We present a broadband spectral study of the radio-loud narrow-line Seyfert 1 galaxy 1H 0323+342 based on multi-epoch observations performed with NuSTAR on 2014 March 15 , and two simultaneous observations performed with Suzaku and Swift on 2009 July 26 and 2013 March 1 .
We found the presence of a strong soft X-ray excess emission , a broad but weak Fe line and hard X-ray excess emission .
We used the blurred reflection ( relxill ) and the intrinsic disc Comptonization ( optxagnf ) , two physically motivated models , to describe the broadband spectra and to disentangle the disk/corona and jet emission .
The relxill model is mainly constrained by the strong soft X-ray excess although the model failed to predict this excess when fitted above 3 { keV } and extrapolated to lower energies .
The joint spectral analysis of the three datasets above 3 { keV } with this model resulted in a high black hole spin ( a > 0.9 ) and moderate reflection fraction R \sim 0.5 .
The optxagnf model fitted to the two simultaneous datasets resulted in an excess emission in the UV band .
The simultaneous UV-to-hard X-ray spectra of 1H 0323+342 are best described by a model consisting of a primary X-ray power-law continuum with \Gamma \sim 1.8 , a blurred reflection component with R \sim 0.5 , Comptonised disk emission as the soft X-ray excess , optical/UV emission from a standard accretion disk around a black hole of mass \sim 10 ^ { 7 } { M _ { \odot } } and a steep power law ( \Gamma \sim 3 - 3.5 ) component , most likely the jet emission in the UV band .
The fractional RMS variability spectra suggest that both the soft excess and the powerlaw component are variable in nature .