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PV diagrams for the maser emission from a Keplerian ring

Published online by Cambridge University Press:  01 March 2007

L. Uscanga ,
J. Cantó  and
A. C. Raga
L. Uscanga
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Ap. 3-72, 58089 Morelia, Mich., Mexico email: l.uscanga@astrosmo.unam.mx
J. Cantó
Affiliation:
Instituto de Astronomía, UNAM, Ap. 70-264, 04510 México, D.F., Mexico
A. C. Raga
Affiliation:
Instituto de Ciencias Nucleares, UNAM, Ap. 70-543, 04510 México, D.F., Mexico
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Abstract

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We study the maser emission arising from a thin, planar, gaseous ring in Keplerian rotation around a central mass when it is observed edge-on. Assuming that the absorption coefficient within the amplifying ring is a decreasing function of distance from the central mass (i.e., κ = κ0r−q), we calculated position-velocity (PV) diagrams for the most intense maser features using different values of the exponent q. We found that, depending on the value of q, these diagrams can be qualitatively different.

Keywords

galaxies: individual (NGC 4258)galaxies: nucleimasers
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 410 - 411
Copyright
Copyright © International Astronomical Union 2008

References

Miyoshi, M., Moran, J., Herrnstein, J. et al. , 1995, Nature, 373, 127CrossRefGoogle Scholar
Uscanga, L., Cantó, J., & Raga, A. C. 2007, ApJ, in pressGoogle Scholar
Watson, W. D., & Wallin, B. K. 1994, ApJ (Letters), 432, L35CrossRefGoogle Scholar