PV Diagrams For The Maser Emission Coming From A Keplerian Ring

Details PV Diagrams For The Maser Emission Coming From A Keplerian Ring PV Diagrams For The Maser Emission Coming From A Keplerian Ring

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...21115705u&link_type=abstract

American Astronomical Society, AAS Meeting #211, #157.05

Astronomy and Astrophysics

Astronomy

Scientific paper

We studied the maser emission coming from a thin, planar, gaseous ring in Keplerian rotation around a central mass observed edge-on. Assuming that the absorption coefficient follows a power-law dependence on the distance from the central mass (κ=κ0r-q), we calculated position-velocity (PV) diagrams for the strongest maser emission using different values of the exponent q. We found that, depending on the value of q, these diagrams can be qualitatively different. Specifically, when qɭ the PV diagram is qualitatively similar to the one observed for the water maser emission in the nucleus of the galaxy NGC 4258. This suggests that the absorption coefficient should be a decreasing function of the distance from the central mass in order to have significant emission coming from the inner edge of the amplifying ring, and hence explain the form of the PV diagram delineated by the water masers in this galaxy.

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