Below you can find movies related to the following papers:
(CLICK HERE TO DOWNLOAD ALL VIDEOS IN A SINGLE ZIP FILE, 465MB)
HI, H2, and CO three colour composite
Three-colour composite showing the spatial relation of three chemical components: HI, H2 and CO. The large panel shows the CMZ, while the smaller rectangular panel at the bottom shows the larger-scale flow.
Evolution of the star formation rate
Star formation rate as a function of time in our simulation. The thick blue, thin pink and thin yellow lines are the SFR in the three different spatial regions (CMZ, DLR, disc) in which we have subdivided our simulation (see Figure 1 in Paper II). The thin black line is the total SFR (CMZ+DLR+disc). The three panels on the top show total gas surface density (total, HI, H2) that allow us to correlate the SFR with the instantaneous CMZ gas morphology. The three panels at the bottom show the SFR mediated over the last 0.5Myr, very young (age <1Myr) and less young (1Myr < age < 0 Myr) stars formed in the simulations.
Evolution of surface density - large scales
This video shows the evolution of the surface density in various tracers on the scales of the Galactic bar. From top-left to bottom-right: Total surface density (all componenents), HI, H2, star formation rate (SFR), CO, H+
Evolution of surface density - CMZ
This video shows the evolution of the surface density in various tracers in the CMZ. From top-left to bottom-right: Total surface density (all componenents), HI, H2, star formation rate (SFR), CO, H+
Inflows & outflows
In this movie we analyse radial inflows and outflows (see Fig. 15 in Paper II). On the left, we show instantaneous radial mass flows. Red indicates spherically inward motion (inflow) while blue indicates spherically outwards motion (outflow). Most of the inward-moving material (red) is concentrated in the two ``dust-lane features'' which mediate the bar-driven accretion. Embedded in the dust-lane features, some blue clouds can often be spotted. These represent ``overshooting'' material which is moving outwards against the inward flow of the dust lane, which causes them to decelerate and eventually join the flow of the dust lanes. On the right, we show instantaneous mass fluxes through two spheres of radius R1=50pc and R2 = 250pc in a Mollweide projection centred on the Galactic centre. Net flux indicates the instantaneous mass flow rate integrated over the surface of the sphere.
Evolution of column densities on large scales - total
In this movie we show the face-on and edge-on time evolution of total (all gas components) column density on large-scales (i.e., the scale of the Galactic bar).
Evolution of column densities in the CMZ - CO
In this movie we show the face-on and edge-on time evolution of total (all gas components) column density in the simulated central molecular zone.
Evolution of star formation rate density
In this movie we show the face-on and edge-on time evolution of the star formation rate density on large-scales (i.e., the scale of the Galactic bar).
Evolution of star formation rate density in the CMZ
In this movie we show the face-on and edge-on time evolution of the star formation rate density in the simulated central molecular zone.
Evolution of column densities on large scales - HI
In this movie we show the face-on and edge-on time evolution of HI column density on large-scales (i.e., the scale of the Galactic bar).
Evolution of column densities in the CMZ - HI
In this movie we show the face-on and edge-on time evolution of HI column density in the simulated central molecular zone.
Evolution of column densities on large scales - H2
In this movie we show the face-on and edge-on time evolution of H2 column density on large-scales (i.e., the scale of the Galactic bar).
Evolution of column densities in the CMZ - H2
In this movie we show the face-on and edge-on time evolution of H2 column density in the simulated central molecular zone.
Evolution of column densities on large scales - CO
In this movie we show the face-on and edge-on time evolution of CO column density on large-scales (i.e., the scale of the Galactic bar).
Evolution of column densities in the CMZ - CO
In this movie we show the face-on and edge-on time evolution of CO column density in the simulated central molecular zone.
Evolution of column densities on large scales - H+
In this movie we show the face-on and edge-on time evolution of H+ column density on large-scales (i.e., the scale of the Galactic bar).
Evolution of column densities in the CMZ - H+
In this movie we show the face-on and edge-on time evolution of H+ column density in the simulated central molecular zone.
Evolution of gas temperature on large scales
In this movie we show the face-on and edge-on time evolution of the integrated mass-weighted gas temperature on large-scales (i.e., the scale of the Galactic bar).
Evolution of gas temperature in the CMZ
In this movie we show the face-on and edge-on time evolution of the integrated mass-weighted gas temperature in the simulated central molecular zone.