Cores in infrared dark clouds (IRDCs) seen in the Hi-GAL survey between l= 300° and 330°

Wilcock, Lucy Ann, Ward-Thompson, Derek ORCID: https://orcid.org/0000-0003-1140-2761, Kirk, Jason M., Stamatellos, Dimitrios, Whitworth, Anthony Peter ORCID: https://orcid.org/0000-0002-1178-5486, Elia, D., Fuller, G. A., DiGiorgio, A., Griffin, Matthew Joseph ORCID: https://orcid.org/0000-0002-0033-177X, Molinari, S., Martin, P., Mottram, J. C., Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Pestalozzi, M., Schisano, E., Plume, R., Smith, H. A. and Thompson, M. A. 2012. Cores in infrared dark clouds (IRDCs) seen in the Hi-GAL survey between l= 300° and 330°. Monthly Notices of the Royal Astronomical Society 422 (2) , pp. 1071-1082. 10.1111/j.1365-2966.2012.20680.x

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Abstract

We have used data taken as part of the Herschel infrared Galactic Plane survey (Hi-GAL) to study 3171 infrared dark cloud (IRDC) candidates that were identified in the mid-IR (8 μm) by Spitzer (we refer to these as ‘Spitzer-dark’ regions). They all lie in the range l= 300–330° and |b|≤ 1°. Of these, only 1205 were seen in emission in the far-IR (250–500 μm) by Herschel (we call these ‘Herschel-bright’ clouds). It is predicted that a dense cloud will not only be seen in absorption in the mid-IR, but will also be seen in emission in the far-IR at the longest Herschel wavebands (250–500 μm). If a region is dark at all wavelengths throughout the mid-IR and far-IR, then it is most likely to be simply a region of lower background IR emission (a ‘hole in the sky’). Hence, it appears that previous surveys, based on Spitzer and other mid-IR data alone, may have overestimated the total IRDC population by a factor of ∼2. This has implications for estimates of the star formation rate in IRDCs in the Galaxy. We studied the 1205 Herschel-bright IRDCs at 250 μm and found that 972 of them had at least one clearly defined 250-μm peak, indicating that they contained one or more dense cores. Of these, 653 (67 per cent) contained an 8-μm point source somewhere within the cloud, 149 (15 per cent) contained a 24-μm point source but no 8-μm source and 170 (18 per cent) contained no 24- or 8-μm point sources. We use these statistics to make inferences about the lifetimes of the various evolutionary stages of IRDCs.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Advanced Research Computing @ Cardiff (ARCCA) Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	stars: formation
Publisher:	Wiley
ISSN:	0035-8711
Last Modified:	05 Nov 2022 15:49
URI:	https://orca.cardiff.ac.uk/id/eprint/24181

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