EDP Sciences
Free Access
Volume 386, Number 1, April IV 2002
Page(s) L1 - L4
Section Letters
DOI https://doi.org/10.1051/0004-6361:20020135
Published online 15 April 2002

A&A 386, L1-L4 (2002)
DOI: 10.1051/0004-6361:20020135


Absorbers and globular cluster formation in powerful high-redshift radio galaxies

M. Krause

Landessternwarte Königstuhl, 69117 Heidelberg, Germany

(Received 14 December 2001 / Accepted 23 January 2002)

A radiative hydrodynamic simulation for a typical, powerful high redshift radio galaxy is presented. The jet is injected at one third the speed of light into a 10 000 times denser, homogeneous medium. In the beginning of the simulation, the bow shock consists of a spherical shell that is similar to a spherical blast wave. This shell cools radiatively down to ${\approx}10^4$ K, providing after $6 \times 10^6$ yrs a neutral column of $3.8 \times 10^{21}\,\mathrm{cm}^{-2}$ around the whole system. The shell starts to fragment and forms condensations. This absorbing screen will cover a smaller and smaller fraction of the radio source, and therefore the emission line region, and eventually form stars in typically 104 globular clusters of $10^6 \ M_\odot$. Approximately $10^9 \ M_\odot$ are entrained into the radio cocoon. This gas, cooling and illuminated from the radio source, could be the emission line gas observed in high redshifted radio galaxies and radio loud quasars. The neutral column behind the bow shock can account for the absorption found in almost all of the small sources. The globular cluster excess of ${\approx}10^4$ systems found in present day brightest cluster galaxies (BCGs), which are believed to be the vestiges of these objects, is consistent with the presented scenario.

Key words: hydrodynamics -- instabilities -- shock waves -- galaxies: jets -- radiation mechanisms: thermal -- intergalactic medium

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© ESO 2002

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