BASS. XLIX. Characterization of highly luminous and obscured AGNs: local X-ray and [NeV]$\lambda$3426 emission in comparison with the high-redshift Universe

Abstract

We present a detailed analysis of the most luminous and obscured Active Galactic Nuclei (AGNs) detected in the ultra-hard X-ray band (14-195 keV) by Swift/BAT. Our sample comprises 21 X-ray luminous (log $L_X/\mathrm{erg}{\mathrm{s}}^{-1}>44.6$, 2-10 keV) AGNs at $z<0.6$, optically classified as Seyfert 1.9-2. Using NuSTAR, XMM-Newton, Suzaku, and Chandra, we constrain AGN properties such as absorption column density $N_H$, photon index $\Gamma$, intrinsic $L_X$, covering factor, and iron K$\alpha$ equivalent width. For sources with black hole mass estimates (12/20), we find a weak correlation between $\Gamma$ and Eddington ratio (${\lambda }_{Edd}$). Of these, six ($50\pm 13\%$) lie in the $N_H$-${\lambda }_{Edd}$ "forbidden region'' and exhibit a combined higher prevalence of $N_H$ variability and outflow signatures, suggesting a transitional phase where AGN feedback may be clearing the obscuring material. For the 13/21 sources with multi-epoch X-ray spectra, $82_{-16}^{+6}\%$ exhibit variability in either 2-10 keV flux ($73_{-16}^{+9}\%$) or line-of-sight $N_H$ ($33_{-10}^{+15}\%$). For the 20/21 sources with available near-UV/optical spectroscopy, we detect [NeV]$\lambda$3426 in 17 ($85_{-11}^{+5}\%$), confirming its reliability to probe AGN emission even in heavily obscured systems. When normalized to the same [OIII]$\lambda$5007 peak flux as $z=2$-$9$ narrow-line AGNs identified with JWST, our sample exhibits significantly stronger [NeV]$\lambda$3426 emission, suggesting that high-redshift obscured AGNs may be intrinsically weaker in [NeV]$\lambda$3426 or that [NeV]$\lambda$3426 is more challenging to detect in those environments. The sources presented here serve as a benchmark for high-redshift analogs, showing the potential of [NeV]$\lambda$3426 to reveal obscured AGNs and the need for future missions to expand X-ray studies into the high-redshift Universe.

arXiv commentAccepted for publication in ApJ

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