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Dynamical Models of the Maser in NGC 4258

Published online by Cambridge University Press:  12 April 2016

J.M. Moran
J.M. Moran*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA

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The presence of two quasars symmetrically displaced from the nucleus of the galaxy NGC 4258 (Pietsch et al. 1994) has given rise to some speculation that they might have some dynamical connection with the high-velocity maser emission seen in the nucleus (Burbidge 1996; Ozernoy 1996). The case that the masers define a simple Keplerian disk is very compelling; nonetheless, it is instructive to investigate whether any other dynamical models could fit the available data.

The evidence that the masers define a thin Keplerian disk can be found in Miyoshi et al. (1995) and Moran et al. (1995). Some of the relevant data are shown elsewhere in this volume (Fig. 2 of Greenhill’s paper). The basic analysis is as follows. The features near the systemic velocity of 470km s−1 show a linear dependence of line-of-sight velocity versus distance along the major axis, while the redshifted and blueshifted high-velocity features show a nearly Keplerian dependence with distance.

Type
VIII. Megamasers in Active Galaxies
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 402 - 405
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

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