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Large-scale velocity-coherent filaments in the SEDIGISM survey: Association with spiral arms and the fraction of dense gas

Ge, Y, Wang, K., Duarte-Cabral, A., Pettitt, A R, Dobbs, C. L., Sanchez-Monge, A., Neralwar, K.R., Urquhart, J.S., Colombo, D., Duran-Camacho, E, and others. (2023) Large-scale velocity-coherent filaments in the SEDIGISM survey: Association with spiral arms and the fraction of dense gas. Astronomy & Astrophysics, 675 . Article Number A119. ISSN 0004-6361. E-ISSN 1432-0746. (doi:10.1051/0004-6361/202245784) (KAR id:101363)

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Context. Filamentary structures in the interstellar medium are closely related to star formation. Dense gas mass fraction (DGMF) or clump formation efficiency in large-scale filaments possibly determine their hosting star formation activities.

Aims. We aim to automatically identify large-scale filaments, characterize them, investigate their association with Galactic structures, and study their DGMFs.

Methods. We use a modified minimum spanning tree (MST) algorithm to chain parsec-scale 13CO clumps previously extracted from the SEDIGISM (Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium) survey. The MST connects nodes in a graph such that the sum of edge lengths is minimum. Modified MST also ensures velocity coherence between nodes, so the identified filaments are coherent in position-position-velocity (PPV) space.

Results. We generate a catalog of 88 large-scale (> 10 pc) filaments in the inner Galactic plane (with −60◦ < l < 18◦ and |b| < 0.5◦). These SEDIGISM filaments are larger and less dense than MST filaments previously identified from the BGPS and ATLASGAL surveys. We find that eight of the filaments run along spiral arms and can be regarded as “bones” of the Milky Way. We also find three bones associated with the Local Spur in PPV space. By compiling 168 large-scale filaments with available DGMF across the Galaxy, an order of magnitude more than previously investigated, we find that DGMFs do not correlate with Galactic location, but bones have higher DGMFs than other filaments.

Item Type: Article
DOI/Identification number: 10.1051/0004-6361/202245784
Uncontrolled keywords: stars: formation; catalogs; ISM: clouds; ISM: molecules; Galaxy: structure; ISM: structure
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Funders: University of Kent (
Depositing User: James Urquhart
Date Deposited: 22 May 2023 08:53 UTC
Last Modified: 09 Jan 2024 17:35 UTC
Resource URI: (The current URI for this page, for reference purposes)

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