Published April 16, 2019
| Version v1
Poster
Open
Mapping M Dwarf Metallicities
Description
We use distances derived from Gaia parallaxes cross-matched with SDSS, WISE and 2MASS photometry to assemble a sample of approximately 2 million M dwarfs, defined as stars with SDSS colors redder than r-i = 0.3 and i-z = 0.2. Previous work has found relations between SDSS r-z and WISE W1-W2 colors and the effective temperature and metallicities of cool stars (3550-4200 K). Using our sample and these previously derived relationships, we measure these stars' metallicities and effective temperatures. We calculate the metallicity distribution gradient as a function of galactic height for M dwarfs within 1000 pc of the Sun, which ultimately lends insight to the kinematic and chemical evolution of the Galaxy.
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VDiTomasso_eslab_poster.pdf
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Additional details
References
- Cheng, J. Y., et al. Metallicity Gradients in the Milky Way Disk as Observed by the SEGUE Survey
- Davenport, J. R. A. & Dorn-Wallenstein, T. Z., Photometric Metallicities for Low-mass Stars with Gaia and WISE
- Garcia Perez, A. E., et al. (2015) ASPCAP: The APOGEE Stellar Parameter and Chemical Abundances Pipeline
- Green, G. M., et al. (2018) Galactic reddening in 3D from stellar photometry - an improved map
- Hartkopf, W.I. & Yoss, K.M. (1982) A Kinematic and Abundance Survey at the Galactic Poles
- Schlesinger, K.J., et al. (2014) The Vertical Metallicity Gradient of the Milky Way Disk: Transitions in [α/Fe] Populations
- Schmidt, S. J., et al. (2016) Examining the relationships between colour, Teff, and [M/H] for APOGEE K and M dwarfs
- Woolf, V. M. & West, A. A. (2012) The M dwarf problem in the Galaxy