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Title:
Compact Stellar Systems in the Fornax Cluster: Super-massive Star Clusters or Extremely Compact Dwarf Galaxies?
Authors:
Drinkwater, M. J.; Jones, J. B.; Gregg, M. D.; Phillipps, S.
Affiliation:
AA(School of Physics, University of Melbourne, Vic. 3010, Australia; ), AB(Department of Physics, University of Bristol, Tyndall Avenue, Bristol, BS8 1TL, UK; ), AC(University of California, Davis, and Institute for Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, L-413, Livermore, CA 94550, USA; ), AD(Department of Physics, University of Bristol, Tyndall Avenue, Bristol, BS8 1TL, UK; )
Publication:
Publications of the Astronomical Society of Australia, Volume 17, Issue 3, p.227-233 (PASA Homepage)
Publication Date:
12/2000
Origin:
PASA; CUP
Astronomy Keywords:
STAR CLUSTERS, DWARF GALAXIES, GALAXY FORMATION, galaxies: star clusters, galaxies: dwarf, galaxies: formation
Abstract Copyright:
2000: Astronomical Society of Australia
DOI:
10.1071/AS00034
Bibliographic Code:
2000PASA...17..227D

Abstract

We describe a population of compact objects in the centre of the Fornax Cluster which were discovered as part of our 2dF Fornax Spectroscopic Survey. These objects have spectra typical of old stellar systems, but are unresolved on photographic sky survey plates. They have absolute magnitudes -13 < MB < -11, so they are 10 times more luminous than any Galactic globular clusters, but fainter than any known compact dwarf galaxies. These objects are all within 30 arcminutes of the central galaxy of the cluster, NGC 1399, but are distributed over larger radii than the globular cluster system of that galaxy. We suggest that these objects are either super-massive star clusters (intra-cluster globular clusters or tidally stripped nuclei of dwarf galaxies) or a new type of low-luminosity, compact elliptical dwarf (`M32-type") galaxy. The best way to test these hypotheses will be to obtain high-resolution imaging and high-dispersion spectroscopy to determine their structures and mass-to-light ratios. This will allow us to compare them to known compact objects and establish whether they represent a new class of hitherto unknown stellar system.

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