Influence of Comptonization region over the ambiance of accretion disc in Active Galactic Nucleus

TL;DR

This study investigates the relationships between X-ray, infrared, and emission line properties in AGNs, revealing correlations and break points that shed light on the interaction between the Comptonization region and accretion disc structures.

Contribution

The paper provides new correlation analyses between X-ray, infrared, and emission line parameters in AGNs, identifying break points related to black hole mass and emission line widths.

Findings

X-ray luminosity correlates linearly with broad Balmer line components.

Strong dependency observed between X-ray and mid-infrared luminosities.

Break points identified in correlations involving black hole mass and emission line widths.

Abstract

Understanding the radiative and physical structures of inner region of a few 100 pc of AGNs is important to constrain the causes of their activities. Although the X-ray emission from the Comptonization region/corona and the accretion disc regulates the broad line emission regions and torus structures, the exact mutual dependency is not understood well. We performed correlation studies for X-ray, mid-infrared, and different components of Balmer emission lines for the selected sample of AGNs. Almost 10 different parameters and their inter-dependencies were explored in order to understand the underlying astrophysics. We found that the X-ray luminosity has a linear dependency on the various components of broad Balmer emission lines (e.g. L$_{\text{2-10 keV}}$ $\propto$ L$^{0.78}_{\text{H}\beta^{\text{B}}}$) and found a strong dependency on the optical continuum luminosity (L$_{\text{2-10 keV}}$ $\propto$ L$^{0.86}_{5100\,\text{\AA}}$). For a selected sample, we also observed a linear dependency between X-ray and mid-infrared luminosity (L$_{\text{2-10 keV}}$ $\propto$ L$^{0.74}_{6\,\upmu \text{m}}$). A break point was observed in our correlation studies for X-ray power-law index, $\Gamma$, and mass of black hole at $\sim$ log (M/M$_{\odot}$) = 8.95. Similarly the relations between $\Gamma$ and FWHM of H$\alpha$ and H$\beta$ broad components show breaks at FWHM$_{\text{H}\alpha}$= 7642$\pm$657 km s$^{-1}$ and FWHM$_{\text{H}\beta}$ = 7336$\pm$650 km s$^{-1}$. However, more data are required to confine the breaks locations exactly. We noted that $\Gamma$ and Eddington ratios are negatively correlated to Balmer decrements in our selected sample. We analyzed and discussed about the implications of new findings in terms of interaction AGN structures.