The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way

J. D. Soler; H. Beuther; J. Syed; Y. Wang; L. D. Anderson; S. C.O. Glover; P. Hennebelle; M. Heyer; Th Henning; A. F. Izquierdo; R. S. Klessen; H. Linz; N. M. McClure-Griffiths; J. Ott; S. E. Ragan; M. Rugel; N. Schneider; R. J. Smith; M. C. Sormani; J. M. Stil; R. Treß; J. S. Urquhart

doi:10.1051/0004-6361/202038882

The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way

J. D. Soler^*, H. Beuther, J. Syed, Y. Wang, L. D. Anderson, S. C.O. Glover, P. Hennebelle, M. Heyer, Th Henning, A. F. Izquierdo, R. S. Klessen, H. Linz, N. M. McClure-Griffiths, J. Ott, S. E. Ragan, M. Rugel, N. Schneider, R. J. Smith, M. C. Sormani, J. M. StilR. Treß, J. S. Urquhart

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

33 Citations (Scopus)

Abstract

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′′ and 1.5-km s-1 resolution position-position-velocity cube, resulting from the combination of the single-dish and interferometric observations in The HI/OH/recombination-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 l ≈ 28° and vLSR ≈ 100 km s-1, (ii) toward l ≈ 45° and vLSR ≈ 50 km s-1, (iii) around the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal velocities. A comparison with numerical simulations indicates that the prevalence of horizontal filamentary structures is most likely the result of 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 behavior of the interstellar medium, from the effect of large-scale Galactic dynamics to the Galactic fountains driven by SNe.

Original language	English
Article number	A163
Journal	Astronomy and Astrophysics
Volume	642
DOIs	https://doi.org/10.1051/0004-6361/202038882
Publication status	Published - 1 Oct 2020

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Soler, J. D., Beuther, H., Syed, J., Wang, Y., Anderson, L. D., Glover, S. C. O., Hennebelle, P., Heyer, M., Henning, T., Izquierdo, A. F., Klessen, R. S., Linz, H., McClure-Griffiths, N. M., Ott, J., Ragan, S. E., Rugel, M., Schneider, N., Smith, R. J., Sormani, M. C., ... Urquhart, J. S. (2020). The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way. Astronomy and Astrophysics, 642, Article A163. https://doi.org/10.1051/0004-6361/202038882

@article{c52396efab2142b4802e5799c353806f,

title = "The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way",

abstract = "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′′ and 1.5-km s-1 resolution position-position-velocity cube, resulting from the combination of the single-dish and interferometric observations in The HI/OH/recombination-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 l ≈ 28° and vLSR ≈ 100 km s-1, (ii) toward l ≈ 45° and vLSR ≈ 50 km s-1, (iii) around the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal velocities. A comparison with numerical simulations indicates that the prevalence of horizontal filamentary structures is most likely the result of 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 behavior of the interstellar medium, from the effect of large-scale Galactic dynamics to the Galactic fountains driven by SNe.",

keywords = "Galaxy: structure, ISM: atoms, ISM: clouds, ISM: kinematics and dynamics, ISM: structure, Radio lines: ISM",

author = "Soler, {J. D.} and H. Beuther and J. Syed and Y. Wang and Anderson, {L. D.} and Glover, {S. C.O.} and P. Hennebelle and M. Heyer and Th Henning and Izquierdo, {A. F.} and Klessen, {R. S.} and H. Linz and McClure-Griffiths, {N. M.} and J. Ott and Ragan, {S. E.} and M. Rugel and N. Schneider and Smith, {R. J.} and Sormani, {M. C.} and Stil, {J. M.} and R. Tre{\ss} and Urquhart, {J. S.}",

note = "Publisher Copyright: {\textcopyright} 2020 J. D. Soler et al.",

year = "2020",

month = oct,

day = "1",

doi = "10.1051/0004-6361/202038882",

language = "English",

volume = "642",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Soler, JD, Beuther, H, Syed, J, Wang, Y, Anderson, LD, Glover, SCO, Hennebelle, P, Heyer, M, Henning, T, Izquierdo, AF, Klessen, RS, Linz, H, McClure-Griffiths, NM, Ott, J, Ragan, SE, Rugel, M, Schneider, N, Smith, RJ, Sormani, MC, Stil, JM, Treß, R & Urquhart, JS 2020, 'The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way', Astronomy and Astrophysics, vol. 642, A163. https://doi.org/10.1051/0004-6361/202038882

TY - JOUR

T1 - The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way

AU - Soler, J. D.

AU - Beuther, H.

AU - Syed, J.

AU - Wang, Y.

AU - Anderson, L. D.

AU - Glover, S. C.O.

AU - Hennebelle, P.

AU - Heyer, M.

AU - Henning, Th

AU - Izquierdo, A. F.

AU - Klessen, R. S.

AU - Linz, H.

AU - McClure-Griffiths, N. M.

AU - Ott, J.

AU - Ragan, S. E.

AU - Rugel, M.

AU - Schneider, N.

AU - Smith, R. J.

AU - Sormani, M. C.

AU - Stil, J. M.

AU - Treß, R.

AU - Urquhart, J. S.

PY - 2020/10/1

Y1 - 2020/10/1

N2 - 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′′ and 1.5-km s-1 resolution position-position-velocity cube, resulting from the combination of the single-dish and interferometric observations in The HI/OH/recombination-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 l ≈ 28° and vLSR ≈ 100 km s-1, (ii) toward l ≈ 45° and vLSR ≈ 50 km s-1, (iii) around the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal velocities. A comparison with numerical simulations indicates that the prevalence of horizontal filamentary structures is most likely the result of 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 behavior of the interstellar medium, from the effect of large-scale Galactic dynamics to the Galactic fountains driven by SNe.

AB - 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′′ and 1.5-km s-1 resolution position-position-velocity cube, resulting from the combination of the single-dish and interferometric observations in The HI/OH/recombination-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 l ≈ 28° and vLSR ≈ 100 km s-1, (ii) toward l ≈ 45° and vLSR ≈ 50 km s-1, (iii) around the Riegel-Crutcher cloud, and (iv) toward the positive and negative terminal velocities. A comparison with numerical simulations indicates that the prevalence of horizontal filamentary structures is most likely the result of 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 behavior of the interstellar medium, from the effect of large-scale Galactic dynamics to the Galactic fountains driven by SNe.

KW - Galaxy: structure

KW - ISM: atoms

KW - ISM: clouds

KW - ISM: kinematics and dynamics

KW - ISM: structure

KW - Radio lines: ISM

UR - http://www.scopus.com/inward/record.url?scp=85094911574&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202038882

DO - 10.1051/0004-6361/202038882

M3 - Article

SN - 0004-6361

VL - 642

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A163

ER -

The history of dynamics and stellar feedback revealed by the H i filamentary structure in the disk of the Milky Way

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