A NIKA view of two star-forming infrared dark clouds: dust emissivity variations and mass concentration

Rigby, Andrew, Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Adam, R, Ade, Peter ORCID: https://orcid.org/0000-0002-5127-0401, Andre, P, Aussel, H, Beelen, A, Benoît, A, Bracco, A, Bideaud, A, Bourrion, O, Calvo, M, Catalano, A, Clark, Christopher J. R., Comis, B, De Petris, M, Désert, F.-X., Doyle, Simon ORCID: https://orcid.org/0000-0002-9054-986X, Driessen, D. F.C, Goupy, J, Kramer, C, Lagache, G, Leclercq, S, Lestrade, J.-F., Macías-Pérez, J.F., Mauskopf, Philip ORCID: https://orcid.org/0000-0001-6397-5516, Mayet, F, Monfardini, A, Pascale, Enzo ORCID: https://orcid.org/0000-0002-3242-8154, Perotto, L, Pisano, Giampaolo ORCID: https://orcid.org/0000-0003-4302-5681, Ponthieu, N, Revéret, V, Ritacco, A, Romero, C, Roussel, H, Ruppin, F, Schuster, K, Sievers, A, Triqueneaux, S, Tucker, Carole ORCID: https://orcid.org/0000-0002-1851-3918 and Zylka, R 2018. A NIKA view of two star-forming infrared dark clouds: dust emissivity variations and mass concentration. Astronomy and Astrophysics 615 , A18. 10.1051/0004-6361/201732258

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Abstract

Context. The thermal emission of dust grains is a powerful tool for probing cold, dense regions of molecular gas in the interstellar medium, and so constraining dust properties is key to obtaining accurate measurements of dust mass and temperature. Aims. By placing constraints on the dust emissivity spectral index, β, towards two star-forming infrared dark clouds – SDC18.888–0.476 and SDC24.489–0.689 – we aim to evaluate the role of mass concentration in the associated star-formation activity. Methods. We exploited the simultaneous 1.2 and 2.0 mm imaging capability of the NIKA camera on the IRAM 30 m telescope to construct maps of β for both clouds, and by incorporating Herschel observations, we created H2 column density maps with 13′′ angular resolution. Results. While we find no significant systematic radial variations around the most massive clumps in either cloud on ≳0.1 pc scales, their mean β values are significantly different, with β̅ = 2.07 ± 0.09 (random) ± 0.25 (systematic) for SDC18.888–0.476 and β̅ = 1.71 ± 0.09 (random) ± 0.25 (systematic) for SDC24.489–0.689. These differences could be a consequence of the very different environments in which both clouds lie, and we suggest that the proximity of SDC18.888–0.476 to the W39 H II region may raise β on scales of ~1 pc. We also find that the mass in SDC24.489–0.689 is more centrally concentrated and circularly symmetric than in SDC18.888–0.476, and is consistent with a scenario in which spherical globally-collapsing clouds concentrate a higher fraction of their mass into a single core than elongated clouds that will more easily fragment, distributing their mass into many cores. Conclusions. We demonstrate that β variations towards interstellar clouds can be robustly constrained with high signal-to-noise ratio (S/N) NIKA observations, providing more accurate estimates of their masses. The methods presented here will be applied to the Galactic Star Formation with NIKA2 (GASTON) guaranteed time large programme, extending our analysis to a statistically significant sample of star-forming clouds.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	EDP Sciences
ISSN:	0004-6361
Funders:	STFC, RS
Date of First Compliant Deposit:	30 January 2018
Date of Acceptance:	29 January 2018
Last Modified:	11 Nov 2024 22:00
URI:	https://orca.cardiff.ac.uk/id/eprint/108595

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