Facial reconstruction

Search LJMU Research Online

Browse Repository | Browse E-Theses

Star formation in a high-pressure environment: An SMA view of the Galactic centre dust ridge

Walker, DL, Longmore, SN, Zhang, Q, Battersby, C, Keto, E, Kruijssen, JMD, Ginsburg, A, Lu, X, Henshaw, JD, Kauffmann, J, Pillai, T, Mills, EAC, Walsh, AJ, Bally, J, Ho, LC, Immer, K and Johnston, KG (2017) Star formation in a high-pressure environment: An SMA view of the Galactic centre dust ridge. Monthly Notices of the Royal Astronomical Society, 474 (2). pp. 2373-2388. ISSN 0035-8711

Star formation in a high-pressure environment An SMA view of the Galactic centre dust ridge.pdf - Published Version

Download (4MB) | Preview


The star formation rate in the Central Molecular Zone (CMZ) is an order of magnitude lower than predicted according to star formation relations that have been calibrated in the disc of our own and nearby galaxies. Understanding how and why star formation appears to be different in this region is crucial if we are to understand the environmental dependence of the star formation process. Here, we present the detection of a sample of high-mass cores in the CMZ's "dust ridge" that have been discovered with the Submillimeter Array as part of the CMZoom survey. These cores range in mass from ~ 50 - 2150 Msun within radii of 0.1 - 0.25 pc. All appear to be young (pre-UCHII), meaning that they are prime candidates for representing the initial conditions of high-mass stars and sub-clusters. We report that at least two of these cores ('c1' and 'e1') contain young, high-mass protostars. We compare all of the detected cores with high-mass cores in the Galactic disc and find that they are broadly similar in terms of their masses and sizes, despite being subjected to external pressures that are several orders of magnitude greater - ~ 10^8 K/cm^3, as opposed to ~ 10^5 K/cm^3. The fact that > 80% of these cores do not show any signs of star-forming activity in such a high-pressure environment leads us to conclude that this is further evidence for an increased critical density threshold for star formation in the CMZ due to turbulence.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: astro-ph.GA; astro-ph.GA
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Related URLs:
Date Deposited: 10 Nov 2017 13:01
Last Modified: 04 Sep 2021 11:01
DOI or ID number: 10.1093/mnras/stx2898
URI: https://researchonline.ljmu.ac.uk/id/eprint/7529
View Item View Item