Clumps in IC 348 - Temperature and density profiles of dense cores

Details Clumps in IC 348 - Temperature and density profiles of dense cores Clumps in IC 348 - Temperature and density profiles of dense cores

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...173..324b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 173, no. 2, Feb. 1987, p. 324-336. CNRS-supported research.

Astronomy and Astrophysics

Astrophysics

65

Abundance, Astronomical Spectroscopy, Density Distribution, Molecular Clouds, Temperature Distribution, Ammonia, Astronomical Maps, Carbon Monoxide, Chemical Fractionation, Dark Matter

Scientific paper

High-resolution observations of the dense core of the nearby molecular cloud IC 348 in NH3 with the 100-m telescope and in (C-13)O and C(O-18) molecules with the IRAM 30-m telescope are presented. They reveal three cold, elongated (0.05 by 0.15 pc), and dense clumps with masses in range 2 to 5 solar mass. Kinetic temperatures deduced from NH3 steadily decrease from more than 25 K at the edges down to 12 to 15 K in the clump cores. The line widths decrease from 1.5 km/s at the edges down to 0.4 km/s in the cores. Comparisons with a numerical radiative-transfer model including the three lower rotational levels of para-NH3 indicate that the best-fit density law is n = r exp (-1.3), and that the data are consistent with a linear variation of temperatures and line widths with r. The total NH3 abundance is about 3 x to to the -8th. The (C-13)O and C(O-18) observations indicate that structure is still present at a scale of 20 arcsec, and imply a significant chemical fractionation in the visual extinction range A(V) = 2-5. From a thermal equilibrium model, it is concluded that the dust temperature in the cloud cores must be less than 14 K, and that photoelectric heating, due to the radiation field from the nearby Perseus OB2 cluster, is responsible for the temperature enhancement at the outer edge.

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