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Title:
CI 492GHz mapping towards Cas A
Authors:
Mookerjea, B.; Kantharia, N. G.; Roshi, D. Anish; Masur, M.
Affiliation:
AA(Department of Astronomy, University of Maryland, College Park, MD 20742, USA; KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77, 50937 Köln, Germany), AB(National Centre for Radio Astrophysics, TIFR, Post Bag 3, Ganeshkhind, Pune 411007, India), AC(Raman Research Institute, Sadashivanagar, Bangalore 560080, India), AD(KOSMA, I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77, 50937 Köln, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 371, Issue 2, pp. 761-768. (MNRAS Homepage)
Publication Date:
09/2006
Origin:
MNRAS
MNRAS Keywords:
ISM: clouds: ISM: general: ISM: lines and bands: Galaxy: general: radio lines: general: radio lines: ISM, ISM: clouds, ISM: general, ISM: lines and bands, Galaxy: general, radio lines: general, radio lines: ISM
DOI:
10.1111/j.1365-2966.2006.10700.x
Bibliographic Code:
2006MNRAS.371..761M

Abstract

We have mapped the [CI]3P1-3P0 emission at 492GHz towards the supernova remnant Cas A. We detect [CI] emission from the periphery of the diffuse photon-dominated region (PDR) covering the disc of Cas A, as traced by the carbon recombination lines, as well as from the denser PDRs associated with the molecular clouds towards the south-east. [CI] emission is detected from both the Perseus and Orion arm molecular clouds, with the -47kms-1 Perseus arm feature being strong enough to be detected at all positions. We estimate the C/CO relative abundance to be 0.2 at the position of the identified CO clouds and >1 for most of the cloud. Here we show that the distribution of [CI] emitting regions compared to the C+ region and molecular cloud is consistent with a scenario involving PDRs. Using physical models for PDRs, we constrain the physical properties of the [CI] line-forming regions. We estimate the densities of the [CI] emitting regions to be between 102 and 103cm-3. Based on rather high volume filling factors (~50 per cent), we conclude that [CI] emission mainly arises from diffuse neutral gas in the Perseus arm.

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