Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1201..135n&link_type=abstract
THE MONSTER'S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP Conference Proceedings, Volume 1201, pp. 135-141 (2
Physics
Interstellar Matter, Radio Galaxies, Redshift, Galactic Nuclei, Quasars, Atomic, Molecular, Chemical, And Grain Processes, Radio Galaxies, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies, Galactic Nuclei, Circumnuclear Matter, And Bulges, Quasars
Scientific paper
We present observational constraints on how AGN may regulate the thermal and dynamical state of the interstellar medium in radio galaxies at low and high redshift, and thus star formation and galaxy growth. Radio galaxies at z~2 reveal energetic, extended outflows of few ×1010 Msolar of warm ionized gas with kinetic energies near the binding energy of a massive galaxy, and a remarkable deficit in cold molecular gas. This suggests that powerful AGN feedback may terminate the active phase of growth of massive galaxies as postulated by models of galaxy evolution.
On the example of a nearby radio galaxy we investigate how the AGN may affect the cold/warm ISM. 3C326 N at z = 0.1 is rich in molecular gas but the Schmidt-Kennicutt diagram suggests a much lower star-formation efficiency than in `normal' galaxies. Most of the molecular gas is warm and appears heated by shocks on timescales of few ×104 yrs, shorter than the free-fall time of molecular clouds. We find a fast outflow of warm neutral gas which cannot be driven by star formation or the radiative energy of the AGN. Long dissipation times suggest these conditions will be maintained for 107-8 yrs. We relate these properties to the radio source through an extended 'cocoon model' and discuss how our observations of radio-loud AGN at low and at high-z may help to better understand the role of AGN feedback for the evolution of massive galaxies across cosmic time.
Boulanger Francois
de Breuck Carlos
Lehnert Matt D.
Nesvadba P. H. N.
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