Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Ilaria Carleo; Oscar Barrágan; Carina M. Persson; Malcolm Fridlund; Kristine W.F. Lam; Sergio Messina; Davide Gandolfi; Alexis M.S. Smith; Marshall C. Johnson; William Cochran; Hannah L.M. Osborne; Rafael Brahm; David R. Ciardi; Karen A. Collins; Mark E. Everett; Steven Giacalone; Eike W. Guenther; Artie Hatzes; Coel Hellier; Jonathan Horner; Petr Kabáth; Judith Korth; Phillip Macqueen; Thomas Masseron; Felipe Murgas; Grzegorz Nowak; Joseph E. Rodriguez; Cristilyn N. Watkins; Rob Wittenmyer; George Zhou; Carl Ziegler; Allyson Bieryla; Patricia T. Boyd; Catherine A. Clark; Courtney D. Dressing; Jason D. Eastman; Jan Eberhardt; Michael Endl; Nestor Espinoza; Michael Fausnaugh; Natalia M. Guerrero; Thomas Henning; Katharine Hesse; Melissa J. Hobson; Steve B. Howell; Andrés Jordán; David W. Latham; Michael B. Lund; Ismael Mireles; Norio Narita; Marcelo Tala Pinto; Teznie Pugh; Samuel N. Quinn; George Ricker; David R. Rodriguez; Felipe I. Rojas; Mark E. Rose; Alexander Rudat; Paula Sarkis; Arjun B. Savel; Martin Schlecker; Richard P. Schwarz; Sara Seager; Avi Shporer; Jeffrey C. Smith; Keivan G. Stassun; Chris Stockdale; Trifon Trifonov; Roland Vanderspek; Joshua N. Winn; Duncan Wright

doi:10.1051/0004-6361/202451313

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Ilaria Carleo, Oscar Barrágan, Carina M. Persson, Malcolm Fridlund, Kristine W.F. Lam, Sergio Messina, Davide Gandolfi, Alexis M.S. Smith, Marshall C. Johnson, William Cochran, Hannah L.M. Osborne, Rafael Brahm, David R. Ciardi, Karen A. Collins, Mark E. Everett, Steven Giacalone, Eike W. Guenther, Artie Hatzes, Coel Hellier, Jonathan HornerPetr Kabáth, Judith Korth, Phillip Macqueen, Thomas Masseron, Felipe Murgas, Grzegorz Nowak, Joseph E. Rodriguez, Cristilyn N. Watkins, Rob Wittenmyer, George Zhou, Carl Ziegler, Allyson Bieryla, Patricia T. Boyd, Catherine A. Clark, Courtney D. Dressing, Jason D. Eastman, Jan Eberhardt, Michael Endl, Nestor Espinoza, Michael Fausnaugh, Natalia M. Guerrero, Thomas Henning, Katharine Hesse, Melissa J. Hobson, Steve B. Howell, Andrés Jordán, David W. Latham, Michael B. Lund, Ismael Mireles, Norio Narita, Marcelo Tala Pinto, Teznie Pugh, Samuel N. Quinn, George Ricker, David R. Rodriguez, Felipe I. Rojas, Mark E. Rose, Alexander Rudat, Paula Sarkis, Arjun B. Savel, Martin Schlecker, Richard P. Schwarz, Sara Seager, Avi Shporer, Jeffrey C. Smith, Keivan G. Stassun, Chris Stockdale, Trifon Trifonov, Roland Vanderspek, Joshua N. Winn, Duncan Wright

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Resumen

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of P_b = 5.8 days, a mass of M_b = 0.9 M_J, and a radius of R_b = 1.3 R_J, with a planetary density of 0.477 g cm^-3. TOI-2485 b has an orbital period of P_b = 11.2 days, a mass of M_b = 2.4 M_J, and a radius of R_b = 1.1 R_J with a density of 2.36 g cm^-3. Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.

Idioma original	Inglés
Número de artículo	A18
Publicación	Astronomy and Astrophysics
Volumen	690
DOI	https://doi.org/10.1051/0004-6361/202451313
Estado	Publicada - 1 oct. 2024
Publicado de forma externa	Sí

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Carleo, I., Barrágan, O., Persson, C. M., Fridlund, M., Lam, K. W. F., Messina, S., Gandolfi, D., Smith, A. M. S., Johnson, M. C., Cochran, W., Osborne, H. L. M., Brahm, R., Ciardi, D. R., Collins, K. A., Everett, M. E., Giacalone, S., Guenther, E. W., Hatzes, A., Hellier, C., ... Wright, D. (2024). Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b. Astronomy and Astrophysics, 690, Artículo A18. https://doi.org/10.1051/0004-6361/202451313

@article{3c16075a58c043b68a6e4e5bbf898ee3,

title = "Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b",

abstract = "Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb = 5.8 days, a mass of Mb = 0.9 MJ, and a radius of Rb = 1.3 RJ, with a planetary density of 0.477 g cm-3. TOI-2485 b has an orbital period of Pb = 11.2 days, a mass of Mb = 2.4 MJ, and a radius of Rb = 1.1 RJ with a density of 2.36 g cm-3. Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.",

keywords = "Planets and satellites: detection, Planets and satellites: gaseous planets",

author = "Ilaria Carleo and Oscar Barr{\'a}gan and Persson, {Carina M.} and Malcolm Fridlund and Lam, {Kristine W.F.} and Sergio Messina and Davide Gandolfi and Smith, {Alexis M.S.} and Johnson, {Marshall C.} and William Cochran and Osborne, {Hannah L.M.} and Rafael Brahm and Ciardi, {David R.} and Collins, {Karen A.} and Everett, {Mark E.} and Steven Giacalone and Guenther, {Eike W.} and Artie Hatzes and Coel Hellier and Jonathan Horner and Petr Kab{\'a}th and Judith Korth and Phillip Macqueen and Thomas Masseron and Felipe Murgas and Grzegorz Nowak and Rodriguez, {Joseph E.} and Watkins, {Cristilyn N.} and Rob Wittenmyer and George Zhou and Carl Ziegler and Allyson Bieryla and Boyd, {Patricia T.} and Clark, {Catherine A.} and Dressing, {Courtney D.} and Eastman, {Jason D.} and Jan Eberhardt and Michael Endl and Nestor Espinoza and Michael Fausnaugh and Guerrero, {Natalia M.} and Thomas Henning and Katharine Hesse and Hobson, {Melissa J.} and Howell, {Steve B.} and Andr{\'e}s Jord{\'a}n and Latham, {David W.} and Lund, {Michael B.} and Ismael Mireles and Norio Narita and {Tala Pinto}, Marcelo and Teznie Pugh and Quinn, {Samuel N.} and George Ricker and Rodriguez, {David R.} and Rojas, {Felipe I.} and Rose, {Mark E.} and Alexander Rudat and Paula Sarkis and Savel, {Arjun B.} and Martin Schlecker and Schwarz, {Richard P.} and Sara Seager and Avi Shporer and Smith, {Jeffrey C.} and Stassun, {Keivan G.} and Chris Stockdale and Trifon Trifonov and Roland Vanderspek and Winn, {Joshua N.} and Duncan Wright",

note = "Publisher Copyright: {\textcopyright} The Authors 2024.",

year = "2024",

month = oct,

day = "1",

doi = "10.1051/0004-6361/202451313",

language = "English",

volume = "690",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Carleo, I, Barrágan, O, Persson, CM, Fridlund, M, Lam, KWF, Messina, S, Gandolfi, D, Smith, AMS, Johnson, MC, Cochran, W, Osborne, HLM, Brahm, R, Ciardi, DR, Collins, KA, Everett, ME, Giacalone, S, Guenther, EW, Hatzes, A, Hellier, C, Horner, J, Kabáth, P, Korth, J, Macqueen, P, Masseron, T, Murgas, F, Nowak, G, Rodriguez, JE, Watkins, CN, Wittenmyer, R, Zhou, G, Ziegler, C, Bieryla, A, Boyd, PT, Clark, CA, Dressing, CD, Eastman, JD, Eberhardt, J, Endl, M, Espinoza, N, Fausnaugh, M, Guerrero, NM, Henning, T, Hesse, K, Hobson, MJ, Howell, SB, Jordán, A, Latham, DW, Lund, MB, Mireles, I, Narita, N, Tala Pinto, M, Pugh, T, Quinn, SN, Ricker, G, Rodriguez, DR, Rojas, FI, Rose, ME, Rudat, A, Sarkis, P, Savel, AB, Schlecker, M, Schwarz, RP, Seager, S, Shporer, A, Smith, JC, Stassun, KG, Stockdale, C, Trifonov, T, Vanderspek, R, Winn, JN & Wright, D 2024, 'Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b', Astronomy and Astrophysics, vol. 690, A18. https://doi.org/10.1051/0004-6361/202451313

TY - JOUR

T1 - Mass determination of two Jupiter-sized planets orbiting slightly evolved stars

T2 - TOI-2420 b and TOI-2485 b

AU - Carleo, Ilaria

AU - Barrágan, Oscar

AU - Persson, Carina M.

AU - Fridlund, Malcolm

AU - Lam, Kristine W.F.

AU - Messina, Sergio

AU - Gandolfi, Davide

AU - Smith, Alexis M.S.

AU - Johnson, Marshall C.

AU - Cochran, William

AU - Osborne, Hannah L.M.

AU - Brahm, Rafael

AU - Ciardi, David R.

AU - Collins, Karen A.

AU - Everett, Mark E.

AU - Giacalone, Steven

AU - Guenther, Eike W.

AU - Hatzes, Artie

AU - Hellier, Coel

AU - Horner, Jonathan

AU - Kabáth, Petr

AU - Korth, Judith

AU - Macqueen, Phillip

AU - Masseron, Thomas

AU - Murgas, Felipe

AU - Nowak, Grzegorz

AU - Rodriguez, Joseph E.

AU - Watkins, Cristilyn N.

AU - Wittenmyer, Rob

AU - Zhou, George

AU - Ziegler, Carl

AU - Bieryla, Allyson

AU - Boyd, Patricia T.

AU - Clark, Catherine A.

AU - Dressing, Courtney D.

AU - Eastman, Jason D.

AU - Eberhardt, Jan

AU - Endl, Michael

AU - Espinoza, Nestor

AU - Fausnaugh, Michael

AU - Guerrero, Natalia M.

AU - Henning, Thomas

AU - Hesse, Katharine

AU - Hobson, Melissa J.

AU - Howell, Steve B.

AU - Jordán, Andrés

AU - Latham, David W.

AU - Lund, Michael B.

AU - Mireles, Ismael

AU - Narita, Norio

AU - Tala Pinto, Marcelo

AU - Pugh, Teznie

AU - Quinn, Samuel N.

AU - Ricker, George

AU - Rodriguez, David R.

AU - Rojas, Felipe I.

AU - Rose, Mark E.

AU - Rudat, Alexander

AU - Sarkis, Paula

AU - Savel, Arjun B.

AU - Schlecker, Martin

AU - Schwarz, Richard P.

AU - Seager, Sara

AU - Shporer, Avi

AU - Smith, Jeffrey C.

AU - Stassun, Keivan G.

AU - Stockdale, Chris

AU - Trifonov, Trifon

AU - Vanderspek, Roland

AU - Winn, Joshua N.

AU - Wright, Duncan

PY - 2024/10/1

Y1 - 2024/10/1

N2 - Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb = 5.8 days, a mass of Mb = 0.9 MJ, and a radius of Rb = 1.3 RJ, with a planetary density of 0.477 g cm-3. TOI-2485 b has an orbital period of Pb = 11.2 days, a mass of Mb = 2.4 MJ, and a radius of Rb = 1.1 RJ with a density of 2.36 g cm-3. Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.

AB - Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb = 5.8 days, a mass of Mb = 0.9 MJ, and a radius of Rb = 1.3 RJ, with a planetary density of 0.477 g cm-3. TOI-2485 b has an orbital period of Pb = 11.2 days, a mass of Mb = 2.4 MJ, and a radius of Rb = 1.1 RJ with a density of 2.36 g cm-3. Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.

KW - Planets and satellites: detection

KW - Planets and satellites: gaseous planets

UR - http://www.scopus.com/inward/record.url?scp=85206218681&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202451313

DO - 10.1051/0004-6361/202451313

M3 - Article

AN - SCOPUS:85206218681

SN - 0004-6361

VL - 690

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A18

ER -

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

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