We present a radio and X-ray study of PKS 1353–341 , the brightest cluster galaxy radio source at the center of a recent Chandra -discovered X-ray cluster .
Our multi-frequency VLA images reveal an edge-brightened ( FR-II ) , double-lobed structure with total \sim 50 kpc extent and 1.5 GHz power of 1.2 \times 10 ^ { 25 } W Hz ^ { -1 } , separated from the bright , arcsecond-scale core .
We reanalyzed the Chandra data and found the X-ray emitting AGN is offset by \sim 9 kpc from a compact X-ray cool-core with temperature , kT = 3.1 \pm 0.5 keV , and a radius of \sim 22 kpc , surrounded by a hotter kT = 6.3 \pm 0.7 keV gas out to \sim 50 kpc .
The offset suggests sloshing inside the cool-core induced by a minor merger or a past outburst of the AGN that produced the large-scale radio lobes .
The comparable spatial scales of the lobes with the interface between the different temperature X-ray plasma indicate the lobes are actively heating the outer layers of what is now a remnant compact cool-core .
Our dual-frequency VLBA images reveal substructure in the central radio source , consisting of a radio core with double-sided pc-scale jets pointing toward the kpc-scale structures .
The northern jet is detected only at 8.4 GHz , indicating its emission is behind an absorbing torus or disk .
We also measured faster apparent motions in the southern jet up to 1.9 \pm 1.1 c than in the northern jet ( 0.8 \pm 0.5 c ) .
While the VLBA observations indicate the southern jet is aligned slightly closer to our line of sight , the asymmetries are overall modest and imply minimal projection effects in the large-scale radio structures .