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Published December 3, 2021 | Supplemental Material
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GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

Lam, Kristine W. F. ORCID icon
Csizmadia, Szilárd ORCID icon
Astudillo-Defru, Nicola ORCID icon
Bonfils, Xavier ORCID icon
Gandolfi, Davide ORCID icon
Padovan, Sebastiano ORCID icon
Esposito, Massimiliano ORCID icon
Hellier, Coel ORCID icon
Hirano, Teruyuki ORCID icon
Livingston, John ORCID icon
Murgas, Felipe ORCID icon
Smith, Alexis M. S. ORCID icon
Collins, Karen A. ORCID icon
Mathur, Savita ORCID icon
Garcia, Rafael A. ORCID icon
Howell, Steve B. ORCID icon
Santos, Nuno C. ORCID icon
Dai, Fei ORCID icon
Ricker, George R. ORCID icon
Vanderspek, Roland ORCID icon
Latham, David W. ORCID icon
Seager, Sara ORCID icon
Winn, Joshua N. ORCID icon
Jenkins, Jon M. ORCID icon
Albrecht, Simon ORCID icon
Almenara, Jose M. ORCID icon
Artigau, Étienne ORCID icon
Barragán, Oscar ORCID icon
Bouchy, François ORCID icon
Cabrera, Juan ORCID icon
Charbonneau, David ORCID icon
Chaturvedi, Priyanka ORCID icon
Chaushev, Alexander ORCID icon
Christiansen, Jessie L. ORCID icon
Cochran, William D. ORCID icon
De Meideiros, José R. ORCID icon
Delfosse, Xavier ORCID icon
Díaz, Rodrigo F. ORCID icon
Doyon, René ORCID icon
Eigmüller, Philipp ORCID icon
Figueira, Pedro ORCID icon
Forveille, Thierry ORCID icon
Fridlund, Malcolm ORCID icon
Gaisné, Guillaume
Goffo, Elisa ORCID icon
Georgieva, Iskra ORCID icon
Grziwa, Sascha ORCID icon
Guenther, Eike ORCID icon
Hatzes, Artie P. ORCID icon
Johnson, Marshall C. ORCID icon
Kabáth, Petr ORCID icon
Knudstrup, Emil ORCID icon
Korth, Judith ORCID icon
Lewin, Pablo ORCID icon
Lissauer, Jack J. ORCID icon
Lovis, Christophe ORCID icon
Luque, Rafael ORCID icon
Melo, Claudio ORCID icon
Morgan, Edward H. ORCID icon
Morris, Robert ORCID icon
Mayor, Michel ORCID icon
Narita, Norio ORCID icon
Osborne, Hannah L. M. ORCID icon
Palle, Enric ORCID icon
Pepe, Francesco ORCID icon
Persson, Carina M. ORCID icon
Quinn, Samuel N. ORCID icon
Rauer, Heike ORCID icon
Redfield, Seth ORCID icon
Schlieder, Joshua E. ORCID icon
Ségransan, Damien ORCID icon
Serrano, Luisa M. ORCID icon
Smith, Jeffrey C. ORCID icon
Šubjak, Ján ORCID icon
Twicken, Joseph D. ORCID icon
Udry, Stéphane ORCID icon
Van Eylen, Vincent ORCID icon
Vezie, Michael ORCID icon
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Abstract

Ultrashort-period (USP) exoplanets have orbital periods shorter than 1 day. Precise masses and radii of USP exoplanets could provide constraints on their unknown formation and evolution processes. We report the detection and characterization of the USP planet GJ 367b using high-precision photometry and radial velocity observations. GJ 367b orbits a bright (V-band magnitude of 10.2), nearby, and red (M-type) dwarf star every 7.7 hours. GJ 367b has a radius of 0.718 ± 0.054 Earth-radii and a mass of 0.546 ± 0.078 Earth-masses, making it a sub-Earth planet. The corresponding bulk density is 8.106 ± 2.165 grams per cubic centimeter—close to that of iron. An interior structure model predicts that the planet has an iron core radius fraction of 86 ± 5%, similar to that of Mercury's interior.

Additional Information

© 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. https://www.sciencemag.org/about/science-licenses-journal-article-reuse This is an article distributed under the terms of the Science Journals Default License. Received: 31 December 2020. Accepted: 12 October 2021. Published in print: 2 December 2021. We acknowledge use of observations from the LCOGT network. We made use of data from the European Space Agency (ESA) mission Gaia (www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC) (www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions. Some of the observations were made at Gemini South using the high-resolution imaging instrument Zorro, funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by S. B. Howell, N. Scott, E. P. Horch, and E. Quigley. Zorro was mounted on the Gemini 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); the National Research Council (Canada); Agencia Nacional de Investigacin y Desarrollo (Chile); Ministerio de Ciencia, Tecnologa e Innovacin (Argentina); Ministrio da Ciłncia, Tecnologia, Inovaes e Comunicaes (Brazil); and the Korea Astronomy and Space Science Institute (Republic of Korea). This is University of Texas Center for Planetary Systems Habitability Contribution no. 0041. K.W.F.L., Sz.Cs., M.E., S.G., A.P.H., and H.R. were supported by Deutsche Forschungsgemeinschaft grants PA525/18-1, PA525/19-1, PA525/20-1, HA3279/12-1, and RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. Sz.Cs. is supported by Deutsche Forschungsgemeinschaft Research Unit 2440, Matter Under Planetary Interior Conditions: High Pressure Planetary and Plasma Physics. T.H. was supported by JSPS KAKENHI grant no. JP19K14783, and N.N. was supported by JSPS KAKENHI grant nos. JP18H01265 and JP18H05439 and JST PRESTO grant no. JPMJPR1775. J.L. is supported by JSPS KAKENHI grant no. JP20K14518. R.A.G. acknowledges support from PLATO and GOLF CNES grants. P.K. acknowledges support from the MSMT grant LTT20015. S.M. acknowledges support by the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship no. RYC-2015-17697 and grant no. PID2019-107187GB-I00. N.C.S. was supported by Fundaçao para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113, and PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953. X.D. and G.G. acknowledge funding in the framework of the Investissements d'Avenir program (ANR-15-IDEX-02), Origin of Life project of the Université Grenoble-Alpes. J.R.D.M. acknowledges grants from CNPq, CAPES, and FAPERN Brazilian agencies. N.A.-D. acknowledges support from FONDECYT project 3180063. Resources for the production of the SPOC data products were provided by the NASA High-End Computing (HEC) program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. S.A. is supported by the Danish National Research Foundation (grant agreement no. DNRF106). D.G. and L.M.S. acknowledge financial support from the Cassa di Risparmio di Torino foundation under grant no. 2018.2323, "Gaseous or rocky? Unveiling the nature of small worlds." Author contributions: K.W.F.L. contributed to the planet detection, transit light curve analysis, gyrochronology age estimate, and tidal evolution calculations and led the writing of the paper. Sz.Cs. performed the joint light curve and RV analysis using the Transit and Light Curve Modeller (TLCM). N.A.-D. and X.B. led the HARPS RV follow-up program and reduced and analyzed the RV data. D.G. performed the frequency analysis of the RV and activity indicators. F.D., O.B., A.P.H., and R.L. analyzed the RV data. S.P. determined the interior composition of the planet and modeled the precursor gaseous planet. M.E. performed the Rapid Eye Mount (REM) robotic telescope observations and analysis. M.E. and A.M.S.S. derived the light curve dilution factor. C.H., K.W.F.L., S.M., and R.A.G. determined the stellar rotation period using WASP data. S.B.H. analyzed the speckle imaging data. T.H. and M.F. performed the spectral analysis using SpecMatch-Emp, and T.H. derived the stellar parameters using an MCMC simulation. J.L. performed stellar characterization using isochrone fitting. F.M. performed the LCOGT and HARPS observations. K.A.C. coordinated the TESS SG1 working group. K.A.C. and P.L. analyzed the ground-based photometric observations. N.C.S. performed spectral characterization using ODUSSEAS. M.C.J. determined the Galactic space velocities of the star. K.W.F.L. and S.R. calculated the emission spectroscopy metric. J.K. performed transit-timing variation (TTV) analysis. J.C., P.E., and S.G. analyzed the light curve for planet detection. E.Gu. analyzed the activity indicators. G.R.R., R.V., D.W.L., S.S., J.N.W., and J.M.J. led and organized the TESS mission, including the observations, processing of the data, working groups coordination, target selection, and dissemination of the data products. E.H.M., M.V., and J.E.S. are members of the TESS POC who coordinated and scheduled the TESS science observations and conducted instrument planning. R.M., J.C.S., and J.D.T. are members of the SPOC who performed data calibration, light curve production, and transit planet detection. D.C., J.C., and S.N.Q. are members of the TSO who reviewed the data and performed planet candidate vetting. J.M.A., E.A., F.B., D.C., J.R.D.M., X.D., R.F.D., R.D., P.F., T.F., G.G., C.L., C.M., F.P., D.S., and S.U. are coinvestigators of the proposal, which provided the HARPS observations of the target and supported the interpretation of results. S.A., P.C., A.C., W.D.C., E.Go., I.G., P.K., E.K., J.J.L., N.N., H.L.M.O., E.P., C.M.P., H.R., L.M.S., J.Š., and V.V.E. are part of the KESPRINT consortium and contributed to the interpretation of the results. All authors contributed to the preparation of the paper. Data and materials availability: The TESS photometric observations are available at the Mikulski Archive for Space Telescopes (MAST) at https://exo.mast.stsci.edu under target name TOI 731.01. The raw HARPS spectroscopic data are available on the ESO Science Archive Facility http://archive.eso.org/cms.html under ESO program IDs 072.C-0488, 082.C-0718, 183.C-0437 (primary investigators: M. Mayor and X. Bonfils), and 1102.C-0339 (primary investigator: X. Bonfils). The ground-based photometry obtained by the LCO telescope and REM as well as the Gemini imaging data are available on the Exoplanet Follow-up Observing Program (ExoFOP) website https://exofop.ipac.caltech.edu/tess/ under target name TOI 731.01. The raw Gemini data are available at https://archive.gemini.edu/searchform under program ID GS-2021A-LP-105. The archival WASP data are available on the NASA Exoplanet Archive https://exoplanetarchive.ipac.caltech.edu/docs/SuperWASPMission.html under object name GJ 367. Our reduced RVs and activity indices are listed in tables S1 and S2 and in machine-readable form in data S1 and S2. The TLCM is available at www.transits.hu/. The authors declare no competing interests.

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