EDP Sciences
Free Access
Issue
A&A
Volume 545, September 2012
Article Number A133
Number of page(s) 11
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361/201118558
Published online 20 September 2012

Online material

thumbnail Fig. 3

Barred-disk model. Distribution of the azimuthal velocity and metallicity after an evolution of 0, 0.1, 0.4 Gyr. Left panels: colour contour plot showing the rotation-metallicity distribution, Vφ vs. [Fe/H], of the particles in the solar annulus, 8 kpc  < R < 10 kpc and 1.5 kpc  <  | z |  < 2.0 kpc. The dashed white line indicates the linear fit in the central region of the distribution, including all particles with  −0.55 <  [Fe/H]  <  − 0.35 and Vφ > 50 km s-1. Right panels: the colour contour plot represents the distribution of the mean original radius,  ⟨ R0 ⟩ , as a function of ([Fe/H],Vφ) of the same particles shown in the left plot. Here, the dotted white lines mark the iso-contours at  ⟨ R0 ⟩  = 6 kpc, 8 kpc, 10 kpc, and 12 kpc. The black contours indicate the iso-density levels of the ([Fe/H],Vφ) distribution shown in the left panel.

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thumbnail Fig. 4

Distribution of the azimuthal velocity and metallicity after an evolution of 1, 3, 5 Gyr.

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thumbnail Fig. 5

Distribution of the azimuthal velocity and metallicity after an evolution of 6, 7, 8 Gyr.

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thumbnail Fig. 6

Left panels: normalised histograms of the original radii of the subset of particles found within 8 kpc  < R < 10 kpc that have 1.5 kpc  <  | z |  < 2 kpc at different evolutionary times. Right panels: normalised distributions of the azimuthal velocity at the same times.

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thumbnail Fig. 8

Normalised distributions of the differences Lfin − Lini between initial and final total angular momenta (after 5 Gyr) of the particles inside the solar annulus for the barred and unbarred disk (the curves represent an interpolation of the histogram).

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© ESO, 2012

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