Detection of an Atmospheric Outflow from the Young Hot Saturn TOI-1268b

Abstract

Photoevaporative mass-loss rates are expected to be highest when planets are young and the host star is more active, but to date there have been relatively few measurements of mass-loss rates for young gas giant exoplanets. In this study we measure the present-day atmospheric mass-loss rate of TOI-1268b, a young (110–380 Myr) and low density (0.71 ${}_{-0.13}^{+0.17}$ g cm ^−3 ) hot Saturn located near the upper edge of the Neptune desert. We use Palomar/WIRC to search for excess absorption in the 1083 nm helium triplet during two transits of TOI-1268b. We find that it has a larger transit depth ( ${0.285}_{-0.050}^{+0.048} \% $ excess) in the helium bandpass than in the TESS observations, and convert this excess absorption into a mass-loss rate by modeling the outflow as a Parker wind. Our results indicate that this planet is losing mass at a rate of $\mathrm{log}\dot{M}=10.2\pm 0.3$ g s ^−1 and has a thermosphere temperature of ${6900}_{-1200}^{+1800}$ K. This corresponds to a predicted atmospheric lifetime much larger than 10 Gyr. Our result suggests that photoevaporation is weak in gas giant exoplanets even at early ages.

Keywords

• Exoplanet atmospheres
• Narrow band photometry