Determinations of Key Physical Parameters Related to Classical Double Radio Sources

Details Determinations of Key Physical Parameters Related to Classical Double Radio Sources Determinations of Key Physical Parameters Related to Classical Double Radio Sources

2000-06-30

arxiv.org/abs/astro-ph/0006455v1

Astronomy and Astrophysics

Astrophysics

53 pages, includes 13 figures, accepted by ApJ

Scientific paper

10.1086/317218

Multi-frequency radio observations of the radio bridge of a powerful classical double radio source can be used to determine: the beam power of the jets emanating from the AGN; the total time the source will actively produce jets that power large-scale radio emission; the thermal pressure of the medium in the vicinity of the radio source; and the total mass, including dark matter, of the galaxy or cluster of galaxies traced by the ambient gas that surrounds the radio source. Empirical determinations of each of these quantities are obtained and analyzed for 22 radio sources. Typical beam powers are about $10^{45} {erg s}^{-1}$. The characteristic or total time the AGN will actively produce a collimated outflow is estimated. Typical total lifetimes are $\sim (10^7$ to $10^8$) years. Total masses, and mass-density profiles, similar to those of low-redshift clusters of galaxies are obtained. Thus, some clusters of galaxies, or cores of clusters, exist at redshifts of one to two. A new method of estimating the thermal pressure of the ambient gas in the vicinity of a powerful classical double radio source is presented. This new estimate is independent of synchrotron and inverse Compton aging arguments, and depends only upon the properties of the radio lobe and the shape of the radio bridge. Thermal pressures on the order of $10^{-10} {dyne cm}^{-2}$, typical of gas in low-redshift clusters of galaxies, are found for the environments of the sources studied here. It is shown that appreciable amounts of cosmic microwave background diminution (the Sunyaev-Zel'dovich effect) are expected from many of these clusters. This could be detected at high frequency where the emission from the radio sources is weak.

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