Stellar Populations in the Galactic Bulge

2006 ◽  
pp. 435-438
Author(s):  
Mathias Schultheis ◽  
Bernhard Aringer ◽  
Ariane Lançon
Keyword(s):  
Stellar Populations ◽  
Galactic Bulge

scholarly journals Metal-poor globular clusters of the galactic bulge

2009 ◽  
Vol 5 (S265) ◽  
pp. 344-345
Author(s):  
B. Barbuy ◽  
S. Ortolani ◽  
M. Zoccali ◽  
V. Hill ◽  
D. Minniti ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Stellar Populations ◽  
Galactic Bulge ◽  
Abundance Pattern ◽  
Individual Stars

AbstractVery few abundance analyses of individual stars in metal-poor globular clusters in the galactic bulge are available. The main purpose of this study is to derive abundances in individual stars of such clusters, in order to establish their abundance pattern, trying to characterize the oldest bulge stellar populations.

Stellar Populations in the Galactic Bulge

2008 ◽  
pp. 376-376
Author(s):  
M. Schultheis ◽  
S. Ganesh ◽  
A. Omont ◽  
B. Aringer ◽  
A. C. Robin
Keyword(s):  
Stellar Populations ◽  
Galactic Bulge

scholarly journals Chemodynamical History of the Galactic Bulge

2018 ◽  
Vol 56 (1) ◽  
pp. 223-276 ◽  
Author(s):  
Beatriz Barbuy ◽  
Cristina Chiappini ◽  
Ortwin Gerhard
Keyword(s):  
Stellar Population ◽  
Chemical Properties ◽  
Stellar Populations ◽  
Observational Evidence ◽  
Galactic Bulge ◽  
Large Samples ◽  
Self Consistent ◽  
History Of ◽  
Bulge Formation ◽  
And Chemical Properties

The Galactic Bulge can uniquely be studied from large samples of individual stars and is therefore of prime importance for understanding the stellar population structure of bulges in general. Here the observational evidence on the kinematics, chemical composition, and ages of Bulge stellar populations based on photometric and spectroscopic data is reviewed. The bulk of Bulge stars are old and span a metallicity range of −1.5≲[Fe/H]≲+0.5. Stellar populations and chemical properties suggest a star-formation timescale below ∼2 Gyr. The overall Bulge is barred and follows cylindrical rotation, and the more metal-rich stars trace a box/peanut (B/P) structure. Dyna-mical models demonstrate the different spatial and orbital distributions of metal-rich and metal-poor stars. We discuss current Bulge-formation scenarios based on dynamical, chemical, chemodynamical, and cosmological models. Despite impressive progress, we do not yet have a successful fully self-consistent chemodynamical Bulge model in the cosmological framework, and we will also need a more extensive chrono-chemical-kinematic 3D map of stars to better constrain such models.

A review of the chemical abundances and kinematics of the Galactic bulge

2013 ◽  
Vol 9 (S298) ◽  
pp. 28-39 ◽  
Author(s):  
Livia Origlia
Keyword(s):  
Galactic Center ◽  
State Of The Art ◽  
Complex Structure ◽  
Stellar Populations ◽  
Galactic Bulge ◽  
Future Perspectives ◽  
Chemical Abundances ◽  
Center Region ◽  
Infrared Surveys

AbstractThis review will attempt to draw a state of the art observational picture of the Galactic bulge. The main chemical, kinematic and evolutionary properties of the gas and stellar populations in the barred bulge and towards the Galactic center region will be discussed in the context of the possible formation scenarios. Future perspectives for our comprehension of the complex structure of the Galactic bulge from ongoing and foreseen optical and infrared surveys will be also highlighted.

scholarly journals Stellar parameters in the bulge cluster NGC 6553

1997 ◽  
Vol 189 ◽  
pp. 203-206 ◽  
Author(s):  
B. Barbuy ◽  
S. Ortolani ◽  
E. Bica ◽  
A. Renzini ◽  
M.D. Guarnieri
Keyword(s):  
Globular Clusters ◽  
Stellar Population ◽  
Spectroscopic Analysis ◽  
Galactic Center ◽  
Stellar Populations ◽  
The Sun ◽  
Galactic Bulge ◽  
Complete Understanding ◽  
Luminosity Functions ◽  
Bulge Formation

Globular clusters in the Galactic bulge form a flattened system, extending from the Galactic center to about 4.5 kpc from the Sun (Barbuy et al. 1997). A study of abundance ratios in these clusters is very important for a more complete understanding of the bulge formation. In this work we present a spectroscopic analysis of individual stars in NGC 6553. This cluster is a key one because it is located at d⊙ ≍ 5.1 kpc, therefore relatively close to us, and at the same time it is representative of the Galactic bulge stellar population: (a) Ortolani et al. (1995) showed that NGC 6553 and NGC 6528 show very similar Colour-Magnitude Diagrams (CMDs), and NGC 6528 is located at d⊙ ≍ 7.83 kpc, very close to the Galactic center; (b) the stellar populations of the Baade Window is also very similar to that of NGC 6553 and NGC 6528 as Ortolani et al. (1995) have shown by comparing their luminosity functions.

scholarly journals Chemical evolution of the Galactic bulge: different stellar populations and possible gradients

2012 ◽  
Vol 548 ◽  
pp. A60 ◽  
Author(s):  
V. Grieco ◽  
F. Matteucci ◽  
A. Pipino ◽  
G. Cescutti
Keyword(s):  
Chemical Evolution ◽  
Stellar Populations ◽  
Galactic Bulge

scholarly journals Correlations between Kinematics and Metallicity in the Galactic Bulge: A Review

2016 ◽  
Vol 33 ◽  
Author(s):  
Carine Babusiaux
Keyword(s):  
Density Profile ◽  
Large Scale ◽  
Milky Way ◽  
Stellar Populations ◽  
The Other ◽  
Galactic Bulge ◽  
Secular Evolution

AbstractRecent large-scale surveys of galactic bulge stars allowed to build a detailed map of the bulge kinematics. The bulge exhibits cylindrical rotation consistent with a disky origin which evolved through bar-driven secular evolution. However, correlations between metallicity and kinematics complicate this picture. In particular a metal-poor component with distinct kinematic signatures has been detected. Its origin, density profile and link with the other Milky Way stellar populations are currently still poorly constrained.

Stellar Populations in the Galactic Bulge

1996 ◽  
Vol 169 ◽  
pp. 317-327
Author(s):  
H.J. Habing
Keyword(s):  
Milky Way ◽  
Stellar Populations ◽  
Galactic Bulge ◽  
Central Cluster ◽  
Intimate Connection ◽  
The Subject ◽  
Sgr A

In this review I discuss stars in the bulge of our Milky Way, but I exclude stars within a few parsec from Sgr A West; they are the subject of other reviews at this Symposium. We should, however, not forget that there may be an intimate connection between the central cluster and the bulge: bulge stars may eject matter that feeds the monster at the center and eruptions by this monster may have an important effect on the bulge.

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