The filamentary structures in the CO emission toward the Milky Way disk

J. D. Soler; H. Beuther; J. Syed; Y. Wang; Th Henning; S. C. O. Glover; R. S. Klessen; M. C. Sormani; M. Heyer; R. J. Smith; J. S. Urquhart; J. Yang; Y. Su; X. Zhou

doi:10.1051/0004-6361/202141327

The filamentary structures in the CO emission toward the Milky Way disk

J. D. Soler, H. Beuther, J. Syed, Y. Wang, Th Henning, S. C. O. Glover, R. S. Klessen, M. C. Sormani, M. Heyer, R. J. Smith, J. S. Urquhart, J. Yang, Y. Su, X. Zhou

School of Physics and Astronomy

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Abstract

We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting survey in the range 25.°8 < l < 49.°7, |b| ≤ 1.°25, and −100 < v_LSR < 135 km s⁻¹. We found that most of the filamentary structures in the ¹²CO and ¹³CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the ¹²CO and ¹³CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.

Original language	English
Article number	L4
Number of pages	8
Journal	Astronomy & Astrophysics
Volume	651
Early online date	6 Jul 2021
DOIs	https://doi.org/10.1051/0004-6361/202141327
Publication status	Published - Jul 2021

Keywords

ISM: structure
ISM: clouds
Galaxies: structure
ISM: molecules
Molecular data
ISM: kinematics and dynamics

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10.1051/0004-6361/202141327Licence: CC BY

Soler--2021-Filamentary-structures-in-the-CO-A&A-651-L4-CCBY
Copyright © J. D. Soler et al. 2021. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 986 KBLicence: CC BY

http://arxiv.org/abs/2106.13206Licence: CC BY-NC-SA

The filamentary structures in the CO emission toward the Milky Way disk (dataset)
Smith, R. J. (Creator), Centre de Donnees Strasbourg (CDS), 2021
https://simbad.u-strasbg.fr/simbad/sim-ref?querymethod=bib&simbo=on&submit=submit+bibcode&bibcode=2021A%26A...651L...4S
Dataset

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@article{35367eec8470403880a2c008137d036c,

title = "The filamentary structures in the CO emission toward the Milky Way disk",

abstract = "We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting survey in the range 25.°8 < l < 49.°7, |b| ≤ 1.°25, and −100 < vLSR < 135 km s−1. We found that most of the filamentary structures in the 12CO and 13CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the 12CO and 13CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.",

keywords = "ISM: structure, ISM: clouds, Galaxies: structure, ISM: molecules, Molecular data, ISM: kinematics and dynamics",

author = "Soler, {J. D.} and H. Beuther and J. Syed and Y. Wang and Th Henning and Glover, {S. C. O.} and Klessen, {R. S.} and Sormani, {M. C.} and M. Heyer and Smith, {R. J.} and Urquhart, {J. S.} and J. Yang and Y. Su and X. Zhou",

note = "Funding: JDS and HB acknowledge funding from the European Research Council under the Horizon 2020 Framework Program via the ERC Consolidator Grant CSF-648505. RJS is funded by an STFC ERF (grant ST/N00485X/1). ",

year = "2021",

month = jul,

doi = "10.1051/0004-6361/202141327",

language = "English",

volume = "651",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

TY - JOUR

T1 - The filamentary structures in the CO emission toward the Milky Way disk

AU - Soler, J. D.

AU - Beuther, H.

AU - Syed, J.

AU - Wang, Y.

AU - Henning, Th

AU - Glover, S. C. O.

AU - Klessen, R. S.

AU - Sormani, M. C.

AU - Heyer, M.

AU - Smith, R. J.

AU - Urquhart, J. S.

AU - Yang, J.

AU - Su, Y.

AU - Zhou, X.

N1 - Funding: JDS and HB acknowledge funding from the European Research Council under the Horizon 2020 Framework Program via the ERC Consolidator Grant CSF-648505. RJS is funded by an STFC ERF (grant ST/N00485X/1).

PY - 2021/7

Y1 - 2021/7

N2 - We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting survey in the range 25.°8 < l < 49.°7, |b| ≤ 1.°25, and −100 < vLSR < 135 km s−1. We found that most of the filamentary structures in the 12CO and 13CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the 12CO and 13CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.

AB - We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting survey in the range 25.°8 < l < 49.°7, |b| ≤ 1.°25, and −100 < vLSR < 135 km s−1. We found that most of the filamentary structures in the 12CO and 13CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the 12CO and 13CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.

KW - ISM: structure

KW - ISM: clouds

KW - Galaxies: structure

KW - ISM: molecules

KW - Molecular data

KW - ISM: kinematics and dynamics

U2 - 10.1051/0004-6361/202141327

DO - 10.1051/0004-6361/202141327

M3 - Letter

SN - 0004-6361

VL - 651

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - L4

ER -

The filamentary structures in the CO emission toward the Milky Way disk

Abstract

Keywords

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The filamentary structures in the CO emission toward the Milky Way disk (dataset)

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