Exploring possible relations between optical variability time scales and broad emission line shapes in AGN

TL;DR

This study links optical variability time scales in AGN to broad emission line shapes, proposing a model that connects these features to the SMBH mass through orbital time scales, offering a new perspective on AGN variability.

Contribution

Introduces a novel model connecting broad emission line profiles with optical variability time scales to estimate SMBH masses in AGN.

Findings

Black hole mass estimates agree with other methods.

Variability time scales are linked to orbital periods, not stochastic processes.

The model provides a new way to interpret AGN variability data.

Abstract

Here we investigate the connection of broad emission line shapes and continuum light curve variability time scales of type-1 Active Galactic Nuclei (AGN). We developed a new model to describe optical broad emission lines as an accretion disk model of a line profile with additional ring emission. We connect ring radii with orbital time scales derived from optical light curves, and using Kepler's third law, we calculate mass of central supermassive black hole (SMBH). The obtained results for central black hole masses are in a good agreement with {other methods. This indicates that the variability time scales of AGN may not be stochastic, but rather connected to the orbital time scales which depend on the central SMBH mass.