Three Long-period Transiting Giant Planets from TESS

Rafael Brahm; Solène Ulmer-Moll; Melissa J. Hobson; Andrés Jordán; Thomas Henning; Trifon Trifonov; Matías I. Jones; Martin Schlecker; Nestor Espinoza; Felipe I. Rojas; Pascal Torres; Paula Sarkis; Marcelo Tala; Jan Eberhardt; Diana Kossakowski; Diego J. Muñoz; Joel D. Hartman; Gavin Boyle; Vincent Suc; François Bouchy; Adrien Deline; Guillaume Chaverot; Nolan Grieves; Monika Lendl; Olga Suarez; Tristan Guillot; Amaury H.M.J. Triaud; Nicolas Crouzet; Georgina Dransfield; Ryan Cloutier; Khalid Barkaoui; Rick P. Schwarz; Chris Stockdale; Mallory Harris; Ismael Mireles; Phil Evans; Andrew W. Mann; Carl Ziegler; Diana Dragomir; Steven Villanueva; Christoph Mordasini; George Ricker; Roland Vanderspek; David W. Latham; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Michael Vezie; Allison Youngblood; Tansu Daylan; Karen A. Collins; Douglas A. Caldwell; David R. Ciardi; Enric Palle; Felipe Murgas

doi:10.3847/1538-3881/accadd

Three Long-period Transiting Giant Planets from TESS

Rafael Brahm, Solène Ulmer-Moll, Melissa J. Hobson, Andrés Jordán, Thomas Henning, Trifon Trifonov, Matías I. Jones, Martin Schlecker, Nestor Espinoza, Felipe I. Rojas, Pascal Torres, Paula Sarkis, Marcelo Tala, Jan Eberhardt, Diana Kossakowski, Diego J. Muñoz, Joel D. Hartman, Gavin Boyle, Vincent Suc, François BouchyAdrien Deline, Guillaume Chaverot, Nolan Grieves, Monika Lendl, Olga Suarez, Tristan Guillot, Amaury H.M.J. Triaud, Nicolas Crouzet, Georgina Dransfield, Ryan Cloutier, Khalid Barkaoui, Rick P. Schwarz, Chris Stockdale, Mallory Harris, Ismael Mireles, Phil Evans, Andrew W. Mann, Carl Ziegler, Diana Dragomir, Steven Villanueva, Christoph Mordasini, George Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Michael Vezie, Allison Youngblood, Tansu Daylan, Karen A. Collins, Douglas A. Caldwell, David R. Ciardi, Enric Palle, Felipe Murgas

Research output: Contribution to journal › Article › peer-review

Abstract

We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single-transit events in the light curves generated from the full-frame images of the Transiting Exoplanet Survey Satellite. Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of M _P = 0.30 ± 0.04 M _J, a radius of R _P = 1.00 ± 0.02 R _J, and a low-eccentricity orbit (e = 0.15 ± 0.05) with a period of P = 30.08364 ±0.00005 days. TOI 2338b has a mass of M _P = 5.98 ± 0.20 M _J, a radius of R _P = 1.00 ± 0.01 R _J, and a highly eccentric orbit (e = 0.676 ± 0.002) with a period of P = 22.65398 ± 0.00002 days. Finally, TOI 2589b has a mass of M _P = 3.50 ± 0.10 M _J, a radius of R _P = 1.08 ± 0.03 R _J, and an eccentric orbit (e = 0.522 ± 0.006) with a period of P = 61.6277 ± 0.0002 days. TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.

Original language	English
Article number	227
Journal	Astronomical Journal
Volume	165
Issue number	6
DOIs	https://doi.org/10.3847/1538-3881/accadd
State	Published - 1 Jun 2023
Externally published	Yes

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Brahm, R., Ulmer-Moll, S., Hobson, M. J., Jordán, A., Henning, T., Trifonov, T., Jones, M. I., Schlecker, M., Espinoza, N., Rojas, F. I., Torres, P., Sarkis, P., Tala, M., Eberhardt, J., Kossakowski, D., Muñoz, D. J., Hartman, J. D., Boyle, G., Suc, V., ... Murgas, F. (2023). Three Long-period Transiting Giant Planets from TESS. Astronomical Journal, 165(6), Article 227. https://doi.org/10.3847/1538-3881/accadd

@article{6b8ea584d93a4670a0b97a1f679410e2,

title = "Three Long-period Transiting Giant Planets from TESS",

abstract = "We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single-transit events in the light curves generated from the full-frame images of the Transiting Exoplanet Survey Satellite. Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of M P = 0.30 ± 0.04 M J, a radius of R P = 1.00 ± 0.02 R J, and a low-eccentricity orbit (e = 0.15 ± 0.05) with a period of P = 30.08364 ±0.00005 days. TOI 2338b has a mass of M P = 5.98 ± 0.20 M J, a radius of R P = 1.00 ± 0.01 R J, and a highly eccentric orbit (e = 0.676 ± 0.002) with a period of P = 22.65398 ± 0.00002 days. Finally, TOI 2589b has a mass of M P = 3.50 ± 0.10 M J, a radius of R P = 1.08 ± 0.03 R J, and an eccentric orbit (e = 0.522 ± 0.006) with a period of P = 61.6277 ± 0.0002 days. TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.",

author = "Rafael Brahm and Sol{\`e}ne Ulmer-Moll and Hobson, {Melissa J.} and Andr{\'e}s Jord{\'a}n and Thomas Henning and Trifon Trifonov and Jones, {Mat{\'i}as I.} and Martin Schlecker and Nestor Espinoza and Rojas, {Felipe I.} and Pascal Torres and Paula Sarkis and Marcelo Tala and Jan Eberhardt and Diana Kossakowski and Mu{\~n}oz, {Diego J.} and Hartman, {Joel D.} and Gavin Boyle and Vincent Suc and Fran{\c c}ois Bouchy and Adrien Deline and Guillaume Chaverot and Nolan Grieves and Monika Lendl and Olga Suarez and Tristan Guillot and Triaud, {Amaury H.M.J.} and Nicolas Crouzet and Georgina Dransfield and Ryan Cloutier and Khalid Barkaoui and Schwarz, {Rick P.} and Chris Stockdale and Mallory Harris and Ismael Mireles and Phil Evans and Mann, {Andrew W.} and Carl Ziegler and Diana Dragomir and Steven Villanueva and Christoph Mordasini and George Ricker and Roland Vanderspek and Latham, {David W.} and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Michael Vezie and Allison Youngblood and Tansu Daylan and Collins, {Karen A.} and Caldwell, {Douglas A.} and Ciardi, {David R.} and Enric Palle and Felipe Murgas",

note = "Funding Information: R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. A.J. acknowledges support from FONDECYT project 1210718. 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. -06-/5. 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. The contributions of S.U., F.B., A.D., G.C., N.G., and M.L. 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. The authors acknowledge the financial support of the SNSF. M.L. acknowledges support of the Swiss National Science Foundation under grant No. PCEFP2_194576. This research received funding from the European Research Council (ERC) under the European Union{\textquoteright}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). 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 publication was made possible through the support of an LSSTC Catalyst Fellowship to T.D., funded through grant 62192 from the John Templeton Foundation to LSST Corporation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of LSSTC or the John Templeton Foundation. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The ASTEP team acknowledges support from IPEV, PNRA, the Universit{\'e} C{\^o}te d{\textquoteright}Azur, the University of Birmingham, and ESA. 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. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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 research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding Information: R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. A.J. acknowledges support from FONDECYT project 1210718. 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. -06-/5. 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. The contributions of S.U., F.B., A.D., G.C., N.G., and M.L. 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. The authors acknowledge the financial support of the SNSF. M.L. acknowledges support of the Swiss National Science Foundation under grant No. PCEFP2_194576. This research received funding from the European Research Council (ERC) under the European Union{\textquoteright}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). 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 publication was made possible through the support of an LSSTC Catalyst Fellowship to T.D., funded through grant 62192 from the John Templeton Foundation to LSST Corporation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of LSSTC or the John Templeton Foundation. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The ASTEP team acknowledges support from IPEV, PNRA, the Universit{\'e} C{\^o}te d{\textquoteright}Azur, the University of Birmingham, and ESA. 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. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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 research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = jun,

day = "1",

doi = "10.3847/1538-3881/accadd",

language = "English",

volume = "165",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "6",

}

Brahm, R, Ulmer-Moll, S, Hobson, MJ, Jordán, A, Henning, T, Trifonov, T, Jones, MI, Schlecker, M, Espinoza, N, Rojas, FI, Torres, P, Sarkis, P, Tala, M, Eberhardt, J, Kossakowski, D, Muñoz, DJ, Hartman, JD, Boyle, G, Suc, V, Bouchy, F, Deline, A, Chaverot, G, Grieves, N, Lendl, M, Suarez, O, Guillot, T, Triaud, AHMJ, Crouzet, N, Dransfield, G, Cloutier, R, Barkaoui, K, Schwarz, RP, Stockdale, C, Harris, M, Mireles, I, Evans, P, Mann, AW, Ziegler, C, Dragomir, D, Villanueva, S, Mordasini, C, Ricker, G, Vanderspek, R, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Vezie, M, Youngblood, A, Daylan, T, Collins, KA, Caldwell, DA, Ciardi, DR, Palle, E & Murgas, F 2023, 'Three Long-period Transiting Giant Planets from TESS', Astronomical Journal, vol. 165, no. 6, 227. https://doi.org/10.3847/1538-3881/accadd

TY - JOUR

T1 - Three Long-period Transiting Giant Planets from TESS

AU - Brahm, Rafael

AU - Ulmer-Moll, Solène

AU - Hobson, Melissa J.

AU - Jordán, Andrés

AU - Henning, Thomas

AU - Trifonov, Trifon

AU - Jones, Matías I.

AU - Schlecker, Martin

AU - Espinoza, Nestor

AU - Rojas, Felipe I.

AU - Torres, Pascal

AU - Sarkis, Paula

AU - Tala, Marcelo

AU - Eberhardt, Jan

AU - Kossakowski, Diana

AU - Muñoz, Diego J.

AU - Hartman, Joel D.

AU - Boyle, Gavin

AU - Suc, Vincent

AU - Bouchy, François

AU - Deline, Adrien

AU - Chaverot, Guillaume

AU - Grieves, Nolan

AU - Lendl, Monika

AU - Suarez, Olga

AU - Guillot, Tristan

AU - Triaud, Amaury H.M.J.

AU - Crouzet, Nicolas

AU - Dransfield, Georgina

AU - Cloutier, Ryan

AU - Barkaoui, Khalid

AU - Schwarz, Rick P.

AU - Stockdale, Chris

AU - Harris, Mallory

AU - Mireles, Ismael

AU - Evans, Phil

AU - Mann, Andrew W.

AU - Ziegler, Carl

AU - Dragomir, Diana

AU - Villanueva, Steven

AU - Mordasini, Christoph

AU - Ricker, George

AU - Vanderspek, Roland

AU - Latham, David W.

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Vezie, Michael

AU - Youngblood, Allison

AU - Daylan, Tansu

AU - Collins, Karen A.

AU - Caldwell, Douglas A.

AU - Ciardi, David R.

AU - Palle, Enric

AU - Murgas, Felipe

N1 - Funding Information: R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. A.J. acknowledges support from FONDECYT project 1210718. 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. -06-/5. 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. The contributions of S.U., F.B., A.D., G.C., N.G., and M.L. 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. The authors acknowledge the financial support of the SNSF. M.L. acknowledges support of the Swiss National Science Foundation under grant No. 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 No. 803193/BEBOP) and from the Science and Technology Facilities Council (STFC; grant No. ST/S00193X/1). 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 publication was made possible through the support of an LSSTC Catalyst Fellowship to T.D., funded through grant 62192 from the John Templeton Foundation to LSST Corporation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of LSSTC or the John Templeton Foundation. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The ASTEP team acknowledges support from IPEV, PNRA, the Université Côte d’Azur, the University of Birmingham, and ESA. 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. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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 research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding Information: R.B. acknowledges support from FONDECYT project 11200751 and from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millenium Science Initiative. A.J. acknowledges support from FONDECYT project 1210718. 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. -06-/5. 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. The contributions of S.U., F.B., A.D., G.C., N.G., and M.L. 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. The authors acknowledge the financial support of the SNSF. M.L. acknowledges support of the Swiss National Science Foundation under grant No. 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 No. 803193/BEBOP) and from the Science and Technology Facilities Council (STFC; grant No. ST/S00193X/1). 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 publication was made possible through the support of an LSSTC Catalyst Fellowship to T.D., funded through grant 62192 from the John Templeton Foundation to LSST Corporation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of LSSTC or the John Templeton Foundation. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation. The ASTEP team acknowledges support from IPEV, PNRA, the Université Côte d’Azur, the University of Birmingham, and ESA. 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. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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 research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

PY - 2023/6/1

Y1 - 2023/6/1

N2 - We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single-transit events in the light curves generated from the full-frame images of the Transiting Exoplanet Survey Satellite. Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of M P = 0.30 ± 0.04 M J, a radius of R P = 1.00 ± 0.02 R J, and a low-eccentricity orbit (e = 0.15 ± 0.05) with a period of P = 30.08364 ±0.00005 days. TOI 2338b has a mass of M P = 5.98 ± 0.20 M J, a radius of R P = 1.00 ± 0.01 R J, and a highly eccentric orbit (e = 0.676 ± 0.002) with a period of P = 22.65398 ± 0.00002 days. Finally, TOI 2589b has a mass of M P = 3.50 ± 0.10 M J, a radius of R P = 1.08 ± 0.03 R J, and an eccentric orbit (e = 0.522 ± 0.006) with a period of P = 61.6277 ± 0.0002 days. TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.

AB - We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single-transit events in the light curves generated from the full-frame images of the Transiting Exoplanet Survey Satellite. Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of M P = 0.30 ± 0.04 M J, a radius of R P = 1.00 ± 0.02 R J, and a low-eccentricity orbit (e = 0.15 ± 0.05) with a period of P = 30.08364 ±0.00005 days. TOI 2338b has a mass of M P = 5.98 ± 0.20 M J, a radius of R P = 1.00 ± 0.01 R J, and a highly eccentric orbit (e = 0.676 ± 0.002) with a period of P = 22.65398 ± 0.00002 days. Finally, TOI 2589b has a mass of M P = 3.50 ± 0.10 M J, a radius of R P = 1.08 ± 0.03 R J, and an eccentric orbit (e = 0.522 ± 0.006) with a period of P = 61.6277 ± 0.0002 days. TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.

UR - http://www.scopus.com/inward/record.url?scp=85158071622&partnerID=8YFLogxK

U2 - 10.3847/1538-3881/accadd

DO - 10.3847/1538-3881/accadd

M3 - Article

AN - SCOPUS:85158071622

SN - 0004-6256

VL - 165

JO - Astronomical Journal

JF - Astronomical Journal

IS - 6

M1 - 227

ER -

Three Long-period Transiting Giant Planets from TESS

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