Thick gas discs in faint dwarf galaxies
Sambit Roychowdhury, Jayaram N. Chengalur, Ayesha Begum, Igor D., Karachentsev

TL;DR
This study analyzes the intrinsic shape of gas disks in extremely faint dwarf irregular galaxies, revealing they are significantly thicker than those in larger galaxies, which impacts mass distribution and rotational studies.
Contribution
It introduces a method to determine the intrinsic axial ratio distribution of gas disks in faint dwarf irregular galaxies, showing these disks are thicker than previously assumed.
Findings
HI disks have a mean axial ratio of ~0.6.
Gas disks are thicker than stellar disks in large spirals.
Results align with higher velocity dispersion in dwarf galaxy gas disks.
Abstract
We determine the intrinsic axial ratio distribution of the 'gas' disks of extremely faint M_B > -14.5 dwarf irregular galaxies. We start with the measured (beam corrected) distribution of apparent axial ratios in the HI 21cm images of dwarf irregular galaxies observed as part of the Faint Irregular Galaxy GMRT Survey (FIGGS). Assuming that the disks can be approximated as oblate spheroids, the intrinsic axial ratio distribution can be obtained from the observed apparent axial ratio distribution. We use a couple of methods to do this, and our final results are based on using Lucy's deconvolution algorithm. This method is constrained to produce physically plausible distributions, and also has the added advantage of allowing for observational errors to be accounted for. While one might a priori expect that gas disks would be thin (because collisions between gas clouds would cause them to…
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