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HATS-71b: A Giant Planet Transiting an M3 Dwarf Star in TESS Sector 1

2020; Institute of Physics; Volume: 159; Issue: 6 Linguagem: Inglês

10.3847/1538-3881/ab8ad1

1538-3881

G. Á. Bakos, D. Bayliss, J. Bento, W. Bhatti, Rafael Brahm, Z. Csubry, Néstor Espinoza, J. D. Hartman, Th. Henning, Andrés Jordán, L. Mancini, K. Penev, M. Rabus, P. Sarkis, V. Suc, M. de Val-Borro, George Zhou, R. Paul Butler, Jeffrey D. Crane, S. Durkan, Stephen A. Shectman, Jaeuk Kim, J. Lázár, I. Papp, P. Sári, G. Ricker, R. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, A. D. Chacon, Gábor Fűrész, B. Goeke, J. Li, Samuel N. Quinn, Elisa V. Quintana, Peter Tenenbaum, Johanna Teske, Michael Vezie, Liang Yu, Chris Stockdale, Phil Evans, Howard M. Relles,

Gamma-ray bursts and supernovae

Abstract We report the discovery of HATS-71b, a transiting gas giant planet on a <?CDATA $P=3.7955$?> day orbit around a <?CDATA $G=15.35$?> mag M3 dwarf star. HATS-71 is the coolest M dwarf star known to host a hot Jupiter. The loss of light during transits is 4.7%, more than in any other confirmed transiting planet system. The planet was identified as a candidate by the ground-based HATSouth transit survey. It was confirmed using ground-based photometry, spectroscopy, and imaging, as well as space-based photometry from the NASA Transiting Exoplanet Survey Satellite mission (TIC 234523599). Combining all of these data, and utilizing Gaia DR2, we find that the planet has a radius of <?CDATA $1.024\pm 0.018$?> <?CDATA ${R}_{{\rm{J}}}$?> and mass of <?CDATA $0.37\,\pm 0.24$?> <?CDATA ${M}_{{\rm{J}}}$?> (95% confidence upper limit of <?CDATA $\lt 0.80$?> <?CDATA ${M}_{{\rm{J}}}$?> ), while the star has a mass of <?CDATA $0.4861\pm 0.0060$?> <?CDATA ${M}_{\odot }$?> and a radius of <?CDATA $0.4783\pm 0.0060$?> <?CDATA ${R}_{\odot }$?> .