HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs

Creators: Jordán, Andrés; Hartman, J. D.; Bayliss, D.; Bakos, G. Á.; Brahm, R.; Bryant, E. M.; Csubry, Z.; Henning, Th.; Hobson, M.; Mancini, L.; Penev, K.; Rabus, M.; Suc, V.; de Val-Borro, M.; Wallace, J.; Barkaoui, K.; Ciardi, David R.; Collins, K. A.; Esparza-Borges, E.; Furlan, E.; Gan, T.; Benkhaldoun, Z.; Ghachoui, M.; Gillon, M.; Howell, S.; Jehin, E.; Fukui, A.; Kawauchi, K.; Livingston, J. H.; Luque, R.; Matson, R.; Matthews, E. C.; Osborn, H. P.; Murgas, F.; Narita, Norio; Palle, E.; Parvianen, H.; Waalkes, W. C.

Abstract

The relative rarity of giant planets around low-mass stars compared with solar-type stars is a key prediction from the core-accretion planet formation theory. In this paper we report on the discovery of four gas giant planets that transit low-mass late K and early M dwarfs. The planets HATS-74Ab (TOI 737b), HATS-75b (TOI 552b), HATS-76b (TOI 555b), and HATS-77b (TOI 730b) were all discovered from the HATSouth photometric survey and follow-up using TESS and other photometric facilities. We use the new ESPRESSO facility at the VLT to confirm systems and measure their masses. We find that these planets have masses of 1.46 ± 0.14 MJ, 0.491 ± 0.039 MJ, 2.629 ± 0.089 MJ, and 1.374^(+0.100)_(-0.074) MJ, respectively, and radii of 1.032 ± 0.021 RJ, 0.884 ± 0.013 RJ, 1.079 ± 0.031 RJ, and 1.165 ± 0.021 RJ, respectively. The planets all orbit close to their host stars with orbital periods ranging from 1.7319 days to 3.0876 days. With further work, we aim to test core-accretion theory by using these and further discoveries to quantify the occurrence rate of giant planets around low-mass host stars.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 September 23; revised 2021 November 9; accepted 2021 November 17; published 2022 February 11. 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 Universidad Adolfo Ibáñez (UAI). The station at Las Campanas Observatory (LCO) of the Carnegie Institute is operated by PU in conjunction with UAI, 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. A.J. thanks Gijs Mulders for informative discussions. 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 1210718, and ANID—Millennium Science Initiative—ICN12_009. J.H. acknowledges partial support from the TESS GI Program, programs G011103 and G022117, through NASA grants 80NSSC19K0386 and 80NSSC19K1728. 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. K.P. acknowledges support from NASA ATP grant 80NSSC18K1009. M.R. acknowledges support from the Universidad Católica de lo Santísima Concepción grant DI-FIAI 03/2021. R.L. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52/AEI/10.13039/501100011033, and the Centre of Excellence "Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). Based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 0103.C-0449(A). Part of this work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation. ECM acknowledges the financial support of the SNSF. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper is partly based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This work is partly supported by JSPS KAKENHI grant No. JP20K14518. Some of the Observations in the paper made use of the High-Resolution Imaging instrument(s) `Alopeke (and/or Zorro). `Alopeke (and/or Zorro) was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Data were reduced using a software pipeline originally written by Elliott Horch and Mark Everett. `Alopeke (and/or Zorro) was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovaçóes e Comunicaçóes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). 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. TRAPPIST-South is a project funded by the Belgian F.R.S.-FNRS under grant PDR T.0120.21, 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. EJ and MG are F.R.S.-FNRS Senior Research Associates. This work is partly supported by JSPS KAKENHI grant No. JP18H05439, JST CREST grant No. JPMJCR1761, the Astrobiology Center of National Institutes of Natural Sciences (NINS; grant No. AB031010). 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. Facility: HATSouth, TESS, LCOGT (0.4 m, 1 m, 2 m MuSCAT3), CTIO 0.9 m, MuSCAT2, TRAPPIST-South, Mt Stuart 0.3 m, VLT (ESPRESSO), Gemini (`Alopeke), Keck (NIRC2), VLT (NaCo), ARC 3.5 m (WHIRC), 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), SpexTool (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, 2018), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013).

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