The AGN Optical Variability Fundamental Plane
arXiv · Astrophysics of Galaxies（2025）
Abstract
We investigate the relationship between AGN optical variability timescales, amplitudes, and supermassive black hole (SMBH) masses using homogeneous light curves from the All-Sky Automated Survey for SuperNovae (ASAS-SN). We fit a damped random walk (DRW) model to high-cadence, long-baseline ASAS-SN light curves to estimate the characteristic variability timescale (τ_DRW) and amplitude (σ) for 57 AGN with precise SMBH mass measurements from reverberation mapping and dynamical methods. We confirm a significant correlation between τ_DRW and SMBH mass, and find: log_10(M_BH/ M_⊙) = (1.85±0.20)×log_10 (τ_DRW/200 days)+7.59±0.08. Incorporating σ̂^2 = 2σ^2/τ_DRW in a plane model significantly improves residuals, and we find: log_10(M_BH/ M_⊙) = (2.27±0.20)×log_10 (τ_DRW/200 days)+(1.20±0.20)×log_10(σ̂/1 mJy/days^1/2)+7.68±0.08 with a scatter of 0.39 dex. We calculate τ_DRW, σ̂, and estimate SMBH masses for 203 bright (V<16 mag) AGN from the Milliquas catalog and compare these estimates with measurements from the BAT AGN Spectroscopic Survey for 42 overlapping AGN. In 10 years, LSST could extend this method to survey 7≲log_10(M_BH/M_⊙)≲9 SMBHs out to z∼1 and log_10(M_BH/M_⊙)∼8.0 out to z∼4, and ASAS-SN could probe 5≲log_10(M_BH/M_⊙)≲10.5 SMBHs in the local universe and log_10(M_BH/M_⊙)∼9.0 out to z∼2. Measuring AGN variability with these datasets will provide a unique probe of SMBH evolution by making estimates of M_BH spanning several orders of magnitude with photometric observations alone.
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