Study of stellar relics from the early galaxy

According to the hierarchical galaxy formation models, the Milky Way stellar halo is formed by continuous accretion from smaller satellite galaxies. The remnant of such accretion events will still be observed in the Milky Way neighborhood as low luminous dwarf galaxies or stellar streams. This can be observationally validated by studying the chemical and kinematical properties of stars in the halo and the nearby satellites. 
In the talk, I will discuss the possible connection between the stellar populations in the halo and a few of the satellite galaxies of the Milky Way, derived from optical and infrared spectroscopic observations (using 8m VLT UVES, APO3.5m, 10m HET and 2m HCT-HESP, HCT-TIRSPEC, HCT-HFOSC). I will also discuss the potential role of infrared observations (e.g., using TANSPEC) for studying the Milky Way disk and halo population.