Extragalactic Globular Clusters and Galaxy Formation

By J. Brodie, J. Strader. 2006

620 citations recorded by the source corpus.

Globular cluster (GC) systems have now been studied in galaxies ranging from dwarfs to giants and spanning the full Hubble sequence of morphological types. Imaging and spectroscopy with the Hubble Space Telescope and large ground-based telescopes have together established that most galaxies have bimodal color distributions that reflect two subpopulations of old GCs: metal-poor and metal-rich. The characteristics of both subpopulations are correlated with those of their parent galaxies. We argue that metal-poor GCs formed in low-mass dark matter halos in the early universe and that their properties reflect biased galaxy assembly. The metal-rich GCs were born in the subsequent dissipational buildup of their parent galaxies and their ages and abundances indicate that most massive early-type galaxies formed the bulk of their stars at early times. Detailed studies of both subpopulations offer some of the strongest constraints on hierarchical galaxy formation that can be obtained in the near-field.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c63d8f68d11859b67baefaeaa20c2a96d7929622

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Citations in the corpus

A Nearby Repeating Fast Radio Burst in the Direction of M81 (2021, background): “Though unremarkable, its presence in the FRB localization region is still noteworthy, as globular clusters in the Milky Way are known to host several exotic systems, like MSPs, blue stragglers, and low-mass X-ray binaries (LMXBs; Brodie & Strader 2006).”
THE NUCLEUS OF THE SAGITTARIUS DSPH GALAXY AND M54: A WINDOW ON THE PROCESS OF GALAXY NUCLEATION (2008, background): “…of the tidal shredding of their host galaxies that once orbited the Milky Way and/or M31 (see Mackey & van den Bergh 2005; Federici et al. 2007; Brodie & Strader 2006, and references therein), or even that most/all globulars were nuclei of Galactic building blocks (i.e. dwarf galaxies, see…”
The dragon simulations: globular cluster evolution with a million stars (2016, background): “On the other hand, galactic mergers create populations of GCs, so the merging history of massive galaxies could be reflected in the properties of their GC systems (Brodie & Strader 2006).”
The mass function of young star clusters in spiral galaxies (2008, background): “A large fraction of all star formation occurs in clusters (Lada & Lada 2003), and massive, long-lived globular clusters (GCs) are potentially useful tracers of stellar populations in their parent galaxies (Brodie & Strader 2006).”
BLACK HOLE TRIPLE DYNAMICS: A BREAKDOWN OF THE ORBIT AVERAGE APPROXIMATION AND IMPLICATIONS FOR GRAVITATIONAL WAVE DETECTIONS (2013, background): “If we take a globular number density of 10/Mpc3 (Brodie & Strader 2006), and that BH-BH mergers can be seen out to a sky-averaged distance of 1 Gpc (as expected for 10 M⊙ − 10 M⊙ coalescences), and if we assume that mergers are distributed uniformly over the lifetimes of the globulars (as opposed…”
The bifurcated age–metallicity relation of Milky Way globular clusters and its implications for the accretion history of the galaxy (2013, background): “The primary theories for the assembly of GC systems in large galaxies (see review by Brodie & Strader 2006) are: accretion of GCs in dwarf galaxies during hierarchical assembly (Cote, Marzke & West 1998), merging of large galaxies (Ashman & Zepf 1992), and in-situ formation (Forbes, Brodie &…”
Globular cluster systems in nearby dwarf galaxies – III. Formation efficiencies of old globular clusters (2010, background): “den Bergh 2000; Harris 1991, 2003; Brodie & Strader 2006, and references therein).”
A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, background): “…have systematically lower SN than ellipticals, field E’s have lower SN than ones in rich clusters of galaxies, and dE’s in denser environments favor higher SN (e.g. Hanes 1977; Harris & van den Bergh 1981; van den Bergh 1982, 2000; Durrell et al. 1996; Harris 2001; Brodie & Strader 2006, and P08).”
Short-Duration Gamma-Ray Bursts (2013, background): “…GRBs originating in globular clusters will also lead to the prediction of a Short-Duration Gamma-Ray Bursts31 dominant population of early-type hosts since the globularcluster specific frequency is several times higher in early-type than in late-type galaxies (Harris 1991, Brodie & Strader 2006).”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “…found in nature to simple stellar populations (SSPs), such star clusters provide both important probes of galaxy formation and test beds for stellar dynamical and evolutionary models (see, e.g., the reviews of Harris 2001; West et al. 2004; Brodie & Strader 2006; Portegies Zwart et al. 2010).”
Galaxy Masses: A Review (2013, background): “3) A bimodality in the colour distribution of GCs in bright ETGs is often observed (Brodie & Strader 2006), which may then call for several decoupled dynamical components in the final modelling.”
A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “GCs are some of the oldest objects in the Universe (e.g. Brodie & Strader 2006), although GC-like objects continue to form in the present day (see § 2.4.1).”
THE FORMATION OF ECCENTRIC COMPACT BINARY INSPIRALS AND THE ROLE OF GRAVITATIONAL WAVE EMISSION IN BINARY–SINGLE STELLAR ENCOUNTERS (2013, background): “(52) To express the above rate in units of volume, we have assumed that the density of galaxies is ngal = 0.1 Mpc−3 and each galaxy has 100 globular clusters, NGC = 102, implying 10 GC/Mpc−3 (Brodie & Strader 2006).”
Re-evaluating old stellar populations (2018, background): “Globular clusters are relatively small systems and may have very low total masses (104 − 106 M , see Brodie & Strader 2006).”
MODELING THE METALLICITY DISTRIBUTION OF GLOBULAR CLUSTERS (2010, background): “Red clusters are usually more spatially concentrated than blue clusters (Brodie & Strader 2006).”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, background): “Similar studies of external galaxies are generally confined to GC color, which is used as a metallicity proxy because of the generally large ages found for the GCs (e.g., Brodie & Strader 2006).”
Globular clusters as the relics of regular star formation in ‘normal’ high-redshift galaxies (2015, background): “There is a wealth of reviews discussing GCs in the nearby Universe (e.g.Harris 1991; Brodie & Strader 2006; Gratton, Carretta & Bragaglia 2012).”
THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED METHOD ALONG WITH COLOR–MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES (2013, background): “For instance, in their extensive review, Brodie & Strader (2006) argued that the most metal-poor GCs formed in low-mass dark matter halos in the early universe (at redshifts z > 10), whereas metal-rich systems were created during the subsequent mergers of gas-rich structures that built up the…”