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We present a systematic X-ray and multiwavelength study of a sample of 47 active galactic nuclei (AGNs) with reverberation-mapping measurements. This sample includes 21 super-Eddington accreting AGNs and 26 sub-Eddington accreting AGNs. Using high-state observations with simultaneous X-ray and UV/optical measurements, we investigate whether super-Eddington accreting AGNs exhibit different accretion disk-corona connections compared to sub-Eddington accreting AGNs. We find tight correlations between the X-ray-to-UV/optical spectral slope parameter ($alpha_{rm OX}$) and the monochromatic luminosity at $2500~r{A}$ ($L_{rm 2500~r{A}}$) for both the super- and sub-Eddington subsamples. The best-fit $alpha_{rm OX}-L_{rm 2500~r{A}}$ relations are consistent overall, indicating that super-Eddington accreting AGNs are not particularly X-ray weak in general compared to sub-Eddington accreting AGNs. We find dependences of $alpha_{rm OX}$ on both the Eddington ratio ($L_{rm Bol}/L_{rm Edd}$) and black hole mass ($M_{rm BH}$) parameters for our full sample. A multi-variate linear regression analysis yields $alpha_{rm OX}=-0.13 {rm log}(L_{rm Bol}/L_{rm Edd})-0.10 {rm log}M_{rm BH}-0.69$, with a scatter similar to that of the $alpha_{rm OX}-L_{rm 2500~r{A}}$ relation. The hard (rest-frame $>2rm ~keV$) X-ray photon index ($Gamma$) is strongly correlated with $L_{rm Bol}/L_{rm Edd}$ for the full sample and the super-Eddington subsample, but these two parameters are not significantly correlated for the sub-Eddington subsample. A fraction of super-Eddington accreting AGNs show strong X-ray variability, probably due to small-scale gas absorption, and we highlight the importance of employing high-state (intrinsic) X-ray radiation to study the accretion disk-corona connections in AGNs.
The physical properties of the accretion flow and of the X-ray emitting plasma, in supermassive black holes accreting at extreme Eddington rates, are still very unclear. Here we present the analysis of simultaneous XMM-Newton and NuSTAR observations
Disks of gas accreting onto supermassive black holes are thought to power active galactic nuclei (AGN). Stars may form in gravitationally unstable regions of these disks, or may be captured from nuclear star clusters. Because of the dense gas environ
Warm coronae, thick ($tau_{mathrm{T}}approx 10$-$20$, where $tau_{mathrm{T}}$ is the Thomson depth) Comptonizing regions with temperatures of $sim 1$ keV, are proposed to exist at the surfaces of accretion discs in active galactic nuclei (AGNs). By c
Super-Eddington mass accretion has been suggested as an efficient mechanism to grow supermassive black holes (SMBHs). We investigate the imprint left by the radiative efficiency of the super-Eddington accretion process on the clustering of quasars us
We present results from the fitting of infrared (IR) spectral energy distributions of 21 active galactic nuclei (AGN) with clumpy torus models. We compiled high spatial resolution ($sim 0.3$--$0.7$ arcsec) mid-IR $N$-band spectroscopy, $Q$-band imagi