Satellites and Haloes of Dwarf Galaxies
Laura V. Sales, Wenting Wang, Simon D. M. White, Julio F. Navarro

TL;DR
This study examines satellite galaxy abundance across a wide range of primary galaxy masses using SDSS data, confirming LCDM model predictions and revealing scale-dependent satellite distributions.
Contribution
It extends previous work by analyzing satellite abundance around primaries from dwarfs to clusters, showing independence for dwarfs and strong dependence for larger galaxies.
Findings
Satellite abundance is independent of primary mass for dwarf galaxies.
Satellite abundance correlates strongly with primary mass for larger galaxies.
Results support LCDM galaxy formation models and the galaxy-halo mass relation.
Abstract
We study the abundance of satellite galaxies as a function of primary stellar mass using the SDSS/DR7 spectroscopic catalogue. In contrast with previous studies, which focussed mainly on bright primaries, our central galaxies span a wide range of stellar mass, 10^7.5 < M_*^pri/M_sun < 10^11, from dwarfs to central cluster galaxies. Our analysis confirms that the average number of satellites around bright primaries, when expressed in terms of satellite-to-primary stellar mass ratio (m_*^sat/M_*^pri), is a strong function of M_*^pri. On the other hand, satellite abundance is largely independent of primary mass for dwarf primaries (M_*^pri<10^10 M_sun). These results are consistent with galaxy formation models in the LCDM scenario. We find excellent agreement between SDSS data and semi-analytic mock galaxy catalogues constructed from the Millennium-II Simulation. Satellite galaxies trace…
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