The history of dynamics and stellar feedback revealed by the HI filamentary structure in the disk of the Milky Way. (arXiv:2007.07285v1 [astro-ph.GA])

The history of dynamics and stellar feedback revealed by the HI filamentary structure in the disk of the Milky Way. (arXiv:2007.07285v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Soler_J/0/1/0/all/0/1">J.D. Soler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beuther_H/0/1/0/all/0/1">H. Beuther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Syed_J/0/1/0/all/0/1">J. Syed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Y. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_L/0/1/0/all/0/1">L.D. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glover_S/0/1/0/all/0/1">S.C.O. Glover</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hennebelle_P/0/1/0/all/0/1">P. Hennebelle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heyer_M/0/1/0/all/0/1">M. Heyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Th. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Izquierdo_A/0/1/0/all/0/1">A.F. Izquierdo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">R.S. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Linz_H/0/1/0/all/0/1">H. Linz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McClure_Griffiths_N/0/1/0/all/0/1">N.M. McClure-Griffiths</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ott_J/0/1/0/all/0/1">J. Ott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ragan_S/0/1/0/all/0/1">S.E. Ragan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rugel_M/0/1/0/all/0/1">M. Rugel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_N/0/1/0/all/0/1">N. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">R.J. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sormani_M/0/1/0/all/0/1">M.C. Sormani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stil_J/0/1/0/all/0/1">J.M. Stil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urquhart_J/0/1/0/all/0/1">J.S. Urquhart</a>

We present a study of the filamentary structure in the emission from the
neutral atomic hydrogen (HI) at 21 cm across velocity channels in the
40″-resolution observations in The HI/OH/Recombination (THOR) line survey of
the inner Milky Way. Using the Hessian matrix method in combination with tools
from circular statistics, we find that the majority of the filamentary
structures in the HI emission are aligned with the Galactic plane. Part of this
trend can be assigned to long filamentary structures that are coherent across
several velocity channels. However, we also find ranges of Galactic longitude
and radial velocity where the HI filamentary structures are preferentially
oriented perpendicular to the Galactic plane. These are located (i) around the
tangent point of the Scutum spiral arm and the terminal velocities of the
Molecular Ring, around $lapprox 28${deg} and $v_{rm LSR}approx 100$ km/s,
(ii) toward $lapprox 45${deg} and $v_{rm LSR}approx 50$ km/s, (iii) around
the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal
velocities. Comparison with numerical simulations indicates that the prevalence
of horizontal filamentary structures is most likely the result of the
large-scale Galactic dynamics and that vertical structures identified in (i)
and (ii) may arise from the combined effect of supernova (SN) feedback and
strong magnetic fields. The vertical filamentary structures in (iv) can be
related to the presence of clouds from extra-planar HI gas falling back into
the Galactic plane after being expelled by SNe. Our results indicate that a
systematic characterization of the emission morphology toward the Galactic
plane provides an unexplored link between the observations and the dynamical
behaviour of the interstellar medium, from the effect of large-scale Galactic
dynamics to the Galactic fountains driven by SNe.

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