Globular cluster systems in nearby dwarf galaxies – III. Formation efficiencies of old globular clusters

By I. Georgiev, Thomas H. Puzia, P. Goudfrooij, Michael Hilker. 2010

136 citations recorded by the source corpus.

We investigate the origin of the shape of the globular cluster (GC) system scaling parameters as a function of galaxy mass, i.e. specific frequency (SN), specific luminosity (SL), specific mass (SM) and specific number ( ˆ T ) of GCs. In the low-mass galaxy regime (MV −16 mag), our analysis is based on Hubble Space Telescope/Advanced Camera for Surveys observations of GC populations of faint, mainly late-type dwarf galaxies in low-density environments. In order to sample the entire range in galaxy mass (MV =− 11 to −23 mag =10 6 –1 0 11 L� ), environment and morphology we augment our sample with data of spiral and elliptical galaxies from the literature, in which old GCs are reliably detected. This large data set confirms (irrespective of the galaxy type) the increase in the specific frequencies of GCs above and below a galaxy magnitude of MV �− 20 mag. Over the full mass range, the SL value of early-type galaxies is, on average, twice that of late types. To investigate the observed trends, we derive theoretical predictions of GC system scaling parameters as a function of host galaxy mass based on the models of Dekel and Birnboim in which star formation processes are , �,

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f08cc80ace004cd3ccec0d15ef83d87caaf5215e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. W. Harris
2. J. Kruijssen
3. P. Durrell
4. L. Ferrarese
5. E. Peng
6. G. Harris
7. P. Harding
8. M. Alessi

In Instrumentation

1. P. Durrell
2. W. Harris
3. J. Kruijssen
4. G. Harris
5. L. Ferrarese
6. E. Peng
7. P. Harding
8. M. Alessi

Citations in the corpus

• A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, background): “Such cases include a few very small dwarfs (Peng et al. 2008; Georgiev et al. 2010) for which NGC ≤ 0 after subtraction of field contamination; or a few galaxies for which the imaging data simply did not reach deep enough to provide a sensible estimate of GC numbers (Kundu & Whitmore 2001a,b).”
• MODELING THE METALLICITY DISTRIBUTION OF GLOBULAR CLUSTERS (2010, unknown): “We later learned of a similar empirical relation for all types of massive galaxies, derived independently by Spitler & Forbes (2009) and Georgiev et al. (2010).”
• GALAXIES AT THE EXTREMES: ULTRA-DIFFUSE GALAXIES IN THE VIRGO CLUSTER (2015, background): “This yields a specific frequency of SN = 40±20, rather large (albeit with large uncertainties) for galaxies of this luminosity, which typically have SN = 10 − 20 with large spread (Peng et al. 2008, Georgiev et al. 2010).”
• Globular clusters as the relics of regular star formation in ‘normal’ high-redshift galaxies (2015, background): “Likewise, recent work (e.g.Forbes & Bridges 2010; Georgiev et al. 2010; Conroy, Loeb & Spergel 2011) seems to rule out that GC formation is the result of a high Jeans mass following recombination (Peebles & Dicke 1968), thermal instabilities in hot galaxy haloes (Fall & Rees 1985), or star…”