Hostname: page-component-78c5997874-j824f Total loading time: 0 Render date: 2024-11-13T05:16:06.732Z Has data issue: false hasContentIssue false
  • English
  • Français

AGN feedback by relativistic jets

Published online by Cambridge University Press:  24 March 2015

G. V. Bicknell ,
B. R. McNamara ,
M. A. Nawaz ,
R. S. Sutherland ,
M. Umemura  and
A. Y. Wagner
G. V. Bicknell
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Weston ACT 2611, Australia email: geoff.bicknell@anu.edu.au
B. R. McNamara
Affiliation:
Department of Physics and Astronomy, University of Waterloo, Waterloo, ON, Canada
M. A. Nawaz
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Weston ACT 2611, Australia email: geoff.bicknell@anu.edu.au
R. S. Sutherland
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Weston ACT 2611, Australia email: geoff.bicknell@anu.edu.au
M. Umemura
Affiliation:
Center for Computational Science, Tsukuba University, 1-1-1 Tennodai, Tsukuba, Ibaraki, 305-8577Japan
A. Y. Wagner
Affiliation:
Center for Computational Science, Tsukuba University, 1-1-1 Tennodai, Tsukuba, Ibaraki, 305-8577Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Feedback provided by relativistic jets may be effective in shaping the galaxy luminosity function. The quenching mode (quasar mode) at redshifts ~2-3 potentially disperses gas in star-forming galaxies. The maintenance mode (radio mode) heats the gas in galaxy clusters counteracting cooling flows. A number of authors have examined the effect of relativistic jets in dispersing clouds in the kpc-scale inhomogeneous interstellar medium of evolving galaxies. We have also investigated a particular case of maintenance-mode feedback in our simulation of the iconic radio galaxy / cooling flow cluster Hydra A. Modelling of the knots produced by the jets in the inner 10 kpc provides an estimate of 0.8 – 0.9 c for the velocities of the jets in agreement with other velocity estimates for FR1 jets. The addition of jet precession provides realistic simulations of the morphology of the Hydra A radio source and raises interesting questions as to the role of black hole and disk precession, in general, in galaxy formation.

Keywords

galaxies: activegalaxies: jetsradio continuum: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S313: Extragalactic jets from every angle , September 2014 , pp. 101 - 107
Copyright
Copyright © International Astronomical Union 2015 

References

Bicknell, G., Sutherland, R., van Breugel, W., et al. 2000, ApJL, 540, 678CrossRefGoogle Scholar
Croton, D. J., et al. 2006a, MNRAS, 367, 864CrossRefGoogle Scholar
Croton, D. J., et al. 2006b, MNRAS, 365, 11CrossRefGoogle Scholar
Fabian, A. C. 1999, MNRAS, 308, L39CrossRefGoogle Scholar
Gaibler, V., Khochfar, S., & Krause, M. 2011, MNRAS, 411, 155CrossRefGoogle Scholar
Gaibler, V., Khochfar, S., Krause, M., & Silk, J. 2012, MNRAS, 425, 438CrossRefGoogle Scholar
Gebhardt, K., et al. 2000, ApJL, 539, L13CrossRefGoogle Scholar
King, A. 2003, ApJ, 596, L27CrossRefGoogle Scholar
King, A. 2005, ApJL, 635, L121CrossRefGoogle Scholar
Lehnert, M. D., Tasse, C., Nesvadba, N. P. H., et al. 2011, A&A, 532, L3Google Scholar
Magorrian, J., et al. 1998, AJ, 115, 2285CrossRefGoogle Scholar
McNamara, B. R. & Nulsen, P. E. J. 2007, ARAA, 45, 117CrossRefGoogle Scholar
Morganti, R., Fogasy, J., Paragi, Z., Oosterloo, T., & Orienti, M. 2013, Science, 341, 1082CrossRefGoogle Scholar
Nesvadba, P. H. N. & Lehnert, M. D. 2008, in SF2A-2008, ed. Charbonnel, C., Combes, F., & Samadi, R., 377Google Scholar
Rasera, Y. & Teyssier, R. 2006, A&A, 445, 1Google Scholar
Saxton, C. J., Bicknell, G. V., Sutherland, R. S., & Midgley, S. 2005, MNRAS, 359, 781CrossRefGoogle Scholar
Scharf, C., Smail, I., Ivison, R., Bower, R., van Breugel, W., & Reuland, M. 2003, ApJ, 596, 105CrossRefGoogle Scholar
Schechter, P. 1976, ApJ, 203, 297CrossRefGoogle Scholar
Silk, J. 2013, ApJ, 772, 112CrossRefGoogle Scholar
Silk, J. & Rees, M. J. 1998, A&A, 331, L1Google Scholar
Sutherland, R. S. & Bicknell, G. V. 2007, ApJS, 173, 37CrossRefGoogle Scholar
Tremaine, S., et al. 2002, ApJ, 574, 740CrossRefGoogle Scholar
Wagner, A. Y. & Bicknell, G. V. 2011, ApJ, 728, 29CrossRefGoogle Scholar
Wagner, A. Y., Bicknell, G. V., & Umemura, M. 2012, ApJ, 757, 136CrossRefGoogle Scholar
Wise, M. W., McNamara, B. R., Nulsen, P. E. J., et al. 2007, ApJ, 659, 1153CrossRefGoogle Scholar