An X-Ray Spectral Study of the Origin of Reflection Features in Bare Seyfert 1 Galaxy ESO 511-G030

The reprocessed X-ray emission from active galactic nuclei is an important diagnostic tool to study the dynamics and geometry of the matter surrounding supermassive black holes (SMBHs). We present a broadband (optical-UV to hard X-ray) spectral study of the bare Seyfert 1 galaxy, ESO 511-G030, using multi-epoch Suzaku and XMM-Newton data from 2012 and 2007, respectively. The broadband spectra of ESO 511-G030 exhibit a UV bump, a prominent soft excess below $2\,\mathrm{keV}$ , a relatively broad ( $\sigma =0.08\mbox{--}0.14\,\mathrm{keV}$ ) Fe emission line at $6.4\,\mathrm{keV}$ , and a weak Compton hump at $E\gt 10\,\mathrm{keV}$ . The soft X-ray excess in ESO 511-G030 can be described either as the thermal Comptonization of disk seed photons by a warm ( ${0.40}_{-0.02}^{+0.02}\,\mathrm{keV}$ ), optically thick ( $\tau ={12.7}_{-0.4}^{+0.5}$ ), and compact ( $\lt 15{r}_{{\rm{g}}}$ ) corona or as the blurred reflection from an untruncated and moderate to highly ionized accretion disk. However, for the blurred reflection, the model requires some extreme configuration of the disk and corona. Both these models prefer a rapidly spinning black hole ( $a\gt 0.78$ ) and a compact corona, indicating a relativistic origin of the broad Fe emission line. We found an inner disk temperature of $\sim 2\mbox{--}3\,\mathrm{eV}$ that characterizes the UV bump and the SMBH accretes at a sub-Eddington rate ( ${\lambda }_{\mathrm{Edd}}=0.004\mbox{--}0.008$ ).