Open AccessThe formation of ultracompact dwarf galaxies
Author(s) -
Fellhauer Michael,
Kroupa Pavel
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05087.x
Subject(s) - physics , astrophysics , supercluster (genetic) , fornax cluster , dwarf galaxy , astronomy , star cluster , galaxy cluster , galaxy , galaxy groups and clusters , surface brightness , population , galaxy group , biochemistry , phylogenetics , demography , sociology , gene , chemistry
Recent spectroscopic observations of galaxies in the Fornax Cluster reveal nearly unresolved ‘star‐like’ objects with redshifts appropriate to the Fornax Cluster. These objects have intrinsic sizes of ≈100 pc and absolute B ‐band magnitudes in the range −14< M B <−11.5 mag and lower limits for the central surface brightness μ B ≳23 mag arcsec −2 , and so appear to constitute a new population of ultracompact dwarf galaxies (UCDs). Such compact dwarfs were predicted to form from the amalgamation of stellar superclusters (by Kroupa), which are rich aggregates of young massive star clusters (YMCs) that can form in collisions between gas‐rich galaxies. Here we present the evolution of superclusters in a tidal field. The YMCs merge on a few supercluster crossing times. Superclusters that are initially as concentrated and massive as knot S in the interacting Antennae galaxies evolve to merger objects that are long‐lived and show properties comparable to the newly discovered UCDs. Less massive superclusters resembling knot 430 in the Antennae may evolve to ω Cen‐type systems. Low‐concentration superclusters are disrupted by the tidal field, dispersing their surviving star clusters while the remaining merger objects rapidly evolve into the μ B − M B region populated by low‐mass Milky Way dSph satellites.