The SEDIGISM survey: The influence of spiral arms on the molecular gas distribution of the inner Milky Way

被引：16

作者：

Colombo, D. ^{[1
]}

Duarte-Cabral, A. ^{[2
]}

Pettitt, A. R. ^{[3
]}

Urquhart, J. S. ^{[4
]}

Wyrowski, F. ^{[1
]}

Csengeri, T. ^{[5
]}

Neralwar, K. R. ^{[1
]}

Schuller, F. ^{[1
,6
]}

Menten, K. M. ^{[1
]}

Anderson, L. ^{[7
,8
,9
]}

Barnes, P. ^{[10
,11
,12
]}

Beuther, H. ^{[13
]}

Bronfman, L. ^{[14
]}

Eden, D. ^{[15
]}

Ginsburg, A. ^{[16
]}

Henning, T. ^{[13
]}

Konig, C. ^{[1
]}

Lee, M-Y ^{[17
]}

Mattern, M. ^{[18
]}

Medina, S. ^{[1
]}

Ragan, S. E. ^{[2
]}

Rigby, A. J. ^{[2
]}

Sanchez-Monge, A. ^{[19
]}

Traficante, A. ^{[20
]}

Yang, A. Y. ^{[1
]}

Wienen, M. ^{[1
]}

机构：

[1] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[2] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, Wales

[3] Hokkaido Univ, Fac Sci, Dept Phys, Sapporo, Hokkaido 0600810, Japan

[4] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England

[5] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France

[6] Leibniz Inst Astrophys Potsdam AlP, Sternwarte 16, D-14482 Potsdam, Germany

[7] West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA

[8] Green Bank Observ, POB 2, Green Bank, WV 24944 USA

[9] West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA

[10] Univ Florida, Dept Astron, 211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA

[11] Space Sci Inst, 4765 Walnut St Suite B, Boulder, CO 80301 USA

[12] Univ New England, Sch Sci & Technol, Armidale, NSW 2351, Australia

[13] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[14] Univ Chile, Astron Dept, Casilla 36-D, Santiago, Chile

[15] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[16] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA

[17] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea

[18] Commissariat Energie Atom & Energies Alternat, F-91191 Gif Sur Yvette, Saclay, France

[19] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

[20] IAPS INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 658卷

基金：

欧洲研究理事会;

关键词：

ISM: clouds; Galaxy: structure; stars: formation; galaxies: ISM; galaxies: star formation; galaxies: spiral; STAR-FORMATION EFFICIENCY; RECONSTRUCTING CO MAPS; NEARBY GALAXIES; PHYSICAL-PROPERTIES; INTERSTELLAR-MEDIUM; GALACTIC DISTRIBUTION; STELLAR STRUCTURE; CLOUD COLLISIONS; COMPLETE SAMPLE; GRAND DESIGN;

D O I：

10.1051/0004-6361/202141287

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The morphology of the Milky Way is still a matter of debate. In order to shed light on uncertainties surrounding the structure of the Galaxy, in this paper, we study the imprint of spiral arms on the distribution and properties of its molecular gas. To do so, we take full advantage of the SEDIGISM (Structure, Excitation, and Dynamics of the Inner Galactic Interstellar Medium) survey that observed a large area of the inner Galaxy in the (CO)-C-13 (2-1) line at an angular resolution of 28 ''. We analyse the influences of the spiral arms by considering the features of the molecular gas emission as a whole across the longitude-velocity map built from the full survey. Additionally, we examine the properties of the molecular clouds in the spiral arms compared to the properties of their counterparts in the inter-arm regions. Through flux and luminosity probability distribution functions, we find that the molecular gas emission associated with the spiral arms does not differ significantly from the emission between the arms. On average, spiral arms show masses per unit length of similar to 10(5)-10(6) M-circle dot kpc(-1). This is similar to values inferred from data sets in which emission distributions were segmented into molecular clouds. By examining the cloud distribution across the Galactic plane, we infer that the molecular mass in the spiral arms is a factor of 1.5 higher than that of the inter-arm medium, similar to what is found for other spiral galaxies in the local Universe. We observe that only the distributions of cloud mass surface densities and aspect ratio in the spiral arms show significant differences compared to those of the inter-arm medium; other observed differences appear instead to be driven by a distance bias. By comparing our results with simulations and observations of nearby galaxies, we conclude that the measured quantities would classify the Milky Way as a flocculent spiral galaxy, rather than as a grand-design one.

引用

页数：38

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