Approximately 10 - 20 \% of Active Galactic Nuclei are known to eject powerful jets from the innermost regions .
There is very little observational evidence if the jets are powered by spinning black holes and if the accretion disks extend to the innermost regions in radio-loud AGN .
Here we study the soft X-ray excess , the hard X-ray spectrum and the optical/UV emission from the radio-loud narrow-line Seyfert 1 galaxy PKS 0558–504 using Suzaku and Swift observations.The broadband X-ray continuum of PKS 0558–504 consists of a soft X-ray excess emission below 2 { keV } that is well described by a blackbody ( kT \sim 0.13 { keV } ) and high energy emission that is well described by a thermal Comptonisation ( compps ) model with kT _ { e } \sim 250 { keV } , optical depth \tau \sim 0.05 ( spherical corona ) or kT _ { e } \sim 90 { keV } , \tau \sim 0.5 ( slab corona ) .
The Comptonising corona in PKS 0558–504 is likely hotter than in radio-quiet Seyferts such as IC 4329A and Swift J2127.4+5654 .
The observed soft X-ray excess can be modeled as blurred reflection from an ionised accretion disk or optically thick thermal Comptonisation in a low temperature plasma .
Both the soft X-ray excess emission when interpreted as the blurred reflection and the optical/UV to soft X-ray emission interpreted as intrinsic disk Comptonised emission implies spinning ( a > 0.6 ) black hole .
These results suggest that disk truncation at large radii and retrograde black hole spin both are unlikely to be the necessary conditions for launching the jets .