Issue |
A&A
Volume 684, April 2024
|
|
---|---|---|
Article Number | A96 | |
Number of page(s) | 19 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202348131 | |
Published online | 09 April 2024 |
Revisiting the warm sub-Saturn TOI-1710b
The impact of stellar activity on the mass measurement
1
Instituto de Astrofísica de Canarias (IAC),
38205
La Laguna, Tenerife, Spain
e-mail: jom@iac.es
2
Departamento de Astrofísica, Universidad de La Laguna (ULL),
38206
La Laguna, Tenerife, Spain
3
Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University,
Grudzia̧dzka 5,
87-100
Toruń, Poland
4
Instituto de Astrofísica de Andalucía (IAA-CSIC),
Glorieta de la Astronomía s/n,
18008
Granada, Spain
5
DTU Space, National Space Institute, Technical University of Denmark,
Elektrovej 328,
2800 Kgs.
Lyngby, Denmark
6
Thomas Jefferson High School,
6560 Braddock Rd,
Alexandria, VA
22312, USA
7
George Mason University, Department of Physics and Astronomy,
4400 University Drive MS 3F3,
Fairfax, VA
22030, USA
8
Centro de Astrobiología (CSIC-INTA),
ESAC Campus, Camino Bajo del Castillo s/n, Villanueva de la Cañada,
28692
Madrid, Spain
9
NASA Exoplanet Science Institute, Caltech/IPAC,
Mail Code 100-22, 1200 E. California Blvd.,
Pasadena, CA
91125, USA
10
NASA Ames Research Center,
Moffett Field, CA
94035, USA
11
Department of Physics and Astronomy, Michigan State University,
East Lansing, MI
48824, USA
12
Max Planck Institute for Astronomy,
Königstuhl 17,
69117
Heidelberg, Germany
13
Department of Earth and Planetary Sciences, University of California Riverside,
900 University Ave,
Riverside, CA
92521, USA
14
Department of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University,
University Park, PA
16802, USA
15
Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University,
University Park, PA
16802, USA
16
Department of Physics and Astronomy, University of New Mexico,
210 Yale Blvd NE,
Albuquerque, NM
87106, USA
17
Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology,
Cambridge, MA
02139, USA
18
Department of Aeronautics and Astronautics, MIT,
77 Massachusetts Avenue,
Cambridge, MA
02139, USA
19
NCCR/PlanetS, Centre for Space & Habitability, University of Bern,
Bern
3012, Switzerland
20
Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology,
Cambridge, MA
02139, USA
21
Department of Astrophysical Sciences,
Peyton Hall, 4 Ivy Lane,
Princeton, NJ
08544, USA
22
Department of Physics and McDonnell Center for the Space Sciences, Washington University,
St. Louis, MO
63130, USA
23
NASA Goddard Space Flight Center,
8800 Greenbelt Road,
Greenbelt, MD
20771, USA
24
SETI Institute,
189 Bernardo Ave., Suite 200,
Mountain View, CA
94043, USA
25
Royal Astronomical Society, Burlington House,
Piccadilly,
London
W1J 0BQ, UK
26
Center for Astrophysics | Harvard & Smithsonian,
60 Garden Street,
Cambridge, MA
02138, USA
27
Planetary Discoveries,
Fredericksburg, VA
22405, USA
Received:
2
October
2023
Accepted:
12
January
2024
The Transiting Exoplanet Survey Satellite (TESS) provides a continuous suite of new planet candidates that need confirmation and precise mass determination from ground-based observatories. This is the case for the G-type star TOI-1710, which is known to host a transiting sub-Saturn planet (Mp = 28.3 ± 4.7 M⊕) in a long-period orbit (P = 24.28 days). Here we combine archival SOPHIE and new and archival HARPS-N radial velocity data with newly available TESS data to refine the planetary parameters of the system and derive a new mass measurement for the transiting planet, taking into account the impact of the stellar activity on the mass measurement. We report for TOI-1710b a radius of Rp = 5.15 ± 0.12 R⊕, a mass of Mp = 18.4 ± 4.5 M⊕, and a mean bulk density of ρp = 0.73 ± 0.18 g cm−3, which are consistent at 1.2σ, 1.5σ, and 0.7σ, respectively, with previous measurements. Although there is not a significant difference in the final mass measurement, we needed to add a Gaussian process component to successfully fit the radial velocity dataset. This work illustrates that adding more measurements does not necessarily imply a better mass determination in terms of precision, even though they contribute to increasing our full understanding of the system. Furthermore, TOI-1710b joins an intriguing class of planets with radii in the range 4–8 R⊕ that have no counterparts in the Solar System. A large gaseous envelope and a bright host star make TOI-1710b a very suitable candidate for follow-up atmospheric characterization.
Key words: techniques: photometric / techniques: radial velocities / planets and satellites: individual: TOI-1710b / stars: individual: TOI-1710
© 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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