A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N
We report the discovery and characterization of the transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite. Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-vel...
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| Other Authors: | |
| Format: | Article |
| Language: | English |
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EDP Sciences
2023
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| Online Access: | https://hdl.handle.net/1721.1/148416 |
| _version_ | 1826200795612184576 |
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| author | Seager, Sara |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Seager, Sara |
| author_sort | Seager, Sara |
| collection | MIT |
| description | We report the discovery and characterization of the transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite. Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic
observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov
chain Monte-Carlo adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC analysis of the
TESS light curve and the radial-velocity evolution allows us to determine the planetary system properties. From our analysis, TOI1710 b is found to be a massive warm super-Neptune (Mp = 28.3 ± 4.7 M⊕ and Rp = 5.34 ± 0.11 R⊕) orbiting a G5V dwarf star
(Teff = 5665 ± 55 K) on a nearly circular 24.3-day orbit (e = 0.16 ± 0.08). The orbital period of this planet is close to the estimated
rotation period of its host star Prot = 22.5 ± 2.0 days and it has a low Keplerian semi-amplitude K = 6.4 ± 1.0 m s−1
; we thus performed
additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of 1.03 ± 0.23 g cm−3
and
orbiting a bright host star (J = 8.3, V = 9.6), TOI-1710 b is one of the best targets in this mass-radius range (near the Neptunian desert)
for atmospheric characterization via transmission spectroscopy, a key measurement in constraining planet formation and evolutionary
models of sub-Jovian planets. |
| first_indexed | 2024-09-23T11:41:33Z |
| format | Article |
| id | mit-1721.1/148416 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T11:41:33Z |
| publishDate | 2023 |
| publisher | EDP Sciences |
| record_format | dspace |
| spelling | mit-1721.1/1484162023-03-09T03:28:37Z A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N Seager, Sara Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences We report the discovery and characterization of the transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite. Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov chain Monte-Carlo adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC analysis of the TESS light curve and the radial-velocity evolution allows us to determine the planetary system properties. From our analysis, TOI1710 b is found to be a massive warm super-Neptune (Mp = 28.3 ± 4.7 M⊕ and Rp = 5.34 ± 0.11 R⊕) orbiting a G5V dwarf star (Teff = 5665 ± 55 K) on a nearly circular 24.3-day orbit (e = 0.16 ± 0.08). The orbital period of this planet is close to the estimated rotation period of its host star Prot = 22.5 ± 2.0 days and it has a low Keplerian semi-amplitude K = 6.4 ± 1.0 m s−1 ; we thus performed additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of 1.03 ± 0.23 g cm−3 and orbiting a bright host star (J = 8.3, V = 9.6), TOI-1710 b is one of the best targets in this mass-radius range (near the Neptunian desert) for atmospheric characterization via transmission spectroscopy, a key measurement in constraining planet formation and evolutionary models of sub-Jovian planets. 2023-03-08T16:15:03Z 2023-03-08T16:15:03Z 2022 2023-03-08T16:10:41Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/148416 Seager, Sara. 2022. "A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N." Astronomy and Astrophysics, 666. en 10.1051/0004-6361/202143002 Astronomy and Astrophysics Creative Commons Attribution 4.0 International license https://creativecommons.org/licenses/by/4.0/ application/pdf EDP Sciences EDP Sciences |
| spellingShingle | Seager, Sara A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title | A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title_full | A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title_fullStr | A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title_full_unstemmed | A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title_short | A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N |
| title_sort | warm super neptune around the g dwarf star toi 1710 revealed with tess sophie and harps n |
| url | https://hdl.handle.net/1721.1/148416 |
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