Revisiting the warm sub-Saturn TOI-1710b
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arXiv
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| Natura: | Preprint |
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2024
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| author | Orell-Miquel, J. Carleo, I. Murgas, F. Nowak, G. Palle, E. Luque, R. Masseron, T. Sanz-Forcada, J. Dragomir, D. Dalba, P. A. Tronsgaard, R. Wittrock, J. Kim, K. Stibbards, C. Collins, K. I. Plavchan, P. Howell, S. B. Furlan, E. Buchhave, L. A. Gnilka, C. L. Gupta, A. F. Henning, Th. Lester, K. V. Rodriguez, J. E. Scott, N. J. Osborn, H. P. Villanueva Jr., S. Seager, S. Winn, J. N. Jenkins, J. M. Vanderspek, R. Latham, D. W. Rowden, P. Watanabe, D. Torres, G. Burke, C. J. Daylan, T. Barclay, T. Twicken, J. D. Ricker, G. R. |
| author_facet | Orell-Miquel, J. Carleo, I. Murgas, F. Nowak, G. Palle, E. Luque, R. Masseron, T. Sanz-Forcada, J. Dragomir, D. Dalba, P. A. Tronsgaard, R. Wittrock, J. Kim, K. Stibbards, C. Collins, K. I. Plavchan, P. Howell, S. B. Furlan, E. Buchhave, L. A. Gnilka, C. L. Gupta, A. F. Henning, Th. Lester, K. V. Rodriguez, J. E. Scott, N. J. Osborn, H. P. Villanueva Jr., S. Seager, S. Winn, J. N. Jenkins, J. M. Vanderspek, R. Latham, D. W. Rowden, P. Watanabe, D. Torres, G. Burke, C. J. Daylan, T. Barclay, T. Twicken, J. D. Ricker, G. R. |
| contents | 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 ($\mathrm{M_p}=$28.3$\pm$4.7$\mathrm{M}_\oplus$) in a long-period orbit (P=24.28\,d). 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 $\mathrm{R_p}$$=$5.15$\pm$0.12$\mathrm{R}_\oplus$, a mass of $\mathrm{M_p}$$=$18.4$\pm$4.5$\mathrm{M}_\oplus$, and a mean bulk density of $ρ_{\rm p}$$=$0.73$\pm$0.18$\mathrm{g \, cm^{-3}}$, which are consistent at 1.2$σ$, 1.5$σ$, and 0.7$σ$, 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 $\mathrm{R}_\oplus$ 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_13574 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Revisiting the warm sub-Saturn TOI-1710b Orell-Miquel, J. Carleo, I. Murgas, F. Nowak, G. Palle, E. Luque, R. Masseron, T. Sanz-Forcada, J. Dragomir, D. Dalba, P. A. Tronsgaard, R. Wittrock, J. Kim, K. Stibbards, C. Collins, K. I. Plavchan, P. Howell, S. B. Furlan, E. Buchhave, L. A. Gnilka, C. L. Gupta, A. F. Henning, Th. Lester, K. V. Rodriguez, J. E. Scott, N. J. Osborn, H. P. Villanueva Jr., S. Seager, S. Winn, J. N. Jenkins, J. M. Vanderspek, R. Latham, D. W. Rowden, P. Watanabe, D. Torres, G. Burke, C. J. Daylan, T. Barclay, T. Twicken, J. D. Ricker, G. R. Earth and Planetary Astrophysics 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 ($\mathrm{M_p}=$28.3$\pm$4.7$\mathrm{M}_\oplus$) in a long-period orbit (P=24.28\,d). 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 $\mathrm{R_p}$$=$5.15$\pm$0.12$\mathrm{R}_\oplus$, a mass of $\mathrm{M_p}$$=$18.4$\pm$4.5$\mathrm{M}_\oplus$, and a mean bulk density of $ρ_{\rm p}$$=$0.73$\pm$0.18$\mathrm{g \, cm^{-3}}$, which are consistent at 1.2$σ$, 1.5$σ$, and 0.7$σ$, 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 $\mathrm{R}_\oplus$ 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. |
| title | Revisiting the warm sub-Saturn TOI-1710b |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2401.13574 |