HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs

Creators: Hartman, J. D.; Jordán, Andrés; Bayliss, D.; Bakos, G. Á.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Henning, Th.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Crane, J. D.; Shectman, S.; Teske, J. K.; Wang, S. X.; Butler, R. P.; Lázár, J.; Papp, I.; Sári, P.; Anderson, D. R.; Hellier, C.; West, R. G.; Barkaoui, K.; Pozuelos, F. J.; Jehin, E.; Gillon, M.; Nielsen, L.; Lendl, M.; Udry, S.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Christiansen, Jessie; Crossfield, Ian J. M.; Henze, Christopher E.; Jenkins, Jon M.; Smith, Jeffrey C.; Ting, Eric B.

Abstract

We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have masses of 0.369^(+0.031)_(−0.021) M_J, 0.243^(+0.022)_(−0.030) M_J, 0.353^(+0.038)_(−0.027) M_J, and 0.1254±0.0039 M_J, respectively, and radii of 1.117±0.014 R_J, 0.800±0.015 R_J, 0.765±0.013 R_J, and 0.7224±0.0032 R_J, respectively. The planets orbit close to their host stars with orbital periods of 3.9228 days, 3.1317 days, 4.1480 days, and 7.3279 days, respectively. The hosts are main-sequence K dwarfs with masses of 0.674^(+0.016)_(−0.012) M⊙, 0.7279±0.0066 M⊙, 0.7133±0.0075 M⊙, and 0.7311±0.0028, and with V-band magnitudes of V=14.829±0.010, 14.35±0.11, 14.998±0.040 and 12.469±0.010. The super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP, and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and Magellan/PFS. We also incorporate TESS observations of the warm Saturn–hosting systems HATS-47 (a.k.a. TOI 1073.01), HATS-48A, and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved 5."4 neighbor in Gaia DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22 and a current projected physical separation of ~1400 au.

Additional Information

© 2020 The American Astronomical Society. Received 2020 January 9; revised 2020 February 10; accepted 2020 February 13; published 2020 March 26. The HATSouth network is operated by a collaboration consisting of Princeton University (PU), the Max Planck Institute für Astronomie (MPIA), the Australian National University (ANU), and the Pontificia Universidad Católica de Chile (PUC). The station at Las Campanas Observatory (LCO) of the Carnegie Institute is operated by PU in conjunction with PUC, the station at the High Energy Spectroscopic Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. Based in part on observations made with the MPG 2.2 m Telescope at the ESO Observatory in La Silla. Based on observations collected at the European Southern Observatory. This paper includes data gathered with the 6.5 meter Magellan Telescopes at Las Campanas Observatory, Chile. We thank the anonymous referee for valuable feedback, which has improved the quality of this paper. Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G, NNX12AH91H, and NNX17AB61G, and follow-up observations have received partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1171208 and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). L.M. acknowledges support from the Italian Ministry 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. K.P. acknowledges support from NASA ATP grant 80NSSC18K1009. V.S. acknowledges support from BASAL CATA PFB-06. J.N.W. thanks the Heising-Simons foundation for support. I.J.M.C. acknowledges support from the NSF through grant AST-1824644, and from NASA through Caltech/JPL grant RSA-1610091. Support for this work was provided to J.K.T. by NASA through Hubble Fellowship grant HST-HF2-51399.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also makes use of observations from the LCOGT network. Some of this time was awarded by NOAO. 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 MPG 2.2 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. TRAPPIST-South is a project funded by the Belgian F.R.S.-FNRS under grant FRFC 2.5.594.09.F, with the participation of the Swiss FNS. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. E.J. and M.G. are F.R.S.-FNRS Senior Research Associates. Contributions at the University of Geneva by L.N., M.L., and S.U. were carried out within the framework of the National Centre for Competence in Research "PlanetS" supported by the Swiss National Science Foundation (SNSF). M.L. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 "GRAPPA." This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use NASA's Astrophysics Data System Bibliographic Services. Facilities: HATSouth - , TESS - , SuperWASP - , Swope - , LCOGT - , TRAPPIST - , Max Planck:2.2 m (FEROS) - , ESO:3.6 m (HARPS) - , Euler1.2 m (Coralie) - , ATT (WiFeS) - , Magellan:Clay (PFS) - , VLT (ESPRESSO) - , NTT (Astralux Sur) - , SOAR - , Gaia - , Exoplanet Archive. - Software: FITSH (Pál 2012), BLS (Kovács et al. 2002), VARTOOLS (Hartman & Bakos 2016), CERES (Brahm et al. 2017a), ZASPE (Brahm et al. 2017b), SPEX-tool (Cushing et al. 2004; Vacca et al. 2004), SExtractor (Bertin & Arnouts 1996), Astrometry.net (Lang et al. 2010), MWDUST (Bovy et al. 2016), TESSCut (Brasseur et al. 2019), Lightkurve (Lightkurve Collaboration et al. 2018), Astropy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018).

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