Connection between Non-Axisymmetric Structures and Neutral Gas Distribution in Disk Galaxies
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arXiv
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| Format: | Preprint |
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2024
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| author | Liang, Ze-Zhong Wang, Jing Gao, Hua Ho, Luis C. Athanassoula, E. |
| author_facet | Liang, Ze-Zhong Wang, Jing Gao, Hua Ho, Luis C. Athanassoula, E. |
| contents | Non-axisymmetric structures, such as bars and spiral arms, are known to concentrate molecular gas and star formation in galaxy centers, actively building up the pseudo-bulges. However, a direct link between the neutral (i.e., molecular and atomic) gas distribution and the exerted torque forces over a broader radial range of galactic disks still remains to be explored. In the present work, we investigate this link by carefully evaluating the torque force field using the $3.6\, \mathrm{μm}$ images for 17 The H I Nearby Galaxy Survey (THINGS) galaxies, and measuring neutral gas distribution on resolved atomic and molecular line maps. We find that galaxies with stronger torque forces show a more concentrated neutral gas distribution over the disk-scale, defined as half the isophotal radius at $25.5\, \mathrm{mag\, arcsec^{-2}}$. The correlation holds regardless of whether the neutral gas fraction, or the effective stellar mass surface density is controlled for. In addition, $\mathrm{kpc}$-scale neutral gas over-densities tend to be located close to the local maxima of torque forces. Most of these correlations involving the torque forces are comparatively stronger than those using the traditional Fourier amplitudes to quantify the non-axisymmetric structures. These results are consistent with the scenario that non-axisymmetric structures exert torque forces, and trigger dissipative processes to transport gas inward, not only to build the pseudo-bulges, but also fuel the inner disk growth. In this regard, non-axisymmetric structures inducing stronger torque forces appear to be more efficient in these processes. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_13595 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Connection between Non-Axisymmetric Structures and Neutral Gas Distribution in Disk Galaxies Liang, Ze-Zhong Wang, Jing Gao, Hua Ho, Luis C. Athanassoula, E. Astrophysics of Galaxies Non-axisymmetric structures, such as bars and spiral arms, are known to concentrate molecular gas and star formation in galaxy centers, actively building up the pseudo-bulges. However, a direct link between the neutral (i.e., molecular and atomic) gas distribution and the exerted torque forces over a broader radial range of galactic disks still remains to be explored. In the present work, we investigate this link by carefully evaluating the torque force field using the $3.6\, \mathrm{μm}$ images for 17 The H I Nearby Galaxy Survey (THINGS) galaxies, and measuring neutral gas distribution on resolved atomic and molecular line maps. We find that galaxies with stronger torque forces show a more concentrated neutral gas distribution over the disk-scale, defined as half the isophotal radius at $25.5\, \mathrm{mag\, arcsec^{-2}}$. The correlation holds regardless of whether the neutral gas fraction, or the effective stellar mass surface density is controlled for. In addition, $\mathrm{kpc}$-scale neutral gas over-densities tend to be located close to the local maxima of torque forces. Most of these correlations involving the torque forces are comparatively stronger than those using the traditional Fourier amplitudes to quantify the non-axisymmetric structures. These results are consistent with the scenario that non-axisymmetric structures exert torque forces, and trigger dissipative processes to transport gas inward, not only to build the pseudo-bulges, but also fuel the inner disk growth. In this regard, non-axisymmetric structures inducing stronger torque forces appear to be more efficient in these processes. |
| title | Connection between Non-Axisymmetric Structures and Neutral Gas Distribution in Disk Galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2410.13595 |