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