TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica

Melissa J. Hobson; Trifon Trifonov; Thomas Henning; Andrés Jordán; Felipe Rojas; Nestor Espinoza; Rafael Brahm; Jan Eberhardt; Matías I. Jones; Djamel Mekarnia; Diana Kossakowski; Martin Schlecker; Marcelo Tala Pinto; Pascal José Torres Miranda; Lyu Abe; Khalid Barkaoui; Philippe Bendjoya; François Bouchy; Marco Buttu; Ilaria Carleo; Karen A. Collins; Knicole D. Colón; Nicolas Crouzet; Diana Dragomir; Georgina Dransfield; Thomas Gasparetto; Robert F. Goeke; Tristan Guillot; Maximilian N. Günther; Saburo Howard; Jon M. Jenkins; Judith Korth; David W. Latham; Monika Lendl; Jack J. Lissauer; Christopher R. Mann; Ismael Mireles; George R. Ricker; Sophie Saesen; Richard P. Schwarz; S. Seager; Ramotholo Sefako; Avi Shporer; Chris Stockdale; Olga Suarez; Thiam-Guan Tan; Amaury H. M. J. Triaud; Solène Ulmer-Moll; Roland Vanderspek; Joshua N. Winn; Bill Wohler; George Zhou

TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica

Melissa J. Hobson, Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, Jan Eberhardt, Matías I. Jones, Djamel Mekarnia, Diana Kossakowski, Martin Schlecker, Marcelo Tala Pinto, Pascal José Torres Miranda, Lyu Abe, Khalid Barkaoui, Philippe Bendjoya, François Bouchy, Marco Buttu, Ilaria CarleoKaren A. Collins, Knicole D. Colón, Nicolas Crouzet, Diana Dragomir, Georgina Dransfield, Thomas Gasparetto, Robert F. Goeke, Tristan Guillot, Maximilian N. Günther, Saburo Howard, Jon M. Jenkins, Judith Korth, David W. Latham, Monika Lendl, Jack J. Lissauer, Christopher R. Mann, Ismael Mireles, George R. Ricker, Sophie Saesen, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Chris Stockdale, Olga Suarez, Thiam-Guan Tan, Amaury H. M. J. Triaud, Solène Ulmer-Moll, Roland Vanderspek, Joshua N. Winn, Bill Wohler, George Zhou

Physics and Astronomy

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Abstract

We present the spectroscopic confirmation and precise mass measurement of the warm giant planet TOI-199 b. This planet was first identified in TESS photometry and confirmed using ground-based photometry from ASTEP in Antarctica including a full 6.5h long transit, PEST, Hazelwood, and LCO; space photometry from NEOSSat; and radial velocities (RVs) from FEROS, HARPS, CORALIE, and CHIRON. Orbiting a late G-type star, TOI-199\,b has a 104.854^+0.001_−0.002d period, a mass of 0.17±0.02M_J, and a radius of 0.810±0.005R_J. It is the first warm exo-Saturn with a precisely determined mass and radius. The TESS and ASTEP transits show strong transit timing variations, pointing to the existence of a second planet in the system. The joint analysis of the RVs and TTVs provides a unique solution for the non-transiting companion TOI-199 c, which has a period of 273.69^+0.26_−0.22d and an estimated mass of 0.28^+0.02_−0.01M_J. This period places it within the conservative Habitable Zone.

Original language	English
Article number	201
Number of pages	26
Journal	The Astronomical Journal
Volume	166
Issue number	5
Early online date	18 Oct 2023
Publication status	Published - 1 Nov 2023

Bibliographical note

Acknowledgments
This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. The specific observations analyzed can be accessed via DOI: 10.17909/cbph-wd44.

This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. We acknowledge the use of public TESS Alert data from the 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.

Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 0101.C-0510, 0102.C-0451, 0104.C-0413, 106.21ER.001, 0102.A-9003, 0102.A-9006, 0102.A-9011, 0102.A-9029, 0103.A-9008, and 0104.A-9007.

This research has made use of the Spanish Virtual Observatory (https://svo.cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00.

T.T. acknowledges support by the DFG Research Unit FOR 2544 "Blue Planets around Red Stars" project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program "VIHREN-2021" project No. KP-06-DV/5.

A.J., R.B., and M.H. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT Project 1120075 and from project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative. This work was funded by the Data Observatory Foundation.

The results reported herein benefited from collaborations and/or information exchange within the program "Alien Earths" (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate.

This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC).

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. K.A.C. acknowledges support from the TESS mission via subaward s3449 from MIT.

The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation.

The contributions of M.L., S.U., and S.S. have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576.

This research received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement n° 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1).

D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136.

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.

J.K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945).

M.T.P. acknowledges support of the ANID-Fondecyt Postdoctoral fellowship no. 3210253.

Facilities: TESS - , ASTEP - , LCOGT - Las Cumbres Observatory Global Telescope, PEST - , NEOSSat - , Hazelwood - , Max Planck:2.2m (FEROS) - , ESO:3.6m (HARPS) - , Euler1.2m (CORALIE) - , CTIO:1.5m (CHIRON - ), and SOAR (HRCam) - .

Software: tesseract (F. Rojas et al. (2023, in preparation)), CERES (Brahm et al. 2017a), juliet (Espinoza et al. 2019), ZASPE (Brahm et al. 2017b), radvel (Fulton et al. 2018), emcee (Foreman-Mackey et al. 2013), MultiNest (Feroz et al. 2009), PyMultiNest (Buchner et al. 2014), batman (Kreidberg 2015), celerite (Foreman-Mackey et al. 2017), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013), Exo-Striker (Trifonov 2019), EqTide (Barnes 2017), and limb-darkening (Espinoza & Jordán 2015).

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Hobson, M. J., Trifonov, T., Henning, T., Jordán, A., Rojas, F., Espinoza, N., Brahm, R., Eberhardt, J., Jones, M. I., Mekarnia, D., Kossakowski, D., Schlecker, M., Pinto, M. T., Miranda, P. J. T., Abe, L., Barkaoui, K., Bendjoya, P., Bouchy, F., Buttu, M., ... Zhou, G. (2023). TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica. The Astronomical Journal, 166(5), Article 201. http://10.3847/1538-3881/acfc1d

@article{5a1e67e183c54b4ba9a0f9c50bb95f72,

title = "TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica",

abstract = "We present the spectroscopic confirmation and precise mass measurement of the warm giant planet TOI-199 b. This planet was first identified in TESS photometry and confirmed using ground-based photometry from ASTEP in Antarctica including a full 6.5h long transit, PEST, Hazelwood, and LCO; space photometry from NEOSSat; and radial velocities (RVs) from FEROS, HARPS, CORALIE, and CHIRON. Orbiting a late G-type star, TOI-199\,b has a 104.854+0.001−0.002d period, a mass of 0.17±0.02MJ, and a radius of 0.810±0.005RJ. It is the first warm exo-Saturn with a precisely determined mass and radius. The TESS and ASTEP transits show strong transit timing variations, pointing to the existence of a second planet in the system. The joint analysis of the RVs and TTVs provides a unique solution for the non-transiting companion TOI-199 c, which has a period of 273.69+0.26−0.22d and an estimated mass of 0.28+0.02−0.01MJ. This period places it within the conservative Habitable Zone.",

author = "Hobson, {Melissa J.} and Trifon Trifonov and Thomas Henning and Andr{\'e}s Jord{\'a}n and Felipe Rojas and Nestor Espinoza and Rafael Brahm and Jan Eberhardt and Jones, {Mat{\'i}as I.} and Djamel Mekarnia and Diana Kossakowski and Martin Schlecker and Pinto, {Marcelo Tala} and Miranda, {Pascal Jos{\'e} Torres} and Lyu Abe and Khalid Barkaoui and Philippe Bendjoya and Fran{\c c}ois Bouchy and Marco Buttu and Ilaria Carleo and Collins, {Karen A.} and Col{\'o}n, {Knicole D.} and Nicolas Crouzet and Diana Dragomir and Georgina Dransfield and Thomas Gasparetto and Goeke, {Robert F.} and Tristan Guillot and G{\"u}nther, {Maximilian N.} and Saburo Howard and Jenkins, {Jon M.} and Judith Korth and Latham, {David W.} and Monika Lendl and Lissauer, {Jack J.} and Mann, {Christopher R.} and Ismael Mireles and Ricker, {George R.} and Sophie Saesen and Schwarz, {Richard P.} and S. Seager and Ramotholo Sefako and Avi Shporer and Chris Stockdale and Olga Suarez and Thiam-Guan Tan and Triaud, {Amaury H. M. J.} and Sol{\`e}ne Ulmer-Moll and Roland Vanderspek and Winn, {Joshua N.} and Bill Wohler and George Zhou",

note = "Acknowledgments This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. The specific observations analyzed can be accessed via DOI: 10.17909/cbph-wd44. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. We acknowledge the use of public TESS Alert data from the 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. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 0101.C-0510, 0102.C-0451, 0104.C-0413, 106.21ER.001, 0102.A-9003, 0102.A-9006, 0102.A-9011, 0102.A-9029, 0103.A-9008, and 0104.A-9007. This research has made use of the Spanish Virtual Observatory (https://svo.cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. T.T. acknowledges support by the DFG Research Unit FOR 2544 {"}Blue Planets around Red Stars{"} project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program {"}VIHREN-2021{"} project No. KP-06-DV/5. A.J., R.B., and M.H. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT Project 1120075 and from project IC120009 {"}Millennium Institute of Astrophysics (MAS){"} of the Millenium Science Initiative. This work was funded by the Data Observatory Foundation. The results reported herein benefited from collaborations and/or information exchange within the program {"}Alien Earths{"} (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC). 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. K.A.C. acknowledges support from the TESS mission via subaward s3449 from MIT. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The contributions of M.L., S.U., and S.S. have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. This research received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement n° 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1). D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136. 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. J.K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945). M.T.P. acknowledges support of the ANID-Fondecyt Postdoctoral fellowship no. 3210253. Facilities: TESS - , ASTEP - , LCOGT - Las Cumbres Observatory Global Telescope, PEST - , NEOSSat - , Hazelwood - , Max Planck:2.2m (FEROS) - , ESO:3.6m (HARPS) - , Euler1.2m (CORALIE) - , CTIO:1.5m (CHIRON - ), and SOAR (HRCam) - . Software: tesseract (F. Rojas et al. (2023, in preparation)), CERES (Brahm et al. 2017a), juliet (Espinoza et al. 2019), ZASPE (Brahm et al. 2017b), radvel (Fulton et al. 2018), emcee (Foreman-Mackey et al. 2013), MultiNest (Feroz et al. 2009), PyMultiNest (Buchner et al. 2014), batman (Kreidberg 2015), celerite (Foreman-Mackey et al. 2017), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013), Exo-Striker (Trifonov 2019), EqTide (Barnes 2017), and limb-darkening (Espinoza & Jord{\'a}n 2015).",

year = "2023",

month = nov,

day = "1",

language = "English",

volume = "166",

journal = "The Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "5",

}

Hobson, MJ, Trifonov, T, Henning, T, Jordán, A, Rojas, F, Espinoza, N, Brahm, R, Eberhardt, J, Jones, MI, Mekarnia, D, Kossakowski, D, Schlecker, M, Pinto, MT, Miranda, PJT, Abe, L, Barkaoui, K, Bendjoya, P, Bouchy, F, Buttu, M, Carleo, I, Collins, KA, Colón, KD, Crouzet, N, Dragomir, D, Dransfield, G, Gasparetto, T, Goeke, RF, Guillot, T, Günther, MN, Howard, S, Jenkins, JM, Korth, J, Latham, DW, Lendl, M, Lissauer, JJ, Mann, CR, Mireles, I, Ricker, GR, Saesen, S, Schwarz, RP, Seager, S, Sefako, R, Shporer, A, Stockdale, C, Suarez, O, Tan, T-G, Triaud, AHMJ, Ulmer-Moll, S, Vanderspek, R, Winn, JN, Wohler, B & Zhou, G 2023, 'TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica', The Astronomical Journal, vol. 166, no. 5, 201. <http://10.3847/1538-3881/acfc1d>

TY - JOUR

T1 - TOI-199 b

T2 - A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica

AU - Hobson, Melissa J.

AU - Trifonov, Trifon

AU - Henning, Thomas

AU - Jordán, Andrés

AU - Rojas, Felipe

AU - Espinoza, Nestor

AU - Brahm, Rafael

AU - Eberhardt, Jan

AU - Jones, Matías I.

AU - Mekarnia, Djamel

AU - Kossakowski, Diana

AU - Schlecker, Martin

AU - Pinto, Marcelo Tala

AU - Miranda, Pascal José Torres

AU - Abe, Lyu

AU - Barkaoui, Khalid

AU - Bendjoya, Philippe

AU - Bouchy, François

AU - Buttu, Marco

AU - Carleo, Ilaria

AU - Collins, Karen A.

AU - Colón, Knicole D.

AU - Crouzet, Nicolas

AU - Dragomir, Diana

AU - Dransfield, Georgina

AU - Gasparetto, Thomas

AU - Goeke, Robert F.

AU - Guillot, Tristan

AU - Günther, Maximilian N.

AU - Howard, Saburo

AU - Jenkins, Jon M.

AU - Korth, Judith

AU - Latham, David W.

AU - Lendl, Monika

AU - Lissauer, Jack J.

AU - Mann, Christopher R.

AU - Mireles, Ismael

AU - Ricker, George R.

AU - Saesen, Sophie

AU - Schwarz, Richard P.

AU - Seager, S.

AU - Sefako, Ramotholo

AU - Shporer, Avi

AU - Stockdale, Chris

AU - Suarez, Olga

AU - Tan, Thiam-Guan

AU - Triaud, Amaury H. M. J.

AU - Ulmer-Moll, Solène

AU - Vanderspek, Roland

AU - Winn, Joshua N.

AU - Wohler, Bill

AU - Zhou, George

N1 - Acknowledgments This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. The specific observations analyzed can be accessed via DOI: 10.17909/cbph-wd44. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. We acknowledge the use of public TESS Alert data from the 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. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programs 0101.C-0510, 0102.C-0451, 0104.C-0413, 106.21ER.001, 0102.A-9003, 0102.A-9006, 0102.A-9011, 0102.A-9029, 0103.A-9008, and 0104.A-9007. This research has made use of the Spanish Virtual Observatory (https://svo.cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. T.T. acknowledges support by the DFG Research Unit FOR 2544 "Blue Planets around Red Stars" project No. KU 3625/2-1. T.T. further acknowledges support by the BNSF program "VIHREN-2021" project No. KP-06-DV/5. A.J., R.B., and M.H. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT Project 1120075 and from project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative. This work was funded by the Data Observatory Foundation. The results reported herein benefited from collaborations and/or information exchange within the program "Alien Earths" (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. This work makes use of observations from the ASTEP telescope. ASTEP benefited from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station program, from OCA, INSU, Idex UCAJEDI (ANR- 15-IDEX-01) and ESA through the Science Faculty of the European Space Research and Technology Centre (ESTEC). 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. K.A.C. acknowledges support from the TESS mission via subaward s3449 from MIT. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The contributions of M.L., S.U., and S.S. have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. This research received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement n° 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1). D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136. 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. J.K. gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020-00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017-04945). M.T.P. acknowledges support of the ANID-Fondecyt Postdoctoral fellowship no. 3210253. Facilities: TESS - , ASTEP - , LCOGT - Las Cumbres Observatory Global Telescope, PEST - , NEOSSat - , Hazelwood - , Max Planck:2.2m (FEROS) - , ESO:3.6m (HARPS) - , Euler1.2m (CORALIE) - , CTIO:1.5m (CHIRON - ), and SOAR (HRCam) - . Software: tesseract (F. Rojas et al. (2023, in preparation)), CERES (Brahm et al. 2017a), juliet (Espinoza et al. 2019), ZASPE (Brahm et al. 2017b), radvel (Fulton et al. 2018), emcee (Foreman-Mackey et al. 2013), MultiNest (Feroz et al. 2009), PyMultiNest (Buchner et al. 2014), batman (Kreidberg 2015), celerite (Foreman-Mackey et al. 2017), AstroImageJ (Collins et al. 2017), TAPIR (Jensen 2013), Exo-Striker (Trifonov 2019), EqTide (Barnes 2017), and limb-darkening (Espinoza & Jordán 2015).

PY - 2023/11/1

Y1 - 2023/11/1

N2 - We present the spectroscopic confirmation and precise mass measurement of the warm giant planet TOI-199 b. This planet was first identified in TESS photometry and confirmed using ground-based photometry from ASTEP in Antarctica including a full 6.5h long transit, PEST, Hazelwood, and LCO; space photometry from NEOSSat; and radial velocities (RVs) from FEROS, HARPS, CORALIE, and CHIRON. Orbiting a late G-type star, TOI-199\,b has a 104.854+0.001−0.002d period, a mass of 0.17±0.02MJ, and a radius of 0.810±0.005RJ. It is the first warm exo-Saturn with a precisely determined mass and radius. The TESS and ASTEP transits show strong transit timing variations, pointing to the existence of a second planet in the system. The joint analysis of the RVs and TTVs provides a unique solution for the non-transiting companion TOI-199 c, which has a period of 273.69+0.26−0.22d and an estimated mass of 0.28+0.02−0.01MJ. This period places it within the conservative Habitable Zone.

AB - We present the spectroscopic confirmation and precise mass measurement of the warm giant planet TOI-199 b. This planet was first identified in TESS photometry and confirmed using ground-based photometry from ASTEP in Antarctica including a full 6.5h long transit, PEST, Hazelwood, and LCO; space photometry from NEOSSat; and radial velocities (RVs) from FEROS, HARPS, CORALIE, and CHIRON. Orbiting a late G-type star, TOI-199\,b has a 104.854+0.001−0.002d period, a mass of 0.17±0.02MJ, and a radius of 0.810±0.005RJ. It is the first warm exo-Saturn with a precisely determined mass and radius. The TESS and ASTEP transits show strong transit timing variations, pointing to the existence of a second planet in the system. The joint analysis of the RVs and TTVs provides a unique solution for the non-transiting companion TOI-199 c, which has a period of 273.69+0.26−0.22d and an estimated mass of 0.28+0.02−0.01MJ. This period places it within the conservative Habitable Zone.

M3 - Article

SN - 0004-6256

VL - 166

JO - The Astronomical Journal

JF - The Astronomical Journal

IS - 5

M1 - 201

ER -

TOI-199 b: A well-characterized 100-day transiting warm giant planet with TTVs seen from Antarctica

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