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The nearby dwarf galaxy POX 52 at $z = 0.021$ hosts an active galacticnucleus (AGN) with a black-hole (BH) mass of $M_{\rm BH} \sim 10^{5-6} M_\odot$and an Eddington ratio of $\sim$ 0.1-1. This object provides the rareopportunity to study both AGN and host-galaxy properties in a low-mass highlyaccreting system. To do so, we collected its multi-wavelength data from X-rayto radio. First, we construct a spectral energy distribution, and by fitting itwith AGN and host-galaxy components, we constrain AGN-disk and dust-toruscomponents. Then, while considering the AGN-disk emission, we decompose opticalHST images. As a result, it is found that a classical bulge component isprobably present, and its mass ($M_{\rm bulge}$) is consistent with an expectedvalue from a local relation. Lastly, we analyze new quasi-simultaneous X-ray(0.2-30 keV) data obtained by NuSTAR and XMM-Newton. The X-ray spectrum can bereproduced by multi-color blackbody, warm and hot coronae, and disk and torusreflection components. Based on this, the spin is estimated to be $a_{\rm spin}= 0.998_{-0.814}$, which could suggest that most of the current BH mass wasachieved by prolonged mass accretion. Given the presence of the bulge, POX 52would have undergone a galaxy merger, while the $M_{\rm BH}$-$M_{\rm bulge}$relation and the inferred prolonged accretion could suggest that AGN feedbackoccurred. Regarding the AGN structure, the spectral slope of the hot corona,its relative strength to the bolometric emission, and the torus structure arefound to be consistent with Eddington-ratio dependencies found for nearby AGNs.

Co-evolution and Nuclear Structure in the Dwarf Galaxy POX 52 Studied by Multi-wavelength Data From Radio to X-ray