S18A0089abst

S18A0089

Given the small stellar radii (thus deeper transits) and proximity of the habitable zone to the central stars, M dwarfs are attractive targets for transiting planet surveys, but the validation and confirmation of transiting planets around M dwarfs are far more limited than those orbiting solar-type stars. Based on our previous observing campaigns, we have identified the possible trends that (1) radii of planets dramatically shrink when the insolation from the central M stars becomes higher, and (2) larger planets are only discovered around metal-rich M dwarfs. In order to enlarge the sample of the lowest-mass planet-hosts and confirm the possible trends (properties) of M-dwarf planets, we here propose to validate ∼ 8 M-dwarf planetary systems, which were observed by K2 and identified by our transit detection pipeline within the KESPRINT team, by combining AO imaging with IRCS and high resolution spectroscopy with HDS. Planets around the lowest-mass stars validated in our project are likely to be ideal targets for future characterizations (e.g., mass measurements) in the upcoming semesters especially with near-infrared high resolution spectroscopy (i.e., Subaru/IRD).

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