Globular Cluster Systems

By W. Harris. 2001

243 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Globular Cluster Systems in Brightest Cluster Galaxies: Bimodal Metallicity Distributions and the Nature of the High-Luminosity Clusters (2005, background): “If as noted earlier the GCLF has a normal Gaussian-like shape with turnover at MI = −8.4 and dispersion σ ≃ 1.4 magnitudes (Harris 2001), then the total GCS population we are drawing from in all eight galaxies, and within the ACS field of view, is nearly 15000 clusters.”
The Colors of Dwarf Elliptical Galaxy Globular Cluster Systems, Nuclei, and Stellar Halos (2004, background): “, Aaronson 1983; but see Geha et al. 2002), whereas star clusters do not have associated dark matter halos (Pryor et al. 1989;Moore 1996). Massive globular clusters are compact, high-surface brightness objects, while dE/dSphs are diffuse and extended with decreasing surface brightnesses with decreas”
The stellar halo of the Galaxy (2008, background): “It should be stressed, however, that the exact sites and conditions under which the various neutron-capture elements are produced, particularly at very low metallicities, are still somewhat uncertain (Travaglio et al. 2004; Arnould et al. 2007).”
Age and Metallicity Distribution of the Galactic Bulge from Extensive Optical and Near-IR Stellar Photometry (2002, background): “Hence, we do not hesitate to refer to them as bulge globular clusters (see also Forbes et al. 2001; Harris 1976, 2001; Zinn 1996).”
The Globular Cluster System of NGC 1399. I. A Wide-Field Photometric Study (2003, background): “With = 1.2, 1.3, and 1.4, which are used for elliptical galaxies (Ashman & Zepf 1998), we find TOM of 23.98 0.11, 24.02 0.09, and 24.05 0.12, respectively.”
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).”
Stellar-mass black holes in star clusters: implications for gravitational-wave radiation (2009, background): “The primordial binary fraction in GCs and their period distribution are still widely debated (Ashman & Zepf 1998; Bellazzini et al. 2002; Sommariva et al. 2009).”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, methodology): “Similar transitions have been found in the Milky Way and NGC 1407, at ∼ 10 and ∼ 60 kpc, respectively (Harris 2001; Forbes et al. 2011).”
Nuclear star clusters (2009, methodology): “Therefore, it remains unknown if a similar trend towards lowmetallicity NSCs exists in late-type galaxies, although the colors of NSCs in these galaxies do seem to be typical of metal-poor GCs (Georgiev et al. 2009).”
Formation of Globular Clusters in Hierarchical Cosmology (2003, background): “Extensive observational surveys of GC systems in the Milky Way and other galaxies have been compiled during the past two decades (e.g., Harris 2001).”
New Insights from HST Studies of Globular Cluster Systems. I. Colors, Distances, and Specific Frequencies of 28 Elliptical Galaxies (2001, methodology): “5 recommended by Holtzman et al. (1995b), consequently the zero points reported below do not include this factor.”
Extragalactic Globular Clusters and Galaxy Formation (2006, methodology): “Harris (2001) provided a good overview of the current situation.”
REVISITING WITH CHANDRA THE SCALING RELATIONS OF THE X-RAY EMISSION COMPONENTS (BINARIES, NUCLEI, AND HOT GAS) OF EARLY-TYPE GALAXIES (2010, methodology): “For example, for NGC 4526 Peng et al. (2008) measured SN = 1.09 with the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) data as part of the ACS Virgo Cluster Survey, while SN = 7.4–7.7 in Kissler-Patig (1997), Ashman & Zepf (1998), and Harris & Harris (1999).”
VLT spectroscopy of globular cluster systems - II. Spectroscopic ages, metallicities and [α/Fe] ratios of globular clusters in early-type galaxies (2005, background): “Arimoto & Yoshii 1987, etc.) the majority of stars in earlytype galaxies forms early, at redshifts z >∼ 2.”