Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.
The tight relation between X-ray and ultraviolet luminosity of quasars
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abstract
The observed relation between the soft X-ray and the optical-ultraviolet emission in active galactic nuclei (AGN) is non-linear and it is usually parametrized as a dependence between the logarithm of the monochromatic luminosity at 2500 {\AA} and at 2 keV. Previous investigations have found that the dispersion of this relation is rather high (~0.35-0.4 in log units), which may be caused by measurement uncertainties, variability, and intrinsic dispersion due to differences in the AGN physical properties (e.g. different accretion modes). We show that, once optically-selected quasars with homogeneous SED and X-ray detection are selected, and dust reddened and/or gas obscured objects are not included, the measured dispersion drops to significantly lower values (i.e. ~0.21-0.24 dex). We show that the residual dispersion is due to some extent to variability, and to remaining measurement uncertainties. Therefore, the real physical intrinsic dispersion should be <0.21 dex. Such a tight relation, valid over 4 decades in luminosity, must be the manifestation of an intrinsic (and universal) physical relation between the disk, emitting the primary radiation, and the hot electron corona emitting X-rays.
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JWST prism spectroscopy of 200 massive galaxies at z~3-15 shows normal star-forming galaxies dominate at z>6 while dusty systems and quiescent galaxies increase at lower redshift, with evidence for multiple quenching pathways.
Intrinsic dispersion in the quasar UV/X-ray luminosity relation decreases with redshift above z~1.6 and modeling it as redshift-dependent shifts Omega_m0 by ~0.025 in flat LambdaCDM.
Galaxy cluster observations yield two preferred directions with cosmic anisotropy amplitude of about 5.3 times 10 to the minus 4 at roughly 1 sigma overall significance, though higher in the XMM-Newton subsample.
Higher Eddington ratio AGN exhibit increased [O III] outflow incidence and reduced obscuration, supporting radiative feedback as the regulator.
Quasar X-ray/UV luminosity relation shows non-linear redshift dependence that cannot be fixed by linear correction and requires further modeling or data screening for cosmological use.
Expanding HST observations of intermediate-redshift quasars can deliver the first systematic rest-frame EUV census of QSOs and warm-hot gas in the CGM/IGM as a low-redshift anchor for future UV missions.
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Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes
Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.