We have identified a large ( \approx 200 h _ { 75 } ^ { -1 } kpc ) , powerful double radio source whose host galaxy is clearly a disk and most likely a spiral .
This FR I-like radio galaxy is located very near the center of the Richness Class 0 cluster Abell 428 .
The existence of such an object violates a fundamental paradigm for radio loud AGN ’ s .
In paper I ( Ledlow , Owen , & Keel,1998 , ApJ,495,227 ) , we showed that this object was most consistent with a spiral host classification with optical emission-line ratios and colors suggestive of an active nucleus .
However , we were not able to confirm actual radio jet emission based on the maps available at that time .
In this paper , we present new , higher resolution radio imaging , a radio/mm continuum spectrum for the nucleus , a detection of HI absorption against the bright radio core , an upper-limit to CO emission and the gas mass , and 70 ( 68 new ) optical redshifts measured in the direction of Abell 428 .
We confirm the existence of a radio jet at 20cm , extending 42 h _ { 75 } ^ { -1 } into the southern lobe .
At 3.6cm , we also detect a nuclear jet similar in length to that in M87 , although 10 times weaker .
We believe that this is the first detection of a radio jet on these scales in a disk/spiral host galaxy .
The nuclear radio spectrum is similar to many blazar or QSO like objects , suggesting that the galaxy harbors an imbedded and obscured AGN .
We model a turnover in the spectrum at low frequencies as a result of Free-Free absorption .
We detect very strong and narrow HI absorption , with nearly the entire 20 cm continuum flux of the core being absorbed , implying an unusually large optical depth ( \tau \approx 1 ) .
The most consistent model is that we are viewing the nucleus through a disk-like distribution of gas in the ISM , possibly through a spiral arm or a warp to account for the above average column density .
From the radial velocity distribution , we find that Abell 428 is in fact made up of at least 2 clumps of galaxies separated by \sim 3300 km sec ^ { -1 } , which themselves appear to be imbedded in a nearly continuous distribution of galaxies over 13000 km sec ^ { -1 } in velocity space .
Thus , the environment around this unusual radio source is more like that of a poor galaxy group imbedded in a filament-like structure viewed end-on .