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First Detection of 661 GHz 13CO J=6 →5: Large Amounts of Warm Molecular Gas

Published online by Cambridge University Press:  03 August 2017

U.U. Graf ,
R. Genzel ,
A.I. Harris ,
R.E. Hills ,
A.P.G. Russell  and
J. Stutzki
U.U. Graf
Affiliation:
MPI für extraterrestrische Physik, Garching (FRG)
R. Genzel
Affiliation:
MPI für extraterrestrische Physik, Garching (FRG)
A.I. Harris
Affiliation:
MRAO, Cavendish Laboratory, Cambridge (UK)
R.E. Hills
Affiliation:
MRAO, Cavendish Laboratory, Cambridge (UK)
A.P.G. Russell
Affiliation:
MPI für extraterrestrische Physik, Garching (FRG) Joint Astronomy Centre, Hilo, Hawaii (USA)
J. Stutzki
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Köln (FRG)

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Submillimeter and far-infrared observations of carbon monoxide (Jaffe, Harris, and Genzel 1987; Genzel, Poglitsch, and Stacey 1988; Schmid-Burgk et al. 1989; Boreiko, Betz, and Zmuidzinas 1989) have indicated the presence of warm, dense molecular gas near regions of recent star forming activity. Estimates based on the comparison of mid-J (submm) and high-J (far-IR) 12CO lines in M17 and S106 (Harris et al. 1987a) gave a lower limit of ≈1018 cm−2 (τ(12CO 7 →6) ≈ 1) to the CO column density of quiescent (Δv ≤ 10 km/s) gas at temperatures of at least 100 K and H2 densities of 104 to 106 cm−3. The mid-J 12CO lines are likely to be optically thick in most sources. In order to obtain a better estimate of the column densities, it is thus of great interest to observe isotopic mid-J CO lines, which are likely to be optically thin.

Type
Poster Sessions
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 424 - 426
Copyright
Copyright © Kluwer 1991 

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