Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk

We present damped harmonic oscillator (DHO) light-curve modeling for a sample of 12,714 spectroscopically confirmed quasars in the Sloan Digital Sky Survey Stripe 82 region. DHO is second-order continuous-time autoregressive moving-average (CARMA) process, which can be fully described using four independent parameters: natural oscillation frequency ($\omega_{0}$), damping ratio ($\xi$), characteristic perturbation timescale ($\tau_{\mathrm{perturb}}$), and an amplitude perturbing white noise ($\sigma_{\mathrm{\epsilon}}$). The asymptotic variability process quantified by $\sigma_{\mathrm{DHO}}$ -- function $\omega_{0}$, $\xi$, $\tau_{\mathrm{perturb}}$, $\sigma_{\mathrm{\epsilon}}$. find that both $\tau_{\mathrm{perturb}}$ $\sigma_{\mathrm{\epsilon}}$ follow different dependencies with rest-frame wavelength ($\lambda_{\mathrm{RF}}$) on either side 2500 \AA, whereas follows single power-law relation $\lambda_{\mathrm{RF}}$. After correcting dependence, exhibits anti-correlations Eddington black hole mass, while typical value days shows anti-correlation bolometric luminosity. Modeling AGN as offers more insight into workings accretion disks close to supermassive holes (SMBHs) at center AGN. newly discovered short-term (characterized $\sigma_{\mathrm{\epsilon}}$) its correlation luminosity pave way new algorithms will derive fundamental properties (e.g., ratio) photometric data alone.