The X-ray emission in young radio AGNs
arXiv:2006.01079 · doi:10.1093/mnras/staa1559
Abstract
In this work, we investigated the X-ray emission for a sample of young radio AGNs by combining their data from Chandra/XMM-Newton and at other wavebands. We find strong correlations between the X-ray luminosity in 210 keV and the radio luminosities at 5 GHz for VLBI radio-core, VLA radio-core and FIRST component, indicating that both pc- and kpc-scale radio emission strongly correlate with X-ray emission in these sources. We find approximately linear dependence of radio on X-ray luminosity in the sources with radiative efficient accretion flows (i.e., the Eddington ratio ) with b 1 ( ) and 1 in fundamental plane using VLBI data, where the dependence is consistent with the re-analysed result on the previous study in \cite{2016ApJ...818..185F} at , however is significantly deviated from the theoretical prediction of accretion flow as the origin of X-ray emission. In contrast to radio-quiet quasars, there is no significant correlation between and Eddington ratio. Our results seem to indicate that the X-ray emission of high-accreting young radio AGNs may be from jet. We constructed the SEDs for 18 sources (most are in radiative efficient accretion) including 9 galaxies and 9 quasars with high-quality X-ray data, and find that the X-ray emission of most quasars is more luminous than that of normal radio-quiet quasars. This is clearly seen from the quasar composite SED, of which the X-ray emission is apparently higher than that of radio-quiet quasars, likely supporting the jet-related X-ray emission in young radio AGNs. The scenario that the X-ray emission is from self-synchrotron Compton (SSC) is discussed.
arXiv comment15 pages,10 figures, 3 tables, accepted for publication in MNRAS
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