Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

Globular clusters (GCs) are some of the most visible tracers of the merging and accretion histories of galaxy halos. Metal-poor GCs, in particular, are thought to arrive in massive galaxies largely through dry, minor merging events, but it is rare to see a direct connection between GCs and visible s...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2017-02, Vol.835 (2), p.123
Main Authors: Lim, Sungsoon, Peng, Eric W., Duc, Pierre-Alain, Fensch, Jérémy, Durrell, Patrick R., Harris, William E., Cuillandre, Jean-Charles, Gwyn, Stephen, Lançon, Ariane, Sánchez-Janssen, Rúben
Format: Article
Language:English
Subjects:
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Correlation
CORRELATIONS
Deposition
Fine structure
Galactic clusters
GALACTIC EVOLUTION
Galactic halos
GALAXIES
galaxies: elliptical and lenticular, cD
galaxies: evolution
galaxies: formation
galaxies: individual (NGC 474)
galaxies: star clusters: general
Globular clusters
Halos
Sciences of the Universe
Shell galaxies
STAR CLUSTERS
Stars & galaxies
Tracers
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:Globular clusters (GCs) are some of the most visible tracers of the merging and accretion histories of galaxy halos. Metal-poor GCs, in particular, are thought to arrive in massive galaxies largely through dry, minor merging events, but it is rare to see a direct connection between GCs and visible stellar streams. NGC 474 is a post-merger early-type galaxy with dramatic fine structures made of concentric shells and radial streams that have been more clearly revealed by deep imaging. We present a study of GCs in NGC 474 to better establish the relationship between merger-induced fine structure and the GC system. We find that many GCs are superimposed on visible streams and shells, and about 35% of GCs outside are located in regions of fine structure. The spatial correlation between GCs and fine structure is significant at the 99.9% level, which shows that this correlation is not coincidental. The colors of GCs on fine structures are mostly blue, and we also find an intermediate-color population that is dominant in the central region and that will likely passively evolve to have colors consistent with a traditional metal-rich GC population. The association of the blue GCs with fine structures is direct confirmation that many metal-poor GCs are accreted onto massive galaxy halos through merging events and that the progenitors of these mergers are sub- galaxies.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/835/2/123