scholarly journals Elemental abundances in the Galactic bulge from microlensed dwarf stars

2009 ◽  
Vol 5 (S265) ◽  
pp. 346-347
Author(s):  
T. Bensby ◽  
S. Feltzing ◽  
J. A. Johnson ◽  
A. Gould ◽  
H. Sana ◽  
...  
Keyword(s):  
Full Range ◽  
Galactic Bulge ◽  
Dwarf Stars ◽  
Elemental Abundances ◽  
Thick Disc ◽  
Abundance Trends ◽  
Subgiant Stars

AbstractWe present elemental abundances of 13 microlensed dwarf and subgiant stars in the Galactic bulge, which constitute the largest sample to date. We show that these stars span the full range of metallicity from Fe/H= −0.8 to +0.4, and that they follow well-defined abundance trends, coincident with those of the Galactic thick disc.

scholarly journals Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars

2017 ◽  
Vol 605 ◽  
pp. A89 ◽  
Author(s):  
T. Bensby ◽  
S. Feltzing ◽  
A. Gould ◽  
J. C. Yee ◽  
J. A. Johnson ◽  
...  
Keyword(s):  
Chemical Evolution ◽  
Galactic Bulge ◽  
Subgiant Stars

The Galactic Bulge and the Thick Disc

1992 ◽  
pp. 77-79 ◽  
Author(s):  
M. W. Feast ◽  
P. A. Whitelock ◽  
R. Sharples
Keyword(s):  
Galactic Bulge ◽  
Thick Disc

scholarly journals On the age of Galactic bulge microlensed dwarf and subgiant stars

2015 ◽  
Vol 577 ◽  
pp. A72 ◽  
Author(s):  
G. Valle ◽  
M. Dell’Omodarme ◽  
P. G. Prada Moroni ◽  
S. Degl’Innocenti
Keyword(s):  
Galactic Bulge ◽  
Subgiant Stars

scholarly journals Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars

2010 ◽  
Vol 512 ◽  
pp. A41 ◽  
Author(s):  
T. Bensby ◽  
S. Feltzing ◽  
J. A. Johnson ◽  
A. Gould ◽  
D. Adén ◽  
...  
Keyword(s):  
Chemical Evolution ◽  
Galactic Bulge ◽  
Subgiant Stars

scholarly journals Globular Clusters in the Galactic Bulge

2016 ◽  
Vol 33 ◽  
Author(s):  
E. Bica ◽  
S. Ortolani ◽  
B. Barbuy
Keyword(s):  
Globular Clusters ◽  
Deep Understanding ◽  
Selective Absorption ◽  
Galactic Bulge ◽  
Chemical Abundances ◽  
Elemental Abundances ◽  
The Galaxy ◽  
Formation And Evolution ◽  
Future Work ◽  
Shed Light

AbstractA view of the Galactic bulge by means of their globular clusters is fundamental for a deep understanding of its formation and evolution. Connections between the globular cluster and field star properties in terms of kinematics, orbits, chemical abundances, and ages should shed light on different stellar population components. Based on spatial distribution and metallicity, we define a probable best list of bulge clusters, containing 43 entries. Future work on newly discovered objects, mostly from the VVV survey, is suggested. These candidates might alleviate the issue of missing clusters on the far side of the bulge. We discuss the reddening law affecting the cluster distances towards the centre of the Galaxy, and conclude that the most suitable total-to-selective absorption value appears to be RV=3.2, in agreement with recent analyses. An update of elemental abundances for bulge clusters is provided.

scholarly journals Evidence of outflow from the Galactic bulge imprinted in stellar elemental abundances

2007 ◽  
Vol 3 (S245) ◽  
pp. 369-370
Author(s):  
Takuji Tsujimoto
Keyword(s):  
Black Hole ◽  
Galactic Halo ◽  
Elemental Abundance ◽  
Stellar Disk ◽  
Galactic Bulge ◽  
Interstellar Gas ◽  
Elemental Abundances ◽  
The Galaxy ◽  
Low Metallicity ◽  
Halo Gas

AbstractWe explore the elemental abundance features of metal-rich disk stars, highlighting the comparisons made with those of the recently revealed Galactic bulge stars. A similarity between two of the comparisons leads to a new theoretical picture of the bulge-disk connection in the Galaxy, where a supermassive black hole resides at the center. We postulate that a metal-rich outflow, triggered by feedback from a black hole, was generated and quenched the star formation, which had lasted several billion years in the bulge. The expelled gas cooled down in the Galactic halo without escaping from the gravitational potential of the Galaxy. The gas gradually started to accrete to the disk around five billion years ago, corresponding to the time of sun's birth, and replaced a low-metallicity halo gas that had been accreting over nearly ten billion years. The metal-rich infalling gas, whose elemental abundance reflects that of metal-rich bulge stars, mixed with the interstellar gas already present in the disk. Stars formed from the mixture compose the metal-rich stellar disk.

scholarly journals The Disc Origin of the Milky Way Bulge

2016 ◽  
Vol 33 ◽  
Author(s):  
P. Di Matteo
Keyword(s):  
Milky Way ◽  
Complex Structure ◽  
Galactic Bulge ◽  
Galactic Disc ◽  
Major Step ◽  
Thick Disc ◽  
Global Properties ◽  
Out Of Plane ◽  
The Galaxy ◽  
Main Components

AbstractThe Galactic bulge, that is the prominent out-of-plane over-density present in the inner few kiloparsecs of the Galaxy, is a complex structure, as the morphology, kinematics, chemistry, and ages of its stars indicate. To understand the nature of its main components—those at [Fe/H] ≳ −1 dex—it is necessary to make an inventory of the stellar populations of the Galactic disc(s), and of their borders: the chemistry of the disc at the solar vicinity, well known from detailed studies of stars over many years, is not representative of the whole disc. This finding, together with the recent revisions of the mass and sizes of the thin and thick discs, constitutes a major step in understanding the bulge complexity. N-body models of a boxy-/peanut-shaped bulge formed from a thin disc through the intermediary of a bar have been successful in interpreting a number of global properties of the Galactic bulge, but they fail in reproducing the detailed chemo-kinematic relations satisfied by its components and their morphology. It is only by adding the thick disc to the picture that we can understand the nature of the Galactic bulge.

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