Abstract
We present the discovery from the TESS mission of two giant planets transiting M-dwarf stars: TOI 4201 b and TOI 5344 b. We also provide precise radial velocity measurements and updated system parameters for three other M dwarfs with transiting giant planets: TOI 519, TOI 3629, and TOI 3714. We measure planetary masses of 0.525 ± 0.064 M J, 0.243 ± 0.020 M J, 0.689 ± 0.030 M J, 2.57 ± 0.15 M J, and 0.412±0.040 M J for TOI 519 b, TOI 3629 b, TOI 3714 b, TOI 4201 b, and TOI 5344 b, respectively. The corresponding stellar masses are 0.372 ± 0.018 M ☉, 0.635 ± 0.032 M ☉, 0.522 ± 0.028 M ☉, 0.626 ± 0.033 M ☉, and 0.612 ± 0.034 M ☉. All five hosts have supersolar metallicities, providing further support for recent findings that, like for solar-type stars, close-in giant planets are preferentially found around metal-rich M-dwarf host stars. Finally, we describe a procedure for accounting for systematic errors in stellar evolution models when those models are included directly in fitting a transiting planet system.
| Original language | English |
|---|---|
| Article number | 163 |
| Journal | The Astronomical Journal |
| Volume | 166 |
| Issue number | 4 |
| DOIs | |
| Publication status | Published - 3 Oct 2023 |
Bibliographical note
The authors thank the anonymous referee for helpful comments that have improved the quality of the paper. J.H., G.B., and Z.C. acknowledge funding from NASA grant 80NSSC22K0315. This work is based in part on observations made with the Keck I telescope at Maunakea Observatory, Hawaii. Time on this facility was awarded through NASA. We would like to acknowledge the following individuals who contributed to gathering the Keck I/HIRES observations presented in this paper: I. Angelo, A. Polanski, S. Yee, D. Tyler, C. Beard, J. Van Zandt, J. Akana Murphy, A. Mayo, E. Petigura, L. Weiss, G. Gilbert, L. Handley, M. MacDougall, F. Dai, A. Householder, M. Rice, N. Saunders, J. Zhang, C. Brinkman, M. He, A. Langford, D. Pidhorodetska, J. Lubin, S. Blunt, E. Turtelboom, E. Louden, S. Dulz, and D. Shaw. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We acknowledge T. Gan for contributing to the data reduction of observations from the LCOGT facilities. This work is partly supported by JSPS KAKENHI grant Nos. JP17H04574, JP18H05439, and JP21K20376 and JST CREST grant No. JPMJCR1761. E.P. acknowledges funding from the Spanish Ministry of Economics and Competitiveness through project PID2021-125627OB-C32. E.E-B. acknowledges financial support from the European Union and the State Agency of Investigation of the Spanish Ministry of Science and Innovation (MICINN) under the grant PRE2020-093107 of the Pre-Doc Program for the Training of Doctors (FPI-SO) through FSE funds. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is 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, Hawaii, operated by the Las Cumbres Observatory. A.J. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and from FONDECYT project 1210718. R.B. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and from FONDECYT project 11200751. H.P. acknowledges support from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship No. RYC2021-031798-I. Funding from the University of La Laguna and the Spanish Ministry of Universities is acknowledged. Based on data collected under the ExTrA project at the ESO La Silla Paranal Observatory. ExTrA is a project of Institut de Planétologie et d'Astrophysique de Grenoble (IPAG/CNRS/UGA), funded by the European Research Council under the ERC grant agreement No. 337591-ExTrA. ExTrA has been supported by Labex OSUG@2020 (Investissements d'avenir—ANR10 LABX56), the "Programme National de Physique Stellaire" (PNPS), and the "Programme National de Palnétologie of CNRS/INSU, cofunded by CEA and CNES. We thank the Swiss National Science Foundation (SNSF) and Geneva University for their continuous support to our planet search programs. This work has in particular been carried out in the frame of the National Centre for Competence in Research "PlanetS" supported by the Swiss National Science Foundation (SNSF). 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. M.G. and A.T. acknowledge the support of the M.V. Lomonosov Moscow State University Program of Development. 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 research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA's Science Mission Directorate. K.A.C. acknowledges support from the TESS mission via subaward s3449 from MIT. This publication makes use of data products from the TRAPPIST project. TRAPPIST is funded by the Belgian National Fund for Scientific Research (F.R.S.-FNRS) under grant PDRT.0120.21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). E.J. is F.R.S.-FNRS Senior Research Associate. M.G. is F.R.S.-FNRS Research Director. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The ULiege's contribution to SPECULOOS has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013; grant agreement No. 336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant No. T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. SPECULOOS-North has received financial support from the Heising-Simons Foundation and from Dr. and Mrs. Colin Masson and Dr. Peter A. Gilman. This research received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 803193/BEBOP) and from the Science and Technology Facilities Council (STFC; grant No. ST/S00193X/1). This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to M.T. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This paper made use of data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA's Science Mission Directorate. The specific observations from MAST analyzed in this paper can be accessed from DOI:10.17909/1cab-7p42.Keywords
- Exoplanet systems