Speaker
Description
The large uncertainties on the measurement of the mass of galaxies is an important issue in modern astrophysics. For both the MW and M31, thanks to the gas rotation curve, the mass of the inner part of the haloes is well constrained. For the outer part of the haloes, we must turn to satellites galaxies as tracers. But, to use dwarf galaxies as such, it is absolutely crucial to determine the dwarf galaxy detection limits so they can be accurately modeled into the dwarf galaxy system models. I will present the first such effort to characterize fully the dwarf galaxy system of the Andromeda galaxy, based on the PAndAS photometric mapping. As expected, the detection limits are a strong function of the size, luminosity and the location of a dwarf galaxy in the survey. I will then present the impact of such completeness on the determination of M31 mass.
| Do you plan to attend the symposium in-person or virtually? | in-person |
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