First direct dynamical detection of a dual supermassive black hole system at sub-kiloparsec separation

TL;DR

This paper reports the first direct dynamical detection of a dual supermassive black hole system at less than a kiloparsec separation in NGC7727, confirming the existence of such systems through high-resolution stellar kinematics.

Contribution

It provides the first dynamical confirmation of a dual SMBH system with sub-kiloparsec separation, using advanced integral-field spectroscopy and modeling techniques.

Findings

Detected SMBH in Nucleus 1 with mass ~1.54×10^8 M☉

Detected SMBH in Nucleus 2 with mass ~6.33×10^6 M☉

Nucleus 2's SMBH is over-massive relative to scaling relations

Abstract

We investigated whether the two recently discovered nuclei in NGC7727 both host a super-massive black hole (SMBH). We used the high spatial resolution mode of the integral-field spectrograph MUSE on the VLT in adaptive optics mode to resolve the stellar kinematics within the sphere of influence of both putative black holes. We combined the kinematic data with an HST-based mass model and used Jeans models to measure their SMBH mass. We report the discovery of a dual SMBH system in NGC7727. We detect a SMBH in the photometric center of the galaxy in Nucleus 1, with a mass of $M_{\rm SMBH}=1.54^{+0.18}_{-0.15} \times10^{8}M_{\odot}$. In the second nucleus, which is 500pc offset from the main nucleus, we also find a clear signal for a SMBH with a mass of $M_{\rm BH}=6.33^{+3.32}_{-1.40}\times10^{6}M_{\odot}$. Both SMBHs are detected at high significance. The off-axis nature of Nucleus 2 makes modeling the system challenging; but a number of robustness tests suggest that a black hole is required to explain the kinematics. The SMBH in the offset Nucleus 2 makes up 3.0% of its total mass, which means its SMBH is over-massive compared to the $M_{\rm BH}-M_{\rm Bulge}$ scaling relation. This confirms it as the surviving nuclear star cluster of a galaxy that has merged with NGC7727. This discovery is the first dynamically confirmed dual SMBH system with a projected separation of less than a kiloparsec and the nearest dynamically confirmed dual SMBH at a distance of 27.4Mpc. The second Nucleus is in an advanced state of inspiral, and it will eventually result in a 1:24 mass ratio SMBH merger. Optical emission lines suggest Nucleus 2 is a Seyfert galaxy, making it a low-luminosity Active Galactic Nuclei (AGN). There are likely many more quiescent SMBHs as well as dual SMBH pairs in the local Universe that have been missed by surveys that focus on bright accretion signatures.