학술논문
Revisiting the warm sub-Saturn TOI-1710b
Document Type
Working Paper
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.
Source
Subject
Language
Abstract
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 $\rho_{\rm p}$$=$0.73$\pm$0.18$\mathrm{g \, cm^{-3}}$, which are consistent at 1.2$\sigma$, 1.5$\sigma$, and 0.7$\sigma$, 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.
Comment: Accepted for publication in A&A. 21 pages, 14 figures
Comment: Accepted for publication in A&A. 21 pages, 14 figures