Astronomy and Astrophysics, volume 501, 89-102 (2009/7-1)
The X-ray view of giga-hertz peaked spectrum radio galaxies.
TENGSTRAND O., GUAINAZZI M., SIEMIGINOWSKA A., FONSECA BONILLA N., LABIANO A., WORRALL D.M., GRANDI P. and PICONCELLI E.
Abstract (from CDS):
This paper presents the X-ray properties of a flux- and volume-limited complete sample of 16 giga-hertz peaked spectrum (GPS) galaxies. This study addresses three basic questions in our understanding of the nature and evolution of GPS sources: a) What is the physical origin of the X-ray emission in GPS galaxies? b) Which physical system is associated with the X-ray obscuration? c) What is the ``endpoint'' of the evolution of compact radio sources? We discuss in this paper the results of the X-ray spectral analysis, and compare the X-ray properties of the sample sources with radio observables. We obtain a 100% (94%) detection fraction in the 0.5-2keV (0.5-10keV) energy band. GPS galaxy X-ray spectra are typically highly obscured (<NHGPS≥ 3x1022cm–2; σNH≃0.5dex). The X-ray column density is larger than the HI column density measured in the radio by a factor 10 to 100. GPS galaxies lie well on the extrapolation to high radio powers of the correlation between radio and X-ray luminosity known in low-luminosity FR I radio galaxies. On the other hand, GPS galaxies exhibit a comparable X-ray luminosity to FR II radio galaxies, notwithstanding their much larger radio luminosity. The X-ray to radio luminosity ratio distribution in our sample is consistent with the bulk of the high-energy emission being produced by the accretion disk, as well as with dynamical models of GPS evolution where X-rays are produced by Compton upscattering of ambient photons. Further support to the former scenario comes from the location of GPS galaxies in the X-ray to O[III] luminosity ratio versus NH plane. We propose that GPS galaxies are young radio sources, which would reach their full maturity as classical FR II radio galaxies. However, column densities ∼1022cm–2 could lead to a significant underestimate of dynamical age determinations based on the hotspot recession velocity measurements.
galaxies: jets - galaxies: active - X-rays: galaxies
Paragraphe 1. 3C 301.1 is a mispirnt for 3C 303.1