S18B0114abst
S18B0114
For mid-to-late M dwarfs (Teff<∼ 3500 K), there are only a handful of transiting planets whose masses have been constrained (i.e., GJ 1214b, GJ 1132b, LHS 1140b, and TRAPPIST-1 planets). This is because the host stars are very faint at “visible" wavelengths, degrading the precision of radial velocity (RV) measurements. The new spectrograph, IRD, developed to achieve an RV precision of <2 m s−1 in the near infrared, was installed on Subaru last year, allowing us to explore new exoplanet parameter space. Here, we propose to observe a few mid-M dwarfs to constrain the masses of the transiting exoplanets around coolest stars. The list of our targets includes K2-33, K2-25, and K2-28, the first two of which are very young and thus especially informative objects. Measurement of planet masses is important not only populating the planet mass-radius diagram for mid-to-late M dwarf systems, but also testing theoretical models to explain the observed distribution of exoplanets (e.g., the photoevaporation scenario to explain the dearth of close-in medium-sized planets).
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