Globular cluster evolution in the Galaxy - A global view

1987 ◽  
Vol 322 ◽  
pp. 113 ◽  
Author(s):  
David F. Chernoff ◽  
Stuart L. Shapiro
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution ◽  
Global View ◽  
The Galaxy

Galactic orbits of stars

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.

scholarly journals The globular cluster system of the Auriga simulations

2020 ◽  
Vol 496 (1) ◽  
pp. 638-648 ◽  
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.

Primordial binaries and globular cluster evolution

Nature ◽  
1989 ◽  
Vol 339 (6219) ◽  
pp. 40-42 ◽  
Author(s):  
Jeremy Goodman ◽  
Piet Hut
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution

scholarly journals FSR1767 - a new globular cluster in the Galaxy

2007 ◽  
Vol 381 (1) ◽  
pp. L45-L49 ◽  
Author(s):  
C. Bonatto ◽  
E. Bica ◽  
S. Ortolani ◽  
B. Barbuy
Keyword(s):  
Globular Cluster ◽  
The Galaxy

scholarly journals The Globular Cluster System of the Galaxy NGC 6876

Galaxies ◽  
2017 ◽  
Vol 5 (3) ◽  
pp. 30 ◽  
Author(s):  
Ana Ennis ◽  
Lilia Bassino ◽  
Juan Caso
Keyword(s):  
Globular Cluster ◽  
Cluster System ◽  
The Galaxy ◽  
Globular Cluster System

scholarly journals Metallicity maps of the globular cluster system in the Galaxy

1993 ◽  
Vol 402 ◽  
pp. L53 ◽  
Author(s):  
Emilio J. Alfaro ◽  
Jesus Cabrera-Cano ◽  
Antonio J. Delgado
Keyword(s):  
Globular Cluster ◽  
Cluster System ◽  
The Galaxy ◽  
Globular Cluster System

scholarly journals A Global View of Molecule-Forming Clouds in the Galaxy

2015 ◽  
Vol 11 (S315) ◽  
Author(s):  
Steven J. Gibson ◽  
Ward S. Howard ◽  
Christian S. Jolly ◽  
Jonathan H. Newton ◽  
Aaron C. Bell ◽  
...  
Keyword(s):  
Line Emission ◽  
Cloud Models ◽  
Global View ◽  
The Galaxy ◽  
Atomic Gas

AbstractWe have mapped cold atomic gas in 21cm line H i self-absorption (HISA) at arcminute resolution over more than 90% of the Milky Way's disk. To probe the formation of H2 clouds, we have compared our HISA distribution with CO J = 1-0 line emission. Few HISA features in the outer Galaxy have CO at the same position and velocity, while most inner-Galaxy HISA has overlapping CO. But many apparent inner-Galaxy HISA-CO associations can be explained as chance superpositions, so most inner-Galaxy HISA may also be CO-free. Since standard equilibrium cloud models cannot explain the very cold H i in many HISA features without molecules being present, these clouds may instead have significant CO-dark H2.

scholarly journals An Overview of the Globular Cluster System of the Galaxy

1988 ◽  
Vol 126 ◽  
pp. 37-48
Author(s):  
Robert Zinn
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
Milky Way ◽  
Galactic Center ◽  
Galactic Plane ◽  
Cluster System ◽  
Open Clusters ◽  
The Galaxy ◽  
Globular Cluster System ◽  
Harlow Shapley

Harlow Shapley (1918) used the positions of globular clusters in space to determine the dimensions of our Galaxy. His conclusion that the Sun does not lie near the center of the Galaxy is widely recognized as one of the most important astronomical discoveries of this century. Nearly as important, but much less publicized, was his realization that, unlike stars, open clusters, HII regions and planetary nebulae, globular clusters are not concentrated near the plane of the Milky Way. His data showed that the globular clusters are distributed over very large distances from the galactic plane and the galactic center. Ever since this discovery that the Galaxy has a vast halo containing globular clusters, it has been clear that these clusters are key objects for probing the evolution of the Galaxy. Later work, which showed that globular clusters are very old and, on average, very metal poor, underscored their importance. In the spirit of this research, which started with Shapley's, this review discusses the characteristics of the globular cluster system that have the most bearing on the evolution of the Galaxy.

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