Issue |
A&A
Volume 664, August 2022
|
|
---|---|---|
Article Number | A84 | |
Number of page(s) | 27 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202142513 | |
Published online | 10 August 2022 |
The SEDIGISM survey: Molecular cloud morphology
II. Integrated source properties
1
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69,
53121
Bonn, Germany
e-mail: kneralwar@mpifr-bonn.mpg.de
2
School of Physics & Astronomy, Cardiff University,
Queen’s Building, The Parade,
Cardiff
CF24 3AA, UK
3
Centre for Astrophysics and Planetary Science, University of Kent,
Canterbury
CT2 7NH,
UK
4
Laboratoire d’Astrophysique (AIM), CEA, CNRS, Université Paris-Saclay, Université Paris Diderot,
Sorbonne Paris Cité,
91191
Gif-sur-Yvette, France
5
Space Science Institute,
4765 Walnut St Suite B,
Boulder,
CO 80301, USA
6
School of Science and Technology, University of New England,
Armidale NSW
2351, Australia
7
I. Physikalisches Institut, Universität zu Köln,
Zülpicher Strasse 77,
50937
Cologne, Germany
8
Astrophysics Research Institute, Liverpool John Moores University, IC2,
Liverpool Science Park, 146 Brownlow Hill,
Liverpool,
L3 5RF, UK
9
Laboratoire d’astrophysique de Bordeaux, CNRS, Univ. Bordeaux,
B18N, allée Geoffroy Saint-Hilaire,
33615
Pessac, France
10
School of Physics and Astronomy, University of Exeter,
Stocker Road,
Exeter
EX4 4QL,
UK
11
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg, Germany
12
Leibniz-Institut für Astrophysik Potsdam (AIP),
An der Sternwarte 16,
14482
Potsdam, Germany
13
INAF – Osservatorio Astronomico di Cagliari,
Via della Scienza 5,
09047
Selargius (CA), Italy
14
The American University of Paris,
2bis, Passage Landrieu
75007
Paris, France
Received:
22
October
2021
Accepted:
4
May
2022
The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial and spectral) resolution 13CO (2−1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the inner Galaxy at an unprecedented level of detail and characterise it into molecular clouds (MCs). In a previous paper, we classified the SEDIGISM clouds into four morphologies. However, how the properties of the clouds vary for these four morphologies is not well understood. Here, we use the morphological classification of SEDIGISM clouds to find connections between the cloud morphologies, their integrated properties, and their location on scaling relation diagrams. We observe that ring-like clouds show the most peculiar properties, having, on average, higher masses, sizes, aspect ratios, and velocity dispersions, compared to other morphologies. We speculate that this is related to the physical mechanisms that regulate their formation and evolution; for example, turbulence from stellar feedback can often result in the creation of bubble-like structures. We also see a trend of morphology with the virial parameter, whereby ring-like, elongated, clumpy, and concentrated clouds have virial parameters in decreasing order. Our findings provide a foundation for a better understanding of MC behaviour, based on their measurable properties.
Key words: ISM: clouds / local insterstellar matter / ISM: bubbles / submillimeter: ISM
© K. R. Neralwar et al. 2022
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.
This article is published in open access under the Subscribe-to-Open model.
Open Access funding provided by Max Planck Society.
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