE-1315231]