We propose to acquire the high-resolution near-infrared spectra of M dwarfs in visual binary systems with FGK primaries for the verification of our chemical analysis method. M dwarfs are the major targets of planet search projects and the knowledge of their chemical composition is crucial to discuss the formation process or interior of their orbiting planets. While the standard chemical analysis using the visible spectra does not work well for M dwarfs due to their faintness and a forest of molecular features, those problems are mitigated in the near-infrared. We developed the line-by-line analysis method using the high-resolution near-infrared spectra of M dwarfs and verified its reliability for early- to mid-M dwarfs (Teff∼ 3200–3800 K) by the comparison between each component of FGK+M binaries. We need to extend the assessment into late-M dwarfs, which are generally so faint (MJ > ∼10) that they are the unique targets for Subaru/IRD. Therefore, we here propose to acquire IRD spectra of eight late-M dwarfs (Teff∼ 2800–3100 K; 3.1 < GBP−GRP < 4.1) in wide binaries with FGK stars. This temperature range exactly matches the targets of the IRD-SSP, so it will be useful to characterize them.
This document was translated from LATEX by HEVEA.