Cardiff University | Prifysgol Caerdydd ORCA
Online Research @ Cardiff 
WelshClear Cookie - decide language by browser settings

Kinematic structure of massive star-forming regions. I. accretion along filaments

Tackenberg, Jochen, Beuther, Henrik, Henning, Thomas, Linz, Hendrik, Sakai, T, Ragan, Sarah, Krause, Oliver, Nielbock, Markus, Hennemann, Martin, Pitann, Jan and Schmiedeke, Anika 2014. Kinematic structure of massive star-forming regions. I. accretion along filaments. Astronomy and Astrophysics 565 , A101. 10.1051/0004-6361/201321555

[img]
Preview
PDF - Published Version
Download (4MB) | Preview

Abstract

Context. The mid- and far-infrared view on high-mass star formation, in particular with the results from the Herschel space observatory, has shed light on many aspects of massive star formation. However, these continuum studies lack kinematic information. Aims: We study the kinematics of the molecular gas in high-mass star-forming regions. Methods: We complemented the PACS and SPIRE far-infrared data of 16 high-mass star-forming regions from the Herschel key project EPoS with N2H+ molecular line data from the MOPRA and Nobeyama 45 m telescope. Using the full N2H+ hyperfine structure, we produced column density, velocity, and linewidth maps. These were correlated with PACS 70 μm images and PACS point sources. In addition, we searched for velocity gradients. Results: For several regions, the data suggest that the linewidth on the scale of clumps is dominated by outflows or unresolved velocity gradients. IRDC 18454 and G11.11 show two velocity components along several lines of sight. We find that all regions with a diameter larger than 1 pc show either velocity gradients or fragment into independent structures with distinct velocities. The velocity profiles of three regions with a smooth gradient are consistent with gas flows along the filament, suggesting accretion flows onto the densest regions. Conclusions: We show that the kinematics of several regions have a significant and complex velocity structure. For three filaments, we suggest that gas flows toward the more massive clumps are present.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: EDP Sciences
ISSN: 0004-6361
Date of First Compliant Deposit: 27 November 2017
Date of Acceptance: 7 January 2014
Last Modified: 28 Nov 2017 22:04
URI: http://orca.cf.ac.uk/id/eprint/106508

Citation Data

Cited 21 times in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item Edit Item

Downloads

Downloads per month over past year

View more statistics