The Occurrence Rate of Terrestrial Planets Orbiting Nearby Mid-to-late M Dwarfs from TESS Sectors 1-42

Abstract

We present an analysis of a volume-complete sample of 363 mid-to-late M dwarfs within 15 pc of the Sun with masses between 0.1 and 0.3 M${}_{\odot }$ observed by TESS within Observation Sectors 1 to 42. The median mass of the stars in this sample is 0.17 M${}_{\odot }$. We search the TESS 2-minute cadence light curves for transiting planets with orbital periods below 7 days using a modified Box-Least Squares (BLS) algorithm and recover all 6 known planets within the sample as well as a likely planet candidate orbiting LHS 475 (TESS Object of Interest 910.01). Each of these planets is consistent with a terrestrial composition, with planet radii ranging from 0.91 R${}_{\oplus }$ to 1.31 R${}_{\oplus }$. In addition, we perform a transit injection and recovery analysis for each of the 363 stars to characterize the transit detection sensitivity as a function of planet radius, insolation, and orbital period. We obtain a cumulative occurrence rate of $0.61_{-0.19}^{+0.24}$ terrestrial planets per M dwarf with radii above 0.5 R${}_{\oplus }$ and orbital periods between 0.4-7 days. We find that for comparable insolations, planets larger than 1.5 R${}_{\oplus }$ (sub-Neptunes and water worlds) are significantly less abundant around mid-to-late M dwarfs compared to earlier-type stars, while the occurrence rate of terrestrial planets is comparable to that of more massive M dwarfs. We estimate that overall, terrestrials outnumber sub-Neptunes around mid-to-late M dwarfs at a ratio of 14 to 1, in contrast to GK dwarfs where they are roughly equinumerous. We place a $1\sigma$ upper limit of 0.07 planets larger than 1.5 R${}_{\oplus }$ per mid-to-late M dwarf, within the orbital period range of 0.5-7 days. We find evidence for a downturn in occurrence rates for planet radii below 0.9 R${}_{\oplus }$, suggesting that Earth-sized and larger terrestrials may be more common around mid-to-late M dwarfs.

arXiv comment25 pages, 8 figures, 9 tables. Accepted for publication in the Astronomical Journal

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