The GIRAFFE Inner Bulge Survey (GIBS)

Gonzalez, O. A.; Zoccali, M.; Vásquez, S.; Hill, V.; Rejkuba, M.; Valenti, E.; Rojas-Arriagada, Á.; Renzini, A.; Babusiaux, C.; Minniti, D.; Brown, Thomas M.

doi:10.1051/0004-6361/201526737

Cited by 71 publications

(145 citation statements)

References 83 publications

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“…6 and 7 show published magnesium abundances from Gonzalez et al (2011), Johnson et al (2014 and Alves-Brito et al (2010) that revise the same stars as in Meléndez et al (2008) and Ryde et al (2016) for red giants, from Hill et al (2011) and Gonzalez et al (2015) for Red Clump (RC) stars and from Bensby et al (2013) for microlensed dwarfs. The data are compared with models with ν SF = 3, 1 and 0.5 Gyr −1 .…”

Section: Comparison With Literature Oxygen Abundancesmentioning

confidence: 88%

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Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

Friaça

Barbuy

2017

A&A

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Context. Galactic bulge abundances can be best understood as indicators of bulge formation and nucleosynthesis processes by comparing them with chemo-dynamical evolution models. Aims. The aim of this work is to study the abundances of alpha-elements in the Galactic bulge, including a revision of the oxygen abundance in a sample of 56 bulge red giants. Methods. Literature abundances for O, Mg, Si, Ca and Ti in Galactic bulge stars are compared with chemical evolution models. For oxygen in particular, we reanalysed high-resolution spectra obtained using FLAMES+UVES on the Very Large Telescope, now taking each star's carbon abundances, derived from CI and C 2 lines, into account simultaneously.Results. We present a chemical evolution model of alpha-element enrichment in a massive spheroid that represents a typical classical bulge evolution. The code includes multi-zone chemical evolution coupled with hydrodynamics of the gas. Comparisons between the model predictions and the abundance data suggest a typical bulge formation timescale of 1-2 Gyr. The main constraint on the bulge evolution is provided by the O data from analyses that have taken the C abundance and dissociative equilibrium into account. Mg, Si, Ca and Ti trends are well reproduced, whereas the level of overabundance critically depends on the adopted nucleosynthesis prescriptions.

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Section: Comparison With Literature Oxygen Abundancesmentioning

confidence: 88%

“…Gonzalez et al (2015) and Ryde et al (2016). d) As regards the IMF, as stated in Sect. 2, our adopted IMF assumes the usual Salpeter index x IMF = 1.35 and extends to 100 M , whereas some chemical evolution models by other authors assume a different IMF.…”

Section: Discussionmentioning

confidence: 99%

Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

Friaça

Barbuy

2017

A&A

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“…• (Gonzalez et al 2015) and it will soon be completed by metallicities and in the near future by VVV proper motions. Preliminary results have also been published on larger-scale spectroscopic surveys that include the bulge in their field selection: the APOGEE survey (Majewski et al 2015;targeting 2MASS M-giants, Nidever et al 2012) and the Gaia-ESO survey (GES, Gilmore et al 2012;targeting VISTA K-giants, Rojas-Arriagada et al 2014).…”

Section: Global Kinematics Of Field Starsmentioning

confidence: 99%

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

Babusiaux

2016

Publ. Astron. Soc. Aust.

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Recent 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.

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“…Stars in the Galactic bulge thus occupy a wide range in the Metallicity Distribution Function (MDF), with [Fe/H] between −3.0 and +1.0 dex (Rich 1988;Zoccali et al 2003;Ness et al 2013a;Gonzalez et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The stellar halo in the inner Milky Way: predicted shape and kinematics

Pérez-Villegas

Portail

Gerhard

2016

Monthly Notices of the Royal Astronomical Society: Letters

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We have used N-body simulations for the Milky Way to investigate the kinematic and structural properties of the old metal-poor stellar halo in the barred inner region of the Galaxy. We find that the extrapolation of the density distribution for bulge RR Lyrae stars, ρ ∼ r −3 , approximately matches the number density of RR Lyrae in the nearby stellar halo. We follow the evolution of such a tracer population through the formation and evolution of the bar and box/peanut bulge in the N-body model. We find that its density distribution changes from oblate to triaxial, and that it acquires slow rotation in agreement with recent measurements. The maximum radial velocity is ∼ 15 − 25 km/s at |l| = 10• − 30 • , and the velocity dispersion is ∼ 120 km/s. Even though the simulated metal-poor halo in the bulge has a barred shape, just 12% of the orbits follow the bar, and it does not trace the peanut/X structure. With these properties, the RR Lyrae population in the Galactic bulge is consistent with being the inward extension of the Galactic metal-poor stellar halo.

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The GIRAFFE Inner Bulge Survey (GIBS)

Cited by 71 publications

References 83 publications

Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

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

The stellar halo in the inner Milky Way: predicted shape and kinematics

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