A Complete Sample of Globular Clusters in NGC 5128

1988 ◽  
pp. 545-546 ◽  
Author(s):  
Ray Sharples
Keyword(s):  
Globular Clusters ◽  
Complete Sample

scholarly journals The Globular Cluster System of NGC 5128

2002 ◽  
Vol 207 ◽  
pp. 315-317
Author(s):  
Marina Rejkuba
Keyword(s):  
High Resolution ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Spiral Galaxies ◽  
Similar Magnitude ◽  
Complete Sample ◽  
Magnitude Diagram ◽  
Kolmogorov Smirnov ◽  
Bona Fide ◽  
Globular Cluster System

On the basis of high resolution ground-based images, taken with VLT and FORS1, 71 bona fide globular clusters were discovered in the halo of NGC 5128. Only 5 of these clusters were previously known. In a UV color-magnitude diagram for the complete sample of 71 clusters and a (U—V)0vs. (V—Ks)0 color-color diagram for a subsample of 23 clusters, the objects span a similar magnitude and color range as the globular clusters in the MW and M31. The GCLFs spanning −10.1 < MV < −4.9 and −9.3 < MU < −3.3 have been constructed. These are the deepest GCLFs of in a gE made so far. The Kolmogorov-Smirnov statistics show that GCLF of the giant elliptical NGC 5128 is consistent with the ones of spiral galaxies like the MW and M31.

scholarly journals A Complete Sample of Globular Clusters in NGC 5128

1988 ◽  
Vol 126 ◽  
pp. 545-546
Author(s):  
Ray Sharples
Keyword(s):  
Power Law ◽  
Density Profile ◽  
Globular Clusters ◽  
Elliptical Galaxy ◽  
Major Axis ◽  
Cluster System ◽  
Radial Velocities ◽  
Complete Sample ◽  
The Core ◽  
The Galaxy

We present the results of an unbiased survey to search for globular clusters around the nearby elliptical galaxy NGC 5128. A total of 44 clusters has been identified on the basis of radial velocities alone. The cluster system appears to be flattened towards the major axis of the galaxy but does not show any dynamically significant rotation. There is a deficit of clusters in the core when compared with the power law density profile seen at large radii.

Recent Advances in High Dispersion Spectroscopy of Globular Cluster Stars

1988 ◽  
Vol 132 ◽  
pp. 525-530
Author(s):  
Raffaele G. Gratton
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
High Dispersion ◽  
Photographic Material ◽  
Recent Advances ◽  
Metal Abundances ◽  
Ccd Detectors ◽  
Major Progress

The use CCD detectors has allowed a major progress in abundance derivations for globular cluster stars in the last years. Abundances deduced from high dispersion spectra now correlates well with other abundance indicators. I discuss some problems concerning the derivation of accurate metal abundances for globular clusters using high dispersion spectra from both the old photographic and the most recent CCD data. The discrepant low abundances found by Cohen (1980), from photographic material for M71 giants, are found to be due to the use of too high microturbulences.

The Formation and Evolution of Candidate Young Globular Clusters in NGC 3256

1999 ◽  
Vol 118 (2) ◽  
pp. 752-764 ◽  
Author(s):  
Stephen E. Zepf ◽  
Keith M. Ashman ◽  
Jayanne English ◽  
Kenneth C. Freeman ◽  
Ray M. Sharples
Keyword(s):  
Globular Clusters ◽  
Formation And Evolution

Extending the Red Giant Branch versus Metallicity Calibration toward Metal-poor Systems: Near-Infrared Photometry of the Galactic Globular Clusters M56 and M15

2000 ◽  
Vol 119 (5) ◽  
pp. 2274-2281 ◽  
Author(s):  
Valentin D. Ivanov ◽  
Jordanka Borissova ◽  
Almudena Alonso-Herrero ◽  
Tatiana Russeva
Keyword(s):  
Globular Clusters ◽  
Near Infrared ◽  
Infrared Photometry ◽  
Galactic Globular Clusters ◽  
Red Giant

Aluminum Abundances, Deep Mixing, and the Blue-Tail Second- Parameter Effect in the Globular Clusters M3 and M1 3

2000 ◽  
Vol 120 (3) ◽  
pp. 1364-1383 ◽  
Author(s):  
Robert M. Cavallo ◽  
Neil M. Nagar
Keyword(s):  
Globular Clusters ◽  
Deep Mixing

Space Velocities of Globular Clusters. III. Cluster Orbits and Halo Substructure

1999 ◽  
Vol 117 (4) ◽  
pp. 1792-1815 ◽  
Author(s):  
Dana I. Dinescu ◽  
Terrence M. Girard ◽  
William F. van Altena
Keyword(s):  
Globular Clusters

Luminosity Functions for Globular Clusters

1998 ◽  
Vol 509 (1) ◽  
pp. 192-202 ◽  
Author(s):  
Fabio Silvestri ◽  
Paolo Ventura ◽  
Francesca D'Antona ◽  
Italo Mazzitelli
Keyword(s):  
Globular Clusters ◽  
Luminosity Functions

scholarly journals Effects of initial density profiles on massive star cluster formation in giant molecular clouds

2021 ◽  
Author(s):  
Yingtian Chen ◽  
Hui Li ◽  
Mark Vogelsberger
Keyword(s):  
Angular Momentum ◽  
Star Formation ◽  
Molecular Clouds ◽  
Globular Clusters ◽  
Cluster Formation ◽  
Initial Density ◽  
Giant Molecular Clouds ◽  
Density Profiles ◽  
Stellar Feedback ◽  
Gas Accretion

Abstract We perform a suite of hydrodynamic simulations to investigate how initial density profiles of giant molecular clouds (GMCs) affect their subsequent evolution. We find that the star formation duration and integrated star formation efficiency of the whole clouds are not sensitive to the choice of different profiles but are mainly controlled by the interplay between gravitational collapse and stellar feedback. Despite this similarity, GMCs with different profiles show dramatically different modes of star formation. For shallower profiles, GMCs first fragment into many self-gravitation cores and form sub-clusters that distributed throughout the entire clouds. These sub-clusters are later assembled ‘hierarchically’ to central clusters. In contrast, for steeper profiles, a massive cluster is quickly formed at the center of the cloud and then gradually grows its mass via gas accretion. Consequently, central clusters that emerged from clouds with shallower profiles are less massive and show less rotation than those with the steeper profiles. This is because 1) a significant fraction of mass and angular momentum in shallower profiles is stored in the orbital motion of the sub-clusters that are not able to merge into the central clusters 2) frequent hierarchical mergers in the shallower profiles lead to further losses of mass and angular momentum via violent relaxation and tidal disruption. Encouragingly, the degree of cluster rotations in steeper profiles is consistent with recent observations of young and intermediate-age clusters. We speculate that rotating globular clusters are likely formed via an ‘accretion’ mode from centrally-concentrated clouds in the early Universe.

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