Optical QPOs with 550 day periodicity in the reverberation mapped broad line quasar PG 1411+442

TL;DR

This study reports a 550-day optical quasi-periodic oscillation in quasar PG 1411+442, supporting the candidate of a sub-pc binary black hole system, confirmed through multiple analysis methods and statistical confidence levels.

Contribution

It demonstrates the detection of stable optical QPOs in a broad line quasar and discusses implications for identifying binary black hole systems using broad emission line profiles.

Findings

550-day optical QPO confirmed with >5σ confidence

QPO not related to intrinsic AGN variability with >3.5σ confidence

Disk and jet precession are unlikely causes

Abstract

In this manuscript, optical quasi-periodic oscillations (QPOs) with 550 day periodicity related to a candidate of sub-pc binary black hole (BBH) system are reported in the reverberation mapped broad line quasar PG 1411+442 but with different line profile of broad H$\alpha$ from that of broad H$\beta$ in its rms spectrum. First, considering sine function to describe the 18.8years-long light curves from the CSS, ASAS-SN and ZTF, 550days periodicity can be confirmed with confidence level higher than 5$\sigma$. Second, the stable 550days optical QPOs can be re-confirmed with confidence levels higher than 5$\sigma$ by the Generalized Lomb-Scargle periodogram, the sine-like phase-folded light curves and the WWZ technique determined power maps. Third, based on simulated light curves by CAR process, confidence level higher than $3.5\sigma$ can be confirmed for the optical QPOs not related to intrinsic AGN variability. Moreover, considering spatial separation of central two BH accreting systems smaller than expected sizes of broad emission line regions (BLRs), central total BH mass higher than $10^6{\rm M_\odot}$ could lead to few effects of supposed BBH systems on estimated virial BH masses. Meanwhile, disk precession is not preferred due to the similar estimated sizes of optical and NUV emission regions, and jet precession can be ruled out due to PG 1411+442 as a radio quiet quasar. The results strongly indicate it would be practicable by applying very different line profiles of broad Balmer emission lines to detect candidates of BBH systems in normal broad line AGN in the near future.