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arXiv · 1309.6324

A high-dispersion molecular gas component in nearby galaxies

Anahi Caldu-Primo·Andreas Schruba·Fabian Walter·Adam Leroy·Karin Sandstrom·W. J. G. de Blok·Roger Ianjamasimanana·K. M. Mogotsi
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Abstract

We present a comprehensive study of the velocity dispersion of the atomic (HI) and molecular (H2) gas components in the disks (R < R25) of a sample of 12 nearby spiral galaxies with moderate inclinations. Our analysis is based on sensitive high resolution data from the THINGS (atomic gas) and HERACLES (molecular gas) surveys. To obtain reliable measurements of the velocity dispersion, we stack regions several kilo-parsecs in size, after accounting for intrinsic velocity shifts due to galactic rotation and large-scale motions. We stack using various parameters: the galacto-centric distance, star formation rate surface density, HI surface density, H2 surface density, and total gas surface density. We fit single Gaussian components to the stacked spectra and measure median velocity dispersions for HI of 11.9 +/- 3.1 km/s and for H2 of 12.0 +/- 3.9 km/s. The CO velocity dispersions are thus, surprisingly, very similar to the corresponding ones of HI, with an average ratio of sigma(HI)/sigma(CO) = 1.0 +/- 0.2 irrespective of the stacking parameter. The measured CO velocity dispersions are significantly higher (factor 2) than the traditional picture of a cold molecular gas disk associated with star formation. The high dispersion implies an additional thick molecular gas disk (possibly as thick as the HI disk). Our finding is in agreement with recent sensitive measurements in individual edge-on and face-on galaxies and points towards the general existence of a thick disk of molecular gas, in addition to the well-known thin disk in nearby spiral galaxies.

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Anahi Caldu-Primo, Andreas Schruba, Fabian Walter, Adam Leroy, Karin Sandstrom, W. J. G. de Blok, Roger Ianjamasimanana, K. M. Mogotsi. 2013-09-24. A high-dispersion molecular gas component in nearby galaxies. https://doi.org/10.1088/0004-6256/146/6/150

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