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TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Šubjak, J. and Endl, M. and Chaturvedi, P. and Karjalainen, R. and Cochran, W. D. and Esposito, M. and Gandolfi, D. and Lam, K. W. F. and Stassun, K. and Žák, J. and Lodieu, N. and Boffin, H. M. J. and MacQueen, P. J. and Hatzes, A. and Guenther, E. W. and Georgieva, I. and Grziwa, S. and Schmerling, H. and Skarka, M. and Blažek, M. and Karjalainen, M. and Špoková, M. and Isaacson, H. and Howard, A. W. and Burke, C. J. and Van Eylen, V. and Falk, B. and Fridlund, M. and Goffo, E. and Jenkins, J. M. and Korth, J. and Lissauer, J. J. and Livingston, J. H. and Luque, R. and Muresan, A. and Osborn, H. P. and Pallé, E. and Persson, C. M. and Redfield, S. and Ricker, G. R. and Seager, S. and Serrano, L. M. and Smith, A. M. S. and Kabáth, P. (2022) TOI-1268b: The youngest hot Saturn-mass transiting exoplanet. Astronomy and Astrophysics, 662 . Art. No. A107. ISSN 0004-6361. doi:10.1051/0004-6361/202142883.

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We report the discovery of TOI-1268b, a transiting Saturn-mass planet from the TESS space mission. With an age of less than 1 Gyr, derived from various age indicators, TOI-1268b is the youngest Saturn-mass planet known to date; it contributes to the small sample of well-characterised young planets. It has an orbital period of P = 8.1577080 ± 0.0000044 days, and transits an early K-dwarf star with a mass of M_* = 0.96 ± 0.04 M_⊙, a radius of R_* = 0.92 ± 0.06 R_⊙, an effective temperature of T_(eff) = 5300 ± 100 K, and a metallicity of 0.36 ± 0.06 dex. By combining TESS photometry with high-resolution spectra acquired with the Tull spectrograph at the McDonald Observatory, and the high-resolution spectrographs at the Tautenburg and Ondřejov Observatories, we measured a planetary mass of Mₚ = 96.4 ± 8.3 M_⊕ and a radius of Rₚ = 9.1 ± 0.6 R_⊕. TOI-1268 is an ideal system for studying the role of star-planet tidal interactions for non-inflated Saturn-mass planets. We used system parameters derived in this paper to constrain the planet’s tidal quality factor to the range of 10^(4.5–5.3). When compared with the sample of other non-inflated Saturn-mass planets, TOI-1268b is one of the best candidates for transmission spectroscopy studies.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Šubjak, J.0000-0002-5313-9722
Endl, M.0000-0002-7714-6310
Chaturvedi, P.0000-0002-1887-1192
Cochran, W. D.0000-0001-9662-3496
Esposito, M.0000-0002-6893-4534
Gandolfi, D.0000-0001-8627-9628
Lam, K. W. F.0000-0002-9910-6088
Stassun, K.0000-0002-3481-9052
Žák, J.0000-0003-3793-7254
Lodieu, N.0000-0002-3612-8968
Boffin, H. M. J.0000-0002-9486-4840
Hatzes, A.0000-0002-3404-8358
Guenther, E. W.0000-0002-9130-6747
Georgieva, I.0000-0002-5056-1899
Grziwa, S.0000-0003-3370-4058
Skarka, M.0000-0002-7602-0046
Karjalainen, M.0000-0003-0751-3231
Isaacson, H.0000-0002-0531-1073
Howard, A. W.0000-0001-8638-0320
Burke, C. J.0000-0002-7754-9486
Van Eylen, V.0000-0001-5542-8870
Fridlund, M.0000-0002-0855-8426
Goffo, E.0000-0001-9670-961X
Jenkins, J. M.0000-0002-4715-9460
Korth, J.0000-0002-0076-6239
Lissauer, J. J.0000-0001-6513-1659
Livingston, J. H.0000-0002-4881-3620
Luque, R.0000-0002-4671-2957
Osborn, H. P.0000-0002-4047-4724
Pallé, E.0000-0003-0987-1593
Persson, C. M.0000-0003-1257-5146
Redfield, S.0000-0003-3786-3486
Ricker, G. R.0000-0003-2058-6662
Seager, S.0000-0002-6892-6948
Serrano, L. M.0000-0001-9211-3691
Smith, A. M. S.0000-0002-2386-4341
Kabáth, P.0000-0002-1623-5352
Additional Information:© ESO 2022. Received: 10 December 2021 Accepted: 16 February 2022. This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterisation and research of exoplanets discovered with space-based missions ( J.S., R.K., M.S., M.K. and P.K. would like to acknowledge support from MSMT grant LTT-20015. J.S. and P.K. acknowledge a travel budget from ERASMUS+ grant 2020-1-CZ01-KA203-078200. J.S. would like to acknowledge support from the Grant Agency of Charles University: GAUK No. 314421. P.C. acknowledges the generous support from Deutsche Forschungsgemeinschaft (DFG) of the grant CH 2636/1-1. We are grateful for the generous support by Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. N.L. was financially supported by the Ministerio de Economia y Competitividad and the Fondo Europeo de Desarrollo Regional (FEDER) under AYA2015-69350-C3-2-P. E.G. is thankful for the generously supported by the by the Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft and the staff of the Alfred-Jensch-Teleskop. I.G., M.F., J.K., and C.M.P., gratefully acknowledge the support of the Swedish National Space Agency (DNR 174/18, 2020-00104, 65/19). This work was supported by JSPS KAKENHI grant number 20K14518. R.L. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). L.M.S. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. 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 includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work has made use of data from the European Space Agency (ESA) mission Gaia (, processed by the Gaia Data Processing and Analysis Consortium (DPAC, Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported by the Spanish MINECO through grant AyA2017-84089. VOSA has been partially updated by using funding from the European Union’s Horizon 2020 Research and Innovation Programme, under Grant Agreement no 776403 (EXOPLANETS-A). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Group:Astronomy Department
Funding AgencyGrant Number
Ministry of Education, Youth and Sports (Czech Republic)LTT-20015
Charles University Grant Agency (GA UK)314421
Deutsche Forschungsgemeinschaft (DFG)CH 2636/1-1
Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale GesellschaftUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)RA714/14-1
Deutsche Forschungsgemeinschaft (DFG)SPP 1992
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2015-69350-C3-2-P
European Regional Development FundUNSPECIFIED
Swedish National Space AgencyDNR 174/18, 2020-00104, 65/19
Japan Society for the Promotion of Science (JSPS)20K14518
Ministerio de Ciencia e Innovación (MICINN)PID2019-109522GB-C52
Severo OchoaSEV-2017-0709
CRT foundation2018.2323
Swiss National Science Foundation (SNSF)UNSPECIFIED
NASANAS 5-26555
Gaia Multilateral AgreementUNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AyA2017-84089
European Research Council (ERC)776403
Subject Keywords:techniques: spectroscopic / techniques: radial velocities / techniques: photometric / planetary systems / planets and satellites: gaseous planets / planets and satellites: atmospheres
Record Number:CaltechAUTHORS:20220721-8563000
Persistent URL:
Official Citation:TOI-1268b: The youngest hot Saturn-mass transiting exoplanet J. Šubjak, M. Endl, P. Chaturvedi, R. Karjalainen, W. D. Cochran, M. Esposito, D. Gandolfi, K. W. F. Lam, K. Stassun, J. Žák, N. Lodieu, H. M. J. Boffin, P. J. MacQueen, A. Hatzes, E. W. Guenther, I. Georgieva, S. Grziwa, H. Schmerling, M. Skarka, M. Blažek, M. Karjalainen, M. Špoková, H. Isaacson, A. W. Howard, C. J. Burke, V. Van Eylen, B. Falk, M. Fridlund, E. Goffo, J. M. Jenkins, J. Korth, J. J. Lissauer, J. H. Livingston, R. Luque, A. Muresan, H. P. Osborn, E. Pallé, C. M. Persson, S. Redfield, G. R. Ricker, S. Seager, L. M. Serrano, A. M. S. Smith and P. Kabáth A&A, 662 (2022) A107 DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115737
Deposited By: George Porter
Deposited On:22 Jul 2022 15:29
Last Modified:22 Jul 2022 15:29

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