The metallicities of the smallest stars are particularly difficult to determine due to their faint magnitudes and complicated spectra. These cool dwarfs are some of the most common stars in the galaxy, however, so their abundances are particularly useful both for detailed Galactic chemical evolution models and for understanding the exoplanets orbiting small stars.
APOGEE is a component of the Sloan Digital Sky Survey focused on determining stellar parameters as a probe of our Galaxy’s structure and evolution. The APOGEE survey consists mid-resolution infrared spectroscopy fit by a model grid to obtain surface temperatures, gravities, and abundance patterns. APOGEE focuses mostly on giant stars, but has also observed thousands of cool (K and M) dwarfs.
In 2015, I worked with an initial sample of these KM dwarfs to confirm their catalog parameters, compare stellar models, and look for optimal colors for photometric indicators of metallicity and surface temperature. We found that previous stellar models didn’t match the coolest M dwarfs, and we also found strong corraltions between SDSS r-z color, WISE W1-W2 color, and these fundamental stellar parameters.
Since the initial work, the APOGEE data set has doubled and Gaia has released parallaxes for the majority of these nearby stars, and I am working with Jennifer Johnson and Victoria DiTomasso to update and expand the APOGEE KM dwarf project and apply the metallicity indicators to a sample of a million M dwarfs in the Solar neighborhood. Expect new results soon!
Examining the relationships between colour, T_eff, and [M/H] for APOGEE K and M dwarfs MNRAS 2016