Abstract by Benne Holwerda
Counting stars is one of the oldest techniques to determine the shape and size of the Milky Way. Long the realm of bright stars, the discovery space in deep WFC3 imaging of the high-redshift Universe covers the same luminosity and color ranges that probe dwarf stars belonging to our own Milky Way.
The BoRG pure-parallel WFC3 survey probes many lines-of-sight out of our own Galaxy with four filters. I present a way to identify the stars in this survey, and calibrate their spectral type from the colors. The ultimate goal is to characterize the shape and size of the components of the Milky Way (thin and thick disk, possible the spheroid) using these bona-fide M-dwarf stars.
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