摘要：Detecting and modeling the reprocessed hard X-ray emission component in the accretion flow, the so-called reflection spectrum, is a main tool used to estimate black hole spins in a wide range of astrophysical black holes, regardless of their mass or distance. In this work, we study the X-ray spectra of the Seyfert I galaxy III Zw 2 by using multiepochXMM-Newton,NuSTAR, andSuzakuobservations. The X-ray spectra exhibit a soft-excess below 1 keV and a prominent excess at the location of the broad Fe Kαline at 6.4 keV. To account for these spectral features, we fit the spectra with multiple models including an ionized partially covering absorber and an accretion disk reflection model. To fully resolve the reflection component, we analyzed jointly theXMM-NewtonandNuSTARobservations taken in 2017 and archivalXMM-Newtondata from 2000. Assuming the reflection scenario, the resulting model fits support for a rapidly spinning black hole (a≥ 0.98) in this radio-intermediate source. The X-ray spectra in 2000 and 2017 are remarkably similar; the only difference pertains to the reflection fraction, which is possibly due to a change in the geometry of the accretion flow. However, theSuzakuobservation is markedly different, and we suggest this could be an effect of a jet contribution in the X-ray band, which is supported by the elevated radio flux during this observation.
关键词：enaccretionaccretion disksblack hole physicsX-rays: galaxiesgalaxies: Seyfertgalaxies: active
