The Gas Content in Galactic Disks: Correlation with Kinematics

Abstract

We consider the relationship between the total HI mass in late-type galaxies and the kinematic properties of their disks. The mass $M_{H}I$ for galaxies with a wide variety of properties, from dwarf dIrr galaxies with active star formation to giant low-brightness galaxies, is shown to correlate with the product $V_c{R}_0$ ($V_c$ is the rotational velocity, and $R_0$ is the radial photometric disks scale length), which characterizes the specific angular momentum of the disk. This relationship, along with the anticorrelation between the relative mass of HI in a galaxy and $V_c$, can be explained in terms of the previously made assumption that the gas density in the disks of most galaxies is maintained at a level close to the threshold (marginal) stability of a gaseous layer to local gravitational perturbations. In this case, the regulation mechanism of the star formation rate associated with the growth of local gravitational instability in the gaseous layer must play a crucial role in the evolution of the gas content in the galactic disk.

revised version to appear in Astronomy Letters, 8 pages, 5 EPS figures

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• Preheating by Previrialization and its Impact on Galaxy Formation
• Kinematic classification of non-interacting spiral galaxies
• Star Formation on Galactic Scales: Empirical Laws
• HI content in the galactic discs: the role of gravitational instability
• The Star-Formation Efficiency and Density of the Disks of Spiral Galaxies
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