Far-infrared and molecular line observations of Lynds 183 – Studies of cold gas and dust ^*

¹ Helsinki University Observatory, Tähtitorninmäki, PO Box 14, SF-00014 University of Helsinki, Finland
² Helsinki University Observatory, Tähtitorninmäki, PO Box 14, SF-00014 University of Helsinki, Finland
³ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁴ ISO Data Centre, Astrophysics Division, Space Science Department of ESA, Villafranca del Castillo, PO Box 50727, 28080 Madrid, Spain
⁵ Astrophysics Division, Space Science Department of ESA, ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands

Corresponding author: M. Juvela, mjuvela@astro.helsinki.fi

Received: 25 September 2001
Accepted: 29 October 2001

Abstract

We have mapped the dark cloud L183 in the far-infrared at 100 μm and 200 μm with the ISOPHOT photometer aboard the ISO satellite. The observations make it possible for the first time to study the distribution and properties of the large dust grains in L183 without confusion from smaller grains. The observations show clear colour temperature variations which are likely to be caused by changes in the emission properties of the dust particles. In the cloud core the far-infrared colour temperature drops below 12 K. The data allow a new determination of the cloud mass and the mass distribution based on dust emission. The estimated mass within a radius of 10′ from the cloud centre is 25 . We have mapped the cloud in several molecular lines including DCO+(2–1) and H¹³CO+(1–0). These species are believed to be tracers of cold and dense molecular material and we detect a strong anticorrelation between the DCO+ emission and the dust colour temperatures. In particular, the DCO+(2–1) emission is not detected towards the maximum of the 100 μm emission where the colour temperature rises above 15 K. The H¹³CO+ emission follows closely the DCO+ distribution but CO isotopes show strong emission even towards the 100 μm peak. Detailed comparison of the DCO+ and C¹⁸O maps shows sharp variations in the relative intensities of the species. Morphologically the 200 μm dust emission traces the distribution of dense molecular material as seen e.g. in C¹⁸O lines. A comparison with dust column density shows, however, that C¹⁸O is depleted by a factor of ~1.5 in the cloud core. We present results of R- and B-band starcounts. The extinction is much better correlated with the 200m than with the 100 μm emission. Based on the 200 μm correlation at low extinction values we deduce a value of ~17m for the visual extinction towards the cloud centre where no background stars are observed anymore.