期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 747, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/2041-8205/747/2/L38
关键词
planetary systems; stars: abundances; stars: late-type; techniques: spectroscopic
资金
- University of Hawaii [NNX-08AE38A]
- National Aeronautics and Space Administration, Science Mission Directorate
- NAI
- PSARC
- NSF [AST-1006676, AST-1126413]
- Pennsylvania State University
- Eberly College of Science
- Pennsylvania Space Grant Consortium
We present an empirical near-infrared (NIR) spectroscopic method for estimating M dwarf metallicities, based on features in the H band, as well as an implementation of a similar published method in the K band. We obtained R similar to 2000 NIR spectra of a sample of M dwarfs using the NASA IRTF-SpeX spectrograph, including 22 M dwarf metallicity calibration targets that have FGK companions with known metallicities. The H-band and K-band calibrations provide equivalent fits to the metallicities of these binaries, with an accuracy of +/- 0.12 dex. We derive the first empirically calibrated spectroscopic metallicity estimate for the giant planet-hosting M dwarf GJ 317, confirming its supersolar metallicity. Combining this result with observations of eight other M dwarf planet hosts, we find that M dwarfs with giant planets are preferentially metal-rich compared to those that host less massive planets. Our H-band calibration relies on stronglymetallicity-dependent features in the H band, which will be useful in compositional studies using mid-to high-resolution NIR M dwarf spectra, such as those produced by multiplexed surveys like SDSS-III APOGEE. These results will also be immediately useful for ongoing spectroscopic surveys of M dwarfs.
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