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Approximately 10-20% of Active Galactic Nuclei are known to eject powerfuljets from the innermost regions. There is very little observational evidence ifthe jets are powered by spinning black holes and if the accretion disks extendto the innermost regions in radio-loud AGN. Here we study the soft X-rayexcess, the hard X-ray spectrum and the optical/UV emission from the radio-loudnarrow-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 excessemission below 2 keV that is well described by a blackbody (kTe ~ 0.13 keV) andhigh energy emission that is well described by a thermal Comptonisation(compps) model with kTe ~ 250 keV, optical depth {\tau} ~ 0.05 (sphericalcorona) or kTe ~ 90 keV, {\tau} ~ 0.5 (slab corona). The Comptonising corona inPKS 0558-504 is likely hotter than in radio-quiet Seyferts such as IC 4329A andSwift J2127.4+5654. The observed soft X-ray excess can be modelled as blurredreflection from an ionised accretion disk or optically thick thermalComptonisation in a low temperature plasma. Both the soft X-ray excess emissionwhen interpreted as the blurred reflection and the optical/UV to soft X-rayemission interpreted as intrinsic disk Comptonised emission implies spinning (a> 0.6) black hole. These results suggest that disk truncation at large radiiand retrograde black hole spin both are unlikely to be the necessary conditionsfor launching the jets.

Accretion disk/corona emission from a radio-loud narrow line Seyfert 1 galaxy PKS 0558-504