S19B0100abst
S19B0100
For understanding the formation or interiors of exoplanets, it is crucial to know the chemical compositions of host stars. M dwarfs are promising targets to discover Earth-like planets recently but their optical faintness and complex molecular absorption hamper the well-established method for chemical analysis with high-resolution optical spectroscopy. The problems are mitigated in the near-infrared spectra, and hence some previous studies derived chemical compositions of M dwarfs by high-resolution near-IR spectroscopy. Especially to measure the individual elementals, the wide wavelength range and the high wavelength resolution of Subaru/IRD is uniquely preferable. However, firstly we had to examine the reliability of the method and calibrate it if necessary, so we planned to use physical FGK+M binaries for the assessment. We already attempted the assessment on 3 early- to mid-M dwarfs (βΌ3200 β 3800 K) by using the CARMENES (on 3.5m telescope) spectra and found the consistency on about 4 elements. Further, we need to expand the assessment into later-M dwarfs, which are generally so faint (MJ > βΌ10) that they are the unique targets for Subaru/IRD with the 8m diameter. Hence, we here propose to acquire IRD spectra of 7 late-M dwarfs (βΌ2800 β 3100 K) in wide binaries with FGK stars.
This document was translated from LATEX by HEVEA.