Relative Ages of the Globular Cluster Subpopulations in M87

Recent Advances in High Dispersion Spectroscopy of Globular Cluster Stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900035610 ◽

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.

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Galactic orbits of stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900105340 ◽

1966 ◽

Vol 25 ◽

pp. 93-97

Author(s):

Richard Woolley

Keyword(s):

Globular Cluster ◽

Potential Field ◽

High Velocity ◽

Velocity Vector ◽

Variable Stars ◽

The Sun ◽

Proper Motions ◽

Rr Lyrae ◽

The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

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A Distance-Independent Age for the Globular Cluster M92

The Astronomical Journal ◽

10.1086/301560 ◽

2000 ◽

Vol 120 (4) ◽

pp. 1884-1891 ◽

Cited By ~ 34

Author(s):

F. Grundahl, ◽

D. A. VandenBerg, ◽

R. A. Bell, ◽

M. I. Andersen, ◽

P. B. Stetson

Keyword(s):

Globular Cluster

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Elemental Abundances in Five Stars in M54, A Globular Cluster Associated with the Sagittarius Galaxy

The Astronomical Journal ◽

10.1086/300996 ◽

1999 ◽

Vol 118 (3) ◽

pp. 1245-1251 ◽

Cited By ~ 42

Author(s):

Jeffery A. Brown ◽

George Wallerstein ◽

Guillermo Gonzalez

Keyword(s):

Globular Cluster ◽

Elemental Abundances

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Proton Capture Chains in Globular Cluster Stars. III. Abundances of Giants in the Second-Parameter Globular Cluster NGC 7006

The Astronomical Journal ◽

10.1086/300279 ◽

1998 ◽

Vol 115 (4) ◽

pp. 1500-1515 ◽

Cited By ~ 53

Author(s):

Robert P. Kraft ◽

Christopher Sneden ◽

Graeme H. Smith ◽

Matthew D. Shetrone ◽

Jon Fulbright

Keyword(s):

Globular Cluster ◽

Proton Capture

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The Globular Cluster System in the Inner Region of M87

The Astrophysical Journal ◽

10.1086/306865 ◽

1999 ◽

Vol 513 (2) ◽

pp. 733-751 ◽

Cited By ~ 107

Author(s):

Arunav Kundu ◽

Bradley C. Whitmore ◽

William B. Sparks ◽

F. Duccio Macchetto ◽

Stephen E. Zepf ◽

...

Keyword(s):

Globular Cluster ◽

Cluster System ◽

Globular Cluster System ◽

Inner Region

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The globular cluster system of the Auriga simulations

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1380 ◽

2020 ◽

Vol 496 (1) ◽

pp. 638-648 ◽

Cited By ~ 1

Author(s):

Timo L R Halbesma ◽

Robert J J Grand ◽

Facundo A Gómez ◽

Federico Marinacci ◽

Rüdiger Pakmor ◽

...

Keyword(s):

Globular Cluster ◽

Milky Way ◽

Cluster Formation ◽

Solar Radius ◽

High Mass ◽

Formation Model ◽

The Galaxy ◽

High Mass Loss ◽

Globular Cluster System ◽

Varying Mass

ABSTRACT We investigate whether the galaxy and star formation model used for the Auriga simulations can produce a realistic globular cluster (GC) population. We compare statistics of GC candidate star particles in the Auriga haloes with catalogues of the Milky Way (MW) and Andromeda (M31) GC populations. We find that the Auriga simulations do produce sufficient stellar mass for GC candidates at radii and metallicities that are typical for the MW GC system (GCS). We also find varying mass ratios of the simulated GC candidates relative to the observed mass in the MW and M31 GCSs for different bins of galactocentric radius metallicity (rgal–[Fe/H]). Overall, the Auriga simulations produce GC candidates with higher metallicities than the MW and M31 GCS and they are found at larger radii than observed. The Auriga simulations would require bound cluster formation efficiencies higher than 10 per cent for the metal-poor GC candidates, and those within the Solar radius should experience negligible destruction rates to be consistent with observations. GC candidates in the outer halo, on the other hand, should either have low formation efficiencies, or experience high mass-loss for the Auriga simulations to produce a GCS that is consistent with that of the MW or M31. Finally, the scatter in the metallicity as well as in the radial distribution between different Auriga runs is considerably smaller than the differences between that of the MW and M31 GCSs. The Auriga model is unlikely to give rise to a GCS that can be consistent with both galaxies.

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