| Name: | Pradyumna Sadhu |
| Affiliation: | University of California, Riverside |
| Conference ID: | ASI2025_187 |
| Title: | Satellites galaxy abundances in clusters of galaxies within ΛCDM: from ultrafaints to ellipticals |
| Authors: | Pradyumna Sadhu 1, Laura V. Sales 1, Raphael Errani 2 3, Julio F. Navarro 4 |
| Authors Affiliation: | 1 Department of Physics and Astronomy, University of California, Riverside, CA, 92521, USA
2 McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA
3 Universite de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550, F-67000 Strasbourg, France
4 Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada |
| Mode of Presentation: | Oral |
| Abstract Category: | Galaxies and Cosmology |
| Abstract: | Current cosmological simulations lack the resolution to make reliable predictions for faint and ultra-faint dwarf satellites, which will become a crucial test of the LCDM model in the upcoming era of the Vera Rubin Observatory and the Roman Space Telescope. To this end, we utilize an analytical model fitted to high-resolution controlled simulations to extend the predictions of the TNG50 cosmological numerical simulations to ultrafaint dwarf regime. We focus on 3 clusters with virial masses ~1e14 Msun, comparable to the Virgo and Fornax clusters, and characterize their luminous satellite population from ultrafaint dwarfs to massive elliptical galaxies. We find that under the assumption of cuspy dark matter halos such as NFW profiles, the majority of all satellite galaxies survive within cluster environments, expecting 10-100 thousand luminous satellites within the virial radius of such clusters. This is contrary to the results directly from the simulation where satellites get merged artificially due to poor numerical resolution. We determine the radial distribution of satellites, finding massive satellite (Mstar > 1e8 Msun) to align well with matter distribution of the cluster while dwarfs display a cored profile. Additionally, tidal evolution drives evolution of satellites along the canonical size-mass relation observed for Local Group and Virgo satellites. |
