Namitha Kizhuprakkat Ramachandran (Institute of Astronomy, NTHU); Andrew P. Cooper (Institute of Astronomy, NTHU); DESI collaboration
Our galaxy, the Milky Way, contains many remnants of ancient dwarf galaxy accretion events that have contributed to its stellar halo and thick disk. Using the Dark Energy Spectroscopic Instrument (DESI), the DESI Milky Way Survey (MWS) is designed to explore the assembly history of the Milky Way through the discovery of these remnants and to improve constraints on the Galaxy’s 3D dark matter distribution. In the bright time of DESI survey, MWS is expected to obtain spectra for ≥ 8 million stars in Milky Way selected from the Gaia DR2 catalog and DESI Legacy Imaging Surveys at galactic latitudes |b| >22◦. Stars are observed between 16 < r < 19 mag and, based on their color and Gaia astrometry we assign them to different target classes. MWS will also include samples of stars with extremely high scientific value, including white dwarfs, stars within a 100 pc of the Sun and rare evolutionary states such as BHBs/blue stragglers. In this poster, we present the scientific motivation and target selection criteria for DESI MWS. We will describe the content and surface density of different target classes and the distribution of targets across the footprint.