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Emission from Interstellar Gas and Dust in M31

Published online by Cambridge University Press:  03 August 2017

E. Koper ,
T.M. Dame ,
F.P. Israel  and
P. Thaddeus
E. Koper
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
T.M. Dame
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, U.S.A.
F.P. Israel
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
P. Thaddeus
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, U.S.A.

Abstract

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We present preliminary results of a comparison of the spatial distributions of 100 μm, Hi and CO emission in M31. Using a scatter diagram of 100 μm intensity versus H i column density, we have derived an upper limit to the molecular gas column density. We have compared these values with the velocity-integrated CO intensity to find an upper limit to the CO-to-H2 conversion factor in the ring of M 31 of 5 1020 mol cm—2 [K km s—1]—1.

Type
I- Local Group Galaxies
Information
Symposium - International Astronomical Union , Volume 146: Dynamics of Galaxies and their Molecular Cloud Distributions , 1991 , pp. 27 - 28
Copyright
Copyright © Kluwer 1991 

References

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