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3.21. Atomic ISM in the nuclear starburst regions of M82 & NGC 253

Published online by Cambridge University Press:  25 May 2016

M. S. Yun ,
P. T. P. Ho  and
K. Y. Lo
M. S. Yun
Affiliation:
National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM 87801 (USA)
P. T. P. Ho
Affiliation:
Smithsonian Astronomy Observatory, 60 Garden St., Cambridge, MA 02138 (USA)
K. Y. Lo
Affiliation:
University of Illinois, Astronomy Department, Urbana, IL 61801 (USA)

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M82 (NGC 3034) is a nearby (D = 3.3 Mpc) “prototypical” starburst galaxy which emits most of its luminosity in the infrared (LIR = 3×1010L⊙, see Rieke et al. 1980). M82 is also a strong radio source 3C 231, with numerous compact knots which are thought to be young SNR's (Kronberg et al., 1981; Muxlow et al., 1994). Its strong 1.4 GHz radio continuum is extended over the entire 500 pc nuclear starburst region, and the HI absorption is easily mapped at 2″ (30 pc) resolution using the VLA. The resulting velocity integrated optical depth (τΔV) map can be converted to HI column density map if HI spin temperature (Tsp) is known.

Type
Part I. Stellar Cluster, Star Formation
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 131 - 132
Copyright
Copyright © Kluwer 1998 

References

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