Gas Dynamics in the Milky Way: Second Pattern Speed and Large-Scale Morphology

Details Gas Dynamics in the Milky Way: Second Pattern Speed and Large-Scale Morphology Gas Dynamics in the Milky Way: Second Pattern Speed and Large-Scale Morphology

2002-12-23

arxiv.org/abs/astro-ph/0212516v1

Mon.Not.Roy.Astron.Soc. 340 (2003) 949

Astronomy and Astrophysics

Astrophysics

Paper accepted for publication in MNRAS. The paper contains many figures. These are not included in the version available here

Scientific paper

10.1046/j.1365-8711.2003.06358.x

We present new gas flow models for the Milky Way inside the solar circle. To this end we use SPH simulations in gravitational potentials determined from the NIR luminosity distribution (including spiral arms) which are based on the COBE/DIRBE maps. Gas flows in models which include massive spiral arms clearly match the observed 12CO lvplot better than if the potential does not include spiral structure. Besides single pattern speed models we investigate models with separate pattern speeds for the bar and spiral arms. The most important difference is that in the latter case the gas spiral arms go through the bar corotation region, keeping the gas aligned with the arms there. In the (l,v) plot this results in characteristic regions which appear to be nearly void of gas.In single pattern speed models these regions are filled with gas because the spiral arms dissolve in the bar corotation region. Comparing with the 12CO data we find evidence for separate pattern speeds in the Milky Way.From a series of models the preferred range for the bar pattern speed is Om_p=60\pm5 /Gyr, corresponding to corotation at 3.4\pm0.3kpc. The spiral pattern speed is less well constrained, but our preferred value is Om_sp\approx 20 /Gyr. A further series of gas models is computed for different bar angles, using separately determined luminosity models and gravitational potentials in each case. We find acceptable gas models for 20<=\phibar<=25. The model with (\phibar=20, Om_p=60 /Gyr, Om_sp=20 /Gyr) gives an excellent fit to the spiral arm ridges in the observed (l,v) plot.

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