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The Stellar and Gas Kinematics of the LITTLE THINGS Dwarf Irregular Galaxy NGC 1569 | | Megan Johnson
; Deidre A. Hunter
; Se-Heon Oh
; Hong-Xin Zhang
; Bruce Elmegreen
; Elias Brinks
; Erik Tollerud
; Kimberly Herrmann
; | | Date: |
12 Sep 2012 | | Abstract: | In order to understand the formation and evolution of dIm galaxies, one needs
to understand their three-dimensional structure. We present measurements of the
stellar velocity dispersion in NGC 1569, a nearby post-starburst dIm galaxy.
The stellar vertical velocity dispersion, $sigma_{
m z}$, coupled with the
maximum rotational velocity derived from ion{H}{1} observations, $V_{
m
max}$, gives a measure of how kinematically hot the galaxy is, and, therefore,
indicates its structure. We conclude that the stars in NGC 1569 are in a thick
disk with a $V_{
m max} / sigma_{
m z}$ = 2.4 $pm$ 0.7. In addition to the
structure, we analyze the ionized gas kinematics from ion{O}{3} observations
along the morphological major axis. These data show evidence for outflow from
the inner starburst region and a potential expanding shell near supermassive
star cluster (SSC) A. When compared to the stellar kinematics, the velocity
dispersion of the stars increase in the region of SSC A supporting the
hypothesis of an expanding shell. The stellar kinematics closely follow the
motion of the gas. Analysis of high resolution ion{H}{1} data clearly reveals
the presence of an ion{H}{1} cloud that appears to be impacting the eastern
edge of NGC 1569. Also, an ultra-dense ion{H}{1} cloud can be seen extending
to the west of the impacting ion{H}{1} cloud. This dense cloud is likely the
remains of a dense ion{H}{1} bridge that extended through what is now the
central starburst area. The impacting ion{H}{1} cloud was the catalyst for the
starburst, thus turning the dense gas into stars over a short timescale, $sim$
1 Gyr. We performed a careful study of the spectral energy distribution using
infrared, optical, and ultraviolet photometry producing a state-of-the-art mass
model for the stellar disk. This mass modeling shows that stars dominate the
gravitational potential in the inner 1 kpc. | | Source: | arXiv, 1209.2453 | | Services: | Forum | Review | PDF | Favorites | |
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