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Dynamical Models of Emission-Line Gas in Radio Galaxies

Published online by Cambridge University Press:  25 May 2016

A. M. Koekemoer  and
G. V. Bicknell
A. M. Koekemoer
Affiliation:
Institut d'Astrophysique de Paris 98bis Bd. Arago, 75014 Paris, France ANU Astrophysical Theory Centre Australian National University, Canberra, ACT 0200, Australia
G. V. Bicknell
Affiliation:
Institut d'Astrophysique de Paris 98bis Bd. Arago, 75014 Paris, France ANU Astrophysical Theory Centre Australian National University, Canberra, ACT 0200, Australia

Extract

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Extended emission-line regions (EELRs) in radio ellipticals are generally thought to trace gas acquired externally, eg. through interaction with a gas-rich disk galaxy (Athanassoula and Bosma 1985, Barnes and Hernquist 1992, Hernquist and Mihos 1995). We examine here the dynamical evolution of gas in mergers, focussing on the conditions required for collisions between streams of gas. We find that such collisions can occur over a relatively wide range of encounter geometries, producing large-velocity-amplitude kinematic signatures characteristic of those observed in EELRs. This is relevant to the formation of shocks, which can account for the ionization properties of EELRs (Koekemoer and Bicknell, this conference).

Type
Radio Source Modelling and Emission Mechanisms
Information
Symposium - International Astronomical Union , Volume 175: Extragalactic Radio Sources , 1996 , pp. 471 - 472
Copyright
Copyright © Kluwer 1996 

References

Athanassoula, E. and Bosma, A.: 1985, Ann. Rev. Astron. Ap. 23, 147 Google Scholar
Barnes, J. E. and Hernquist, L.: 1992, Ann. Rev. Astron. Ap. 30, 705 CrossRefGoogle Scholar
Hernquist, L. and Mihos, J. C.: 1995, Ap.J. 448, 41 Google Scholar
Koekemoer, A. M. and Bicknell, G. V.: 1995, in preparation Google Scholar