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Ammonia clumps in the Orion and Cepheus clouds

Published online by Cambridge University Press:  03 August 2017

J. Harju ,
C.M. Walmsley  and
J.G.A. Wouterloot
J. Harju
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki
C.M. Walmsley
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn
J.G.A. Wouterloot
Affiliation:
I. Physikalisches Institut, Universität zu Köln

Abstract

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We present statistics of clump properties in the Orion and Cepheus cloud complexes based on ammonia mapping observations. Surroundings of about 50 IRAS sources earlier found to have associated molecular line emission (Wouterloot, Walmsley and Henkel, 1988) were mapped in NH3(1,1) and (2,2) with the Effelsberg 100-m telescope. Our main interest has been in determining the clump sizes and masses on the basis of the ammonia column density distribution, which together with the observed velocity dispersion lead to a rough estimate of the dynamical state. We also have studied the star-clump separations which should give us estimates of the source ages. Special attention has been paid to comparison of our Orion data with the Benson and Myers (1989, hereafter BM89) results in Taurus because the linear resolutions in the two studies are similar.

Type
Poster Sessions
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 436 - 437
Copyright
Copyright © Kluwer 1991 

References

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