Abstract
AbstractWe study numerically the formation of dSph galaxies. Intense starbursts, e.g., in gas-rich environments, typically produce a few to a few hundred young star clusters within a region of just a few hundred pc. The dynamical evolution of these star clusters may explain the formation of the luminous component of dwarf spheroidal (dSph) galaxies. Here, we perform a numerical experiment to show that the evolution of star cluster complexes in dark-matter haloes can explain the formation of the luminous components of dSph galaxies.
Highlights
Understanding the formation and evolution of galaxies is a fundamental goal in astronomy
This leads to subsequent dissolution of the SCs and the distribution of their stars in the central area of the DM halo, building up the luminous component of the dwarf spheroidal (dSph) galaxy
We study numerically the formation of dSph galaxies from merging star clusters, considering two distinct types of profiles for the dark-matter halo
Summary
Understanding the formation and evolution of galaxies is a fundamental goal in astronomy. The dynamical evolution of these star clusters, i.e., their dissolution due to gas expulsion and subsequent merging in the centre of the DM halo, may explain the formation of dSph galaxies. The distribution of the star clusters inside the central area of the DM halo follows a Plummer distribution, while we take two distinct types of DM haloes into account: a cusped Navarro, Frenk & White (NFW; Navarro et al 1997) and a cored Plummer profile (Plummer 1911).
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