Issue |
A&A
Volume 690, October 2024
|
|
---|---|---|
Article Number | A18 | |
Number of page(s) | 14 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202451313 | |
Published online | 26 September 2024 |
Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b
1
INAF – Osservatorio Astrofisico di Torino,
Via Osservatorio 20,
10025
Pino Torinese,
Italy
2
Instituto de Astrofísica de Canarias (IAC),
38205
La Laguna, Tenerife,
Spain
3
Departamento de Astrofísica, Universidad de La Laguna (ULL),
38206
La Laguna, Tenerife,
Spain
4
Sub-department of Astrophysics, Department of Physics, University of Oxford,
Oxford,
OX1 3RH,
UK
5
Chalmers University of Technology, Department of Space, Earth and Environment, Onsala Space Observatory,
439 92
Onsala,
Sweden
6
Leiden Observatory, University of Leiden,
PO Box 9513,
2300
RA,
Leiden,
The Netherlands
7
Institute of Planetary Research, German Aerospace Center (DLR),
Rutherfordstrasse 2,
12489
Berlin,
Germany
8
INAF – Osservatorio Astrofisico di Catania,
Via S. Sofia 78,
95123
Catania,
Italy
9
Dipartimento di Fisica, Università degli Studi di Torino,
via Pietro Giuria 1,
10125
Torino,
Italy
10
Department of Astronomy, The Ohio State University,
4055 McPherson Laboratory, 140 West 18th Avenue,
Columbus,
OH
43210,
USA
11
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking,
Surrey
RH5 6NT,
UK
12
European Southern Observatory,
Karl-Schwarzschild-Straße 2,
85748
Garching bei Munchen,
Germany
13
Facultad de Ingeniera y Ciencias, Universidad Adolfo Ibáñez,
Av. Diagonal las Torres 2640,
Peñalolén, Santiago,
Chile
14
Millennium Institute for Astrophysics,
Chile
15
NASA Exoplanet Science Institute-Caltech/IPAC,
Pasadena,
CA
91125,
USA
16
Center for Astrophysics | Harvard & Smithsonian,
60 Garden Street,
Cambridge,
MA
02138,
USA
17
Department of Astronomy and McDonald Observatory, University of Texas at Austin,
2515 Speedway, Stop C1400,
Austin,
TX
78712,
USA
18
NSF National Optical-Infrared Astronomy Research Laboratory,
950 N. Cherry Ave.,
Tucson,
AZ
85719,
USA
19
Department of Astronomy, California Institute of Technology,
Pasadena,
CA
91125,
USA
20
Thüringer Landessternwarte Tautenburg,
Sternwarte 5,
07778
Tautenberg,
Germany
21
Astrophysics Group, Keele University,
Staffordshire
ST5 5BG,
UK
22
Astronomical Institute, Czech Academy of Sciences,
Fričova 298,
25165
Ondřejov,
Czech Republic
23
Lund Observatory, Division of Astrophysics, Department of Physics, Lund University,
Box 43,
22100
Lund,
Sweden
24
Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University,
Grudziądzka 5,
87-100
Toruń,
Poland
25
Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University,
East Lansing,
MI
48824,
USA
26
University of Southern Queensland, Centre for Astrophysics, UniSQ Toowoomba,
West Street,
QLD
4350,
Australia
27
Department of Physics, Engineering and Astronomy, Stephen F. Austin State University,
1936 North St,
Nacogdoches,
TX
75962,
USA
28
NASA Goddard Space Flight Center,
Greenbelt,
MD
20771,
USA
29
Jet Propulsion Laboratory, California Institute of Technology,
Pasadena,
CA
91109,
USA
30
Department of Astronomy, University of California Berkeley,
Berkeley,
CA
94720,
USA
31
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg,
Germany
32
Space Telescope Science Institute,
3700 San Martin Drive,
Baltimore,
MD
21218,
USA
33
Department of Physics & Astronomy, Texas Tech University,
Lubbock,
TX
79410-1051,
USA
34
Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology,
77 Massachusetts Avenue,
Cambridge,
MA
02139,
USA
35
Department of Astronomy, University of Florida,
Gainesville,
FL
32611,
USA
36
Observatoire de Genève, Département d’Astronomie, Université de Genève,
Chemin Pegasi 51b,
1290
Versoix,
Switzerland
37
NASA Ames Research Center,
Moffett Field,
CA
94035,
USA
38
Department of Physics and Astronomy, University of New Mexico,
210 Yale Blvd NE,
Albuquerque,
NM,
USA
39
Komaba Institute for Science, The University of Tokyo,
3-8-1 Komaba, Meguro,
Tokyo
153-8902,
Japan
40
Astrobiology Center,
2-21-1 Osawa, Mitaka,
Tokyo
181-8588,
Japan
41
Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile,
Chile
42
Department of Astronomy, University of Maryland,
College Park,
College Park,
MD
20742,
USA
43
Department of Astronomy/Steward Observatory, The University of Arizona,
933 North Cherry Avenue,
Tucson,
AZ
85721,
USA
44
Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology,
77 Massachusetts Avenue,
Cambridge,
MA
02139,
USA
45
Department of Aeronautics and Astronautics, Massachusetts Institute of Technology,
77 Massachusetts Avenue,
Cambridge,
MA
02139,
USA
46
SETI Institute,
339 N Bernardo Ave Suite 200,
Mountain View,
CA
94043,
USA
47
Department of Physics & Astronomy, Vanderbilt University,
Nashville,
TN,
USA
48
Hazelwood Observatory,
Australia
49
Department of Astronomy, Sofia University “St Kliment Ohridski”,
5 James Bourchier Blvd,
BG-1164
Sofia,
Bulgaria
50
Landessternwarte, Zentrum für Astronomie der Universität Heidelberg,
Königstuhl 12,
69117
Heidelberg,
Germany
51
CAS Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences,
Nanjing
210008,
China
52
Department of Astrophysical Sciences, Princeton University,
Princeton,
NJ
08544,
USA
Received:
30
June
2024
Accepted:
8
August
2024
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.
Key words: planets and satellites: detection / planets and satellites: gaseous planets
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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