HAT-P-58b–HAT-P-64b: Seven Planets Transiting Bright Stars

Creators: Bakos, G. Á.; Hartman, J. D.; Bhatti, W.; Csubry, Z.; Penev, K.; Bieryla, A.; Latham, D. W.; Quinn, S.; Buchhave, L. A.; Kovács, G.; Torres, Guillermo; Noyes, R. W.; Falco, E.; Béky, Bence; Szklenár, T.; Esquerdo, G. A.; Howard, A. W.; Isaacson, H.; Marcy, G.; Sato, B.; Boisse, I.; Santerne, A.; Hébrard, G.; Rabus, M.; Harbeck, D.; McCully, C.; Everett, M. E.; Horch, E. P.; Hirsch, L.; Howell, S. B.; Huang, C. X.; Lázár, J.; Papp, I.; Sári, P.

Abstract

We report the discovery and characterization of seven transiting exoplanets from the HATNet survey. The planets, which are hot Jupiters and Saturns transiting bright Sun-like stars, include: HAT-P-58b (with mass M_p = 0.37 M_J, radius R_p = 1.33 R_J, and orbital period P = 4.0138 days), HAT-P-59b (M_p = 1.54 M_J, R_p = 1.12 R_J, P = 4.1420 days), HAT-P-60b (M_p = 0.57 M_J, R_p = 1.63 R_J, P = 4.7948 days), HAT-P-61b (M_p = 1.06 M_J, R_p = 0.90 R_J, P = 1.9023 days), HAT-P-62b (M_p = 0.76 M_J, R_p = 1.07 R_J, P = 2.6453 days), HAT-P-63b (M_p = 0.61 M_J, R_p = 1.12 R_J, P = 3.3777 days), and HAT-P-64b (M_p = 0.58 M_J, R_p = 1.70 R_J, P = 4.0072 days). The typical errors on these quantities are 0.06 M_J, 0.03 R_J, and 0.2 s, respectively. We also provide accurate stellar parameters for each of the host stars. With V = 9.710 ± 0.050 mag, HAT-P-60 is an especially bright transiting planet host, and an excellent target for additional follow-up observations. With R_p = 1.703 ± 0.070 R_J, HAT-P-64b is a highly inflated hot Jupiter around a star nearing the end of its main-sequence lifetime, and is among the largest known planets. Five of the seven systems have long-cadence observations by TESS which are included in the analysis. Of particular note is HAT-P-59 (TOI-1826.01) which is within the northern continuous viewing zone of the TESS mission, and HAT-P-60, which is the TESS candidate TOI-1580.01.

Additional Information

© 2021. The American Astronomical Society. Received 2020 July 6; revised 2021 January 8; accepted 2021 February 15; published 2021 June 8. Based on observations of the Hungarian-made Automated Telescope Network and observations obtained at the following observatories: W. M. Keck Observatory, the 1.5 m and the 1.2 m telescopes at the Fred Lawrence Whipple Observatory of the Smithsonian Astrophysical Observatory, the Kitt Peak National Observatory, the 1.93 m telescope at Observatoire de Haute-Provence, the Subaru Telescope of the National Astronomical Observatory of Japan, the Nordic Optical Telescope in the Spanish Observatorio del Roque de los Muchachos of the Intituto de Astrofísica de Canarias, and the Apache Point Observatory 3.5 m telescope. We thank the referee, David James, for helpful comments which improved the quality of this paper. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and NNX13AJ15G. Follow-up of HATNet targets has been partially supported through NSF grant AST-1108686. G.Á.B, J.H., Z.C., and K.P. acknowledge partial support from NASA grant NNX17AB61G. G.B. acknowledges support from the Hungarian Academy of Sciences, and thanks for the warm hospitality of Konkoly Observatory in carrying out some of his research. J.H. acknowledges support from NASA grant NNX14AF87G. K.P. acknowledges support from NASA grant 80NSSC18K1009. G.K. thanks the support from the National Research, Development and Innovation Office (grant K 129249). We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NNX13AB58A (D.W.L., PI). Data presented in this paper are based on observations obtained at the HAT station at the Submillimeter Array of SAO, and the HAT station at the Fred Lawrence Whipple Observatory of SAO. We acknowledge J.A. Johnson in supporting the Keck HIRES observations. The authors wish to acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. This research has made use of Keck telescope time granted through NOAO (programs: A245Hr, A202Hr; PI: G.B) and NASA (programs: N154Hr, N133Hr, N136Hr, N143Hr, N169Hr, N186Hr; PI: G.B). Based on observations at Kitt Peak, NOAO (NOAO Prop. ID: 2015B-0156; PI: J.H.), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Based on radial velocities obtained with the SOPHIE spectrograph mounted on the 1.93 m telescope at Observatoire de Haute-Provence. Based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Norway, Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Intituto de Astrofísica de Canarias. Based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. This research has made use of the NASA Exoplanet Archive, which is operated by Caltech, under contract with NASA under the Exoplanet Exploration Program. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555.

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