Temperatures and sizescales of giant cloud complexes in the spiral galaxy IC 342

Details Temperatures and sizescales of giant cloud complexes in the spiral galaxy IC 342 Temperatures and sizescales of giant cloud complexes in the spiral galaxy IC 342

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...113..155h&link_type=abstract

Astronomy and Astrophysics, vol. 113, no. 1, Sept. 1982, p. 155-164. Research supported by the Miller Institute for Basic Resea

Astronomy and Astrophysics

Astronomy

15

Ammonia, Cosmic Gases, Galactic Nuclei, Gas Temperature, Molecular Clouds, Spiral Galaxies, Astronomical Spectroscopy, B Stars, Carbon Monoxide, Emission Spectra, Line Spectra, Milky Way Galaxy, O Stars, Radio Astronomy, Stellar Evolution

Scientific paper

The (J, K) equals (1,1) and (2,2) inversion lines of NH3 have been detected toward the nucleus of IC 342. The relative intensities of these lines indicate that the gas temperature is on the order of 50 K. It is argued that this gas is probably heated by collisions with warm dust grains at roughly the observed gas temperature. It is then deduced that the total extent of the NH3 emission complex is on the order of 25-30 pc. The observed CO emission probably arises from cooler envelopes surrounding the NH3 emission regions. If these giant cloud complexes are to bear a resemblance to Galactic observations, the morphology probably consists of approximately 100 giant molecular clouds each with an embedded OB cluster. The total mass for molecular gas is then 10 to the 7th-10 to the 8th solar masses. It is suggested that the large number of molecular clouds accompanied by active OB star formation is probably a time-stable configuration. It is argued that collisions between these molecular clouds in the nucleus may in fact be responsible for both maintaining stability against further collapse and initiating star formation.

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