TY - JOUR
T1 - HATS-70b
T2 - A 13 MJ Brown Dwarf Transiting an A Star
AU - Zhou, G.
AU - Bakos, G.
AU - Bayliss, D.
AU - Bento, J.
AU - Bhatti, W.
AU - Brahm, R.
AU - Csubry, Z.
AU - Espinoza, N.
AU - Hartman, J. D.
AU - Henning, T.
AU - Jordán, A.
AU - Mancini, L.
AU - Penev, K.
AU - Rabus, M.
AU - Sarkis, P.
AU - Suc, V.
AU - Val-Borro, M. De
AU - Rodriguez, J. E.
AU - Osip, D.
AU - Kedziora-Chudczer, L.
AU - Bailey, J.
AU - Tinney, C. G.
AU - Durkan, S.
AU - Lázár, J.
AU - Papp, I.
AU - Sári, P.
N1 - Funding Information:
Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, and operations have been supported by NASA grants NNX09AB29G, NNX12AH91H, and NNX17AB61G, and follow-up observations receive partial support from grant NSF/AST-1108686. Work by G.Z. is provided by NASA through Hubble Fellowship grant HST-HF2-51402.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. J.H. acknowledges support from NASA grant NNX14AE87G. A.J. acknowledges support from FONDECYT project 1171208, BASAL CATA PFB-06, and project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millennium Science Initiative, Chilean Ministry of Economy. N.E. is supported by BASAL CATA PFB-06. R.B. and N.E. acknowledge support from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. L.M. acknowledges support from the Italian Minister of Instruction, University and Research (MIUR) through FFABR 2017 fund. L.M. acknowledges support from the University of Rome Tor Vergata through “Mission: Sustainability 2016” fund. The modeling in this paper was performed on the Smithsonian Institution High Performance Cluster (SI/HPC). This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. We thank the MPG 2.2 m telescope support team for their technical assistance during observations.
Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/1
Y1 - 2019/1
N2 - We report the discovery of HATS-70b, a transiting brown dwarf at the deuterium burning limit. HATS-70b has a mass of Mp = 12.9+1.8-1.6 MJup and a radius of Rp 1.384+ 0.074 0.079 MJup, residing in a close-in orbit with a period of 1.89 days. The host star is a M∗= M 1.78 0.12 M A star rotating at = v sin I 40.61+ km s- 0.35 0.32 1, enabling us to characterize the spectroscopic transit of the brown dwarf via Doppler tomography. We find that HATS-70b, like other massive planets and brown dwarfs previously sampled, orbits in a low projected-obliquity orbit with l = 8.9+4.5 5.6. The low obliquities of these systems is surprising given all brown dwarf and massive planets with obliquities measured orbit stars hotter than the Kraft break. This trend is tentatively inconsistent with dynamically chaotic migration for systems with massive companions, though the stronger tidal influence of these companions makes it difficult to draw conclusions on the primordial obliquity distribution of this population. We also introduce a modeling scheme for planets around rapidly rotating stars, accounting for the influence of gravity darkening on the derived stellar and planetary parameters.
AB - We report the discovery of HATS-70b, a transiting brown dwarf at the deuterium burning limit. HATS-70b has a mass of Mp = 12.9+1.8-1.6 MJup and a radius of Rp 1.384+ 0.074 0.079 MJup, residing in a close-in orbit with a period of 1.89 days. The host star is a M∗= M 1.78 0.12 M A star rotating at = v sin I 40.61+ km s- 0.35 0.32 1, enabling us to characterize the spectroscopic transit of the brown dwarf via Doppler tomography. We find that HATS-70b, like other massive planets and brown dwarfs previously sampled, orbits in a low projected-obliquity orbit with l = 8.9+4.5 5.6. The low obliquities of these systems is surprising given all brown dwarf and massive planets with obliquities measured orbit stars hotter than the Kraft break. This trend is tentatively inconsistent with dynamically chaotic migration for systems with massive companions, though the stronger tidal influence of these companions makes it difficult to draw conclusions on the primordial obliquity distribution of this population. We also introduce a modeling scheme for planets around rapidly rotating stars, accounting for the influence of gravity darkening on the derived stellar and planetary parameters.
KW - stars: individual (HATS-70)
KW - techniques: photometric
KW - techniques: spectroscopic
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U2 - 10.3847/1538-3881/aaf1bb
DO - 10.3847/1538-3881/aaf1bb
M3 - Article
AN - SCOPUS:85060180795
SN - 0004-6256
VL - 157
JO - Astronomical Journal
JF - Astronomical Journal
IS - 1
M1 - 31
ER -