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Characterising the high-mass star forming filament G351.776–0.527 with Herschel* and APEX** dust continuum and gas observations

Leurini, S., Schisano, E., Pillai, T., Giannetti, A., Urquhart, J.S., Csengeri, T., Casu, S., Cunningham, M., Elia, D., Jones, P. A., and others. (2019) Characterising the high-mass star forming filament G351.776–0.527 with Herschel* and APEX** dust continuum and gas observations. Astronomy & Astrophysics, 621 . ISSN 0004-6361. E-ISSN 1432-0746. (doi:10.1051/0004-6361/201833612)

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https://doi.org/10.1051/0004-6361/201833612

Abstract

G351.776-0.527 is among the most massive, closest, and youngest filaments in the inner Galactic plane and therefore it is an ideal laboratory to study the kinematics of dense gas and mass replenishment on a large scale. In this paper, we present far-infrared (FIR) and submillimetre wavelength continuum observations combined with spectroscopic C18O(2–1) data of the entire region to study its temperature, mass distribution, and kinematics. The structure is composed of a main elongated region with an aspect ratio of ~ 23, which is associated with a network of filamentary structures. The main filament has a remarkably constant width of 0.2 pc. The total mass of the network (including the main filament) is > 2600M, while we estimate a mass of ~ 2000M for the main structure. Therefore, the network harbours a large reservoir of gas and dust that could still be accreted onto the main structure. From the analysis of the gas kinematics, we detect two velocity components in the northern part of the main filament. The data also reveal velocity oscillations in C18O along the spine in the main filament and in at least one of the branches. Considering the region as a single structure, we find that it is globally close to virial equilibrium indicating that the entire structure is approximately in a stable state.

Item Type: Article
DOI/Identification number: 10.1051/0004-6361/201833612
Uncontrolled keywords: ISM: kinematics and dynamics– ISM: clouds– stars: formation
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: James Urquhart
Date Deposited: 03 Dec 2018 16:19 UTC
Last Modified: 11 Jul 2019 14:55 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/70581 (The current URI for this page, for reference purposes)
Urquhart, J.S.: https://orcid.org/0000-0002-1605-8050
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