Prospecting in late-type dwarfs: a calibration of infrared and visible spectroscopic metallicities of late-K and M dwarfs spanning 1.5 dex

TL;DR

This study develops new methods and calibrations to accurately determine the metallicities of late-K and M dwarfs using visible and infrared spectra, aiding planet search efforts and stellar modeling.

Contribution

It introduces improved empirical calibrations for metallicity estimation from moderate resolution spectra across multiple wavelength ranges, applicable to a wide metallicity and spectral type range.

Findings

Metallicity can be reliably estimated to < 0.10 dex using visible, J, H, or K band spectra.

Existing calibrations are accurate for [Fe/H] > -0.5 but less so for more metal-poor stars.

The zeta parameter correlates with [Fe/H] at super-solar metallicities but is unreliable for metal-poor M dwarfs.

Abstract

Knowledge of late K and M dwarf metallicities can be used to guide planet searches and constrain planet formation models. However, the determination of metallicities of late-type stars is difficult because visible wavelength spectra of their cool atmospheres contain many overlapping absorption lines, preventing the measurement of equivalent widths. We present new methods, and improved calibrations of existing methods, to determine metallicities of late-K and M dwarfs from moderate resolution (1300 < R < 2000) visible and infrared spectra. We select a sample of 112 wide binary systems that contain a late-type companion to a solar-type primary star. Our sample includes 62 primary stars with previously published metallicities, as well as 50 stars with metallicities determined from our own observations. We use our sample to empirically determine which features in the spectrum of the companion are best correlated with the metallicity of the primary. We derive metallicity calibrations for different wavelength ranges, and show that it is possible to get metallicities reliable to < 0.10 dex using either visible, J, H, or K band spectra. Our calibrations are applicable to dwarfs with metallicities of -1.04 < [Fe/H]< +0.56 and spectral types from K7 to M5. Lastly, we use our sample of wide binaries to test and refine existing calibrations to determine M dwarf metallicities. We find that the zeta parameter, which measures the ratio of TiO can CaH bands, is correlated with [Fe/H] for super-solar metallicities, and zeta does not always correctly identify metal-poor M dwarfs. We also find that existing calibrations in the K and H band are quite reliable for stars with [Fe/H] > -0.5, but are less useful for more metal-poor stars.