A Case for a Binary Black Hole System Revealed via Quasi-Periodic Outflows

Binary black hole systems in close orbits are thought to be the precursors of gravitational wave events and their identification has fundamental implications for our understanding of black hole growth and evolution. However, a gravitationally bound companion orbiting closer than about a milli-parsec to an accreting supermassive black hole (SMBH, mass ≥106 solar masses) in an external galaxy cannot be spatially resolved with present-day instruments. Instead, its detection requires a combination of indirect observational methods and advanced modelling. Here we report the detection of quasi-periodic variability in X-ray spectral features after an outburst from a previously low-luminosity Active Galactic Nucleus (AGN) in a galaxy at redshift z=0.056. We interpret this variability as due to Quasi-Periodic Outflows (QPOuts) from the SMBH. The puzzling phenomenon repeats roughly once every 8.5 days and photo-ionization modeling of the energy spectra implies that the outflowing material moves with a high velocity of about a third of the speed of light. The mass of the central black hole, roughly 30 million solar masses, as derived from the optical broad line--SMBH mass scaling relation, implies that the outflows are launched from a few tens of gravitational radii from the SMBH event horizon. By performing 2D and 3D general relativistic magnetohydrodynamic (GRMHD) simulations and by comparing their results over a broad range of the system parameters we show that these QPOuts can be explained with an orbiting intermediate-mass black hole (IMBH) secondary (mass range of 100--10,000 solar masses) at a distance of about 100 gravitational radii (less than a milli-parsec) from the primary SMBH. Outflows are naturally enhanced when the secondary object punches through the SMBH's inner accretion disc during each orbital period and this is revealed as regular increases in X-ray absorption along our line of sight. The overall optical, UV and X-ray outburst properties indicate that a major accretion episode -- perhaps from a stellar tidal disruption by the SMBH -- could have provided the gas to illuminate the presence of the pre-existing IMBH secondary. Our work highlights the new astrophysical phenomenon of QPOuts and the importance of high cadence X-ray monitoring observations to potentially uncover electromagnetic signatures of such tight binary black hole systems.