Cloud structure of three Galactic infrared dark star-forming regions from combining ground and space based bolometric observations

Lin, Y and Liu, HB and Dale, JE and Li, D and Busquet, G and Zhang, Z-Y and Ginsburg, A and Galvan-Madrid, R and Kovacs, A and Koch, E and Qian, L and Wang, K and Longmore, SN and Chen, H-R and Walker, DL (2017) Cloud structure of three Galactic infrared dark star-forming regions from combining ground and space based bolometric observations. The Astrophysical Journal, 840 (1). ISSN 1538-4357

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Open Access URL: https://arxiv.org/pdf/1704.06448.pdf (Accepted version)

Abstract

We have modified the iterative procedure introduced by Lin et al. (2016), to systematically combine the submm images taken from ground based (e.g., CSO, JCMT, APEX) and space (e.g., Herschel, Planck) telescopes. We applied the updated procedure to observations of three well studied Infrared Dark Clouds (IRDCs): G11.11-0.12, G14.225-0.506 and G28.34+0.06, and then performed single-component, modified black-body fits to derive $\sim$10$"$ resolution dust temperature and column density maps. The derived column density maps show that these three IRDCs exhibit complex filamentary structures embedding with rich clumps/cores. We compared the column density probability distribution functions (N-PDFs) and two-point correlation (2PT) functions of the column density field between these IRDCs with several OB cluster-forming regions. Based on the observed correlation and measurements, and complementary hydrodynamical simulations for a 10$^{4}$ $\rm M_{\odot}$ molecular cloud, we hypothesize that cloud evolution can be better characterized by the evolution of the (column) density distribution function and the relative power of dense structures as a function of spatial scales, rather than merely based on the presence of star-forming activity. Based on the small analyzed sample, we propose four evolutionary stages, namely: {\it cloud integration, stellar assembly, cloud pre-dispersal and dispersed-cloud.} The initial {\it cloud integration} stage and the final {\it dispersed cloud} stage may be distinguished from the two intermediate stages by a steeper than $-$4 power-law index of the N-PDF. The {\it cloud integration} stage and the subsequent {\it stellar assembly} stage are further distinguished from each other by the larger luminosity-to-mass ratio ($>$40 $\rm L_{\odot}/M_{\odot}$) of the latter.

Item Type: Article astro-ph.GA; astro-ph.GA Q Science > QB AstronomyQ Science > QC Physics Astrophysics Research Institute American Astronomical Society Author 28 Apr 2017 10:17 30 Jun 2017 10:43 10.3847/1538-4357/aa6c67 http://researchonline.ljmu.ac.uk/id/eprint/6318