Properties of dust in the high-latitude translucent cloud L1780

Free access article

Issue		A&A Volume 451, Number 3, June I 2006


Page(s)		961 - 971
Section		Interstellar and circumstellar matter
DOI		http://dx.doi.org/10.1051/0004-6361:20053467

A&A 451, 961-971 (2006)
DOI: 10.1051/0004-6361:20053467

I. Spatially distinct dust populations and increased dust emissivity from ISO observations*

M. Ridderstad¹, M. Juvela¹, K. Lehtinen¹, D. Lemke² and T. Liljeström¹

¹ Helsinki University Observatory, Tähtitorninmäki, PO Box 14, 00014 University of Helsinki, Finland
e-mail: marianna@astro.helsinki.fi
² Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Germany

(Received 18 May 2005 / Accepted 26 January 2006)

Abstract
We have analyzed the properties of dust in the high galactic latitude translucent cloud Lynds 1780 using ISOPHOT maps at 100 $\mu$ m and 200 $\mu$ m and raster scans at 60 $\mu$ m, 80 $\mu$ m, 100 $\mu$ m, 120 $\mu$ m, 150 $\mu$ m and 200 $\mu$ m. In far-infrared (FIR) emission, the cloud has a single core that coincides with the maxima of visual extinction and 200 $\mu$ m optical depth. At the resolution of 3.0 $\arcmin$ , the maximum visual extinction is 4.0 mag. At the cloud core, the minimum temperature and the maximum 200 $\mu$ m optical depth are 14.9 $\pm$ 0.4 K and 2.0 $\pm$ 0.2 $\times$ 10^-3, respectively, at the resolution of 1.5 $\arcmin$ . The cloud mass is estimated to be 18 $M_{\odot}$ . The FIR observations, combined with IRAS observations, suggest the presence of different, spatially distinct dust grain populations in the cloud: the FIR core region is the realm of the "classical" large grains, whereas the very small grains and the PAHs have separate maxima on the Eastern side of the cold core, towards the "tail" of this cometary-shaped cloud. The color ratios indicate an overabundance of PAHs and VSGs in L1780. Our FIR observations combined with the optical extinction data indicate an increase of the emissivity of the big grain dust component in the cold core, suggesting grain coagulation or some other change in the properties of the large grains. Based on our observations, we also address the question, to what extent the 80 $\mu$ m emission and even the 100 $\mu$ m and the 120 $\mu$ m emission contain a contribution from the small-grain component.

Key words: ISM: clouds -- infrared: ISM -- ISM: individual objects: L1780

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