Bento (Da Silva Bento), JoaoHartman, Joel DBakos, G ABhatti, WaqasCsubry, ZPenev, K.Bayliss, Dde Val-Borro, MiguelZhou, G.Brahm, REspinoza, NRabus, MJordan, ASuc, VCiceri, Simona2024-04-162024-04-160035-8711http://hdl.handle.net/1885/316806We report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS- 39b, HATS-40b, HATS-41b, and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5 ≲ v ≲ 13.7) F dwarf stars on short (2-5 d) periods. The planets have similar radii, ranging from 1.33-0.20 +0.29 RJ for HATS-41b to 1.58-0.12+0.16 RJ for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63 ± 0.13MJ, and an inflated radius of 1.57 ± 0.12 RJ, making it a good target for future transmission spectroscopic studies. HATS- 41b is a very massive 9.7 ± 1.6MJ planet and one of only a few hot Jupiters found to date with a mass over 5 MJ. This planet orbits the highest metallicity star ([Fe/H] = 0.470 ± 0.010) known to host a transiting planet and is also likely on an eccentric orbit. The highmass, coupled with a relatively young age (1.34-0.51+0.31 Gyr) for the host star, is a factor that may explain why this planet's orbit has not yet circularized.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. JH acknowledges support from NASA grant NNX14AE87G. AJ acknowledges support from FONDECYT project 1171208, BASAL CATA PFB-06, and project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Millenium Science Initiative, Chilean Ministry of Economy. RB and NE acknowledge support from project IC120009 ‘Millenium Institute of Astrophysics (MAS)’ of the Millennium Science Initiative, Chilean Ministry of Economy. VS acknowledges support from BASAL CATA PFB-06. This work also uses observations obtained with facilities of the LCOGT. 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 work is based on observations made with ESO Telescopes at the La Silla Observatory. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD data base, 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 are grateful to P.Sackett for her help in the early phase of the HATSouth project. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work is based on observations collected with HARPS and FEROS at the European Organization for Astronomical Research in the Southern hemisphere under ESO programmes 095.C-0367, CN2013A-171, CN2013B-55, CN2014A-104, CN2014B-57, CN2015A-51, and ESO 096.C-0544application/pdfen-AU© 2018 The authorshttp://creativecommons.org/licenses/by/4.0/techniques: photometrictechniques: spectroscopicstars: individual: HATS39, HATS-40, HATS-41, HATS-42stars: individual: GSC 6550-00341, GSC 6533-01514, GSC 6530-01596, GSC 7107-03973planetary systems201810.1093/mnras/sty7262022-12-11