Occurrence Rate of Hot Jupiters Around Early-type M Dwarfs Based on Transiting Exoplanet Survey Satellite Data

Gan, Tianjun; Wang, Sharon X.; Wang, Songhu; Mao, Shude; Huang, Chelsea X.; Collins, Karen A.; Stassun, Keivan G.; Shporer, Avi; Zhu, Wei; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Barkaoui, Khalid; Belinski, Alexander A.; Ciardi, David R.; Evans, Phil; Girardin, Eric; Maslennikova, Nataliia A.; Mazeh, Tsevi; Panahi, Aviad; Pozuelos, Francisco J.; Radford, Don J.; Schwarz, Richard P.; Twicken, Joseph D.; Wünsche, Anaël; Zucker, Shay
Bibliographical reference

The Astronomical Journal

Advertised on:
1
2023
Number of authors
29
IAC number of authors
1
Citations
5
Refereed citations
2
Description
We present an estimate of the occurrence rate of hot Jupiters (7 R ⊕ ≤ R p ≤ 2 R J, 0.8 ≤ P b ≤ 10 days) around early-type M dwarfs based on stars observed by the Transiting Exoplanet Survey Satellite (TESS) during its primary mission. We adopt stellar parameters from the TESS Input Catalog and construct a sample of 60,819 M dwarfs with 10.5 ≤ T mag ≤ 13.5, effective temperatures 2900 ≤ T eff ≤ 4000 K, and stellar masses 0.45 ≤ M * ≤ 0.65 M ⊙. We conduct a uninformed transit search using a detection pipeline based on the box least square search and characterize the searching completeness through an injection and recovery experiment. We combine a series of vetting steps including light centroid measurement, odd/even and secondary eclipse analysis, rotation and transit period synchronization tests as well as inspecting the ground-based photometric, spectroscopic, and imaging observations. Finally, we find a total of nine planet candidates, all of which are known TESS objects of interest. We obtain an occurrence rate of 0.27% ± 0.09% for hot Jupiters around early-type M dwarfs that satisfy our selection criteria. Compared with previous studies, the occurrence rate of hot Jupiters around early-type M dwarfs is smaller than all measurements for FGK stars, although they are consistent within 1σ-2σ. There is a trend that the occurrence rate of hot Jupiters has a peak at G dwarfs and falls toward both hotter and cooler stars. Combining results from transit, radial velocity, and microlensing surveys, we find that hot Jupiters around early-type M dwarfs possibly show a steeper decrease in the occurrence rate per logarithmic semimajor axis bin ( ${dN}/d{\mathrm{log}}_{10}a$ ) when compared with FGK stars.