Metal abundances for a large sample of globular clusters in M87

1993 ◽  
Vol 106 ◽  
pp. 493 ◽  
Author(s):  
Myung G. Lee ◽  
Doug Geisler
Keyword(s):  
Globular Clusters ◽  
Large Sample ◽  
Metal Abundances

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.

scholarly journals The Chemical Abundances of the Halo Clusters of the Galaxy

1978 ◽  
Vol 80 ◽  
pp. 177-182
Author(s):  
R. Canterna ◽  
R. A. Schommer
Keyword(s):  
Globular Clusters ◽  
Broad Band ◽  
Mean Value ◽  
Red Giants ◽  
Galactocentric Distance ◽  
Chemical Abundances ◽  
Dwarf Spheroidal Galaxies ◽  
The Galaxy ◽  
Ursa Minor ◽  
Metal Abundances

Photometric metal abundances of individual red giants in eight extremely distant halo globular clusters and the Draco and Ursa Minor dwarf spheroidal galaxies have been obtained using the Washington broad-band system, C, M, T1, T2(Canterna 1976). Observations were made at the KPNO 2.1-m and CTIO 1.5-m telescopes. In Table I we list for each system the mean value of [Fe/H], the number of stars observed in each system, n, the Galactocentric distance, RGC, the intrinsic color of the giant branch at the level of the horizontal branch (HB), (B-V)o,g, and the fraction of HB stars bluer than the RR Lyrae gap, fB. Sources for unpublished color-magnitude diagram (CMD) data are: Pal 11 (Canterna and Schommer), Pal 12 (Canterna and Harris), and Ursa Minor (Schommer, Olszewski and Kunkel).

Metal abundances from Washington photometry of globular clusters in NGC 5128

1992 ◽  
Vol 104 ◽  
pp. 613 ◽  
Author(s):  
Gretchen L. H. Harris ◽  
Doug Geisler ◽  
Hugh C. Harris ◽  
James E. Hesser
Keyword(s):  
Globular Clusters ◽  
Metal Abundances

Metal abundances of RR Lyrae stars in globular clusters

1982 ◽  
Vol 261 ◽  
pp. 576 ◽  
Author(s):  
H. A. Smith ◽  
G. J. Perkins
Keyword(s):  
Globular Clusters ◽  
Rr Lyrae Stars ◽  
Rr Lyrae ◽  
Metal Abundances ◽  
Lyrae Stars

The eye of Gaia on globular cluster kinematics: Internal rotation

2019 ◽  
Vol 14 (S351) ◽  
pp. 516-519
Author(s):  
A. Sollima ◽  
H. Baumgardt ◽  
M. Hilker
Keyword(s):  
Internal Rotation ◽  
Globular Cluster ◽  
Globular Clusters ◽  
Stellar Systems ◽  
Large Sample ◽  
Data Release ◽  
Extensive Collection ◽  
Formation And Evolution ◽  
The Impact ◽  
Insight Into

AbstractI present the results of a survey of the kinematics of a large sample of Galactic globular clusters performed thanks to the synergy between the 2nd Gaia data release and the most extensive collection of radial velocities. This unprecedented dataset of 3D velocities of thousand of stars in 62 globular clusters has been used to investigate the rotation patterns of these stellar systems providing insight into the impact of two-body relaxation and tides on the formation and evolution of their rotation.

scholarly journals The Fundamental Plane of Globular Clusters

2005 ◽  
Vol 13 ◽  
pp. 181-182
Author(s):  
Dean E. McLaughlin
Keyword(s):  
Globular Clusters ◽  
Magellanic Clouds ◽  
Fundamental Plane ◽  
Large Sample ◽  
Cluster Energy ◽  
Young Clusters ◽  
Shed Light

AbstractThe fundamental plane of globular clusters can be expressed as a particular scaling of cluster energy vs. mass: Eb ~ M2. New calculations of energy and mass for a large sample of young clusters in the Magellanic Clouds may shed light on the origins of this scaling.

Sign in / Sign up

Export Citation Format

Share Document