2022A&A...658A.152V


Query : 2022A&A...658A.152V

2022A&A...658A.152V - Astronomy and Astrophysics, volume 658A, 152-152 (2022/2-1)

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

VOGGEL K.T., SETH A.C., BAUMGARDT H., HUSEMANN B., NEUMAYER N., HILKER M., PECHETTI R., MIESKE S., DUMONT A. and GEORGIEV I.

Abstract (from CDS):

We investigated whether the two recently discovered nuclei in NGC 7727 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 NGC 7727. We detect a SMBH in the photometric center of the galaxy in Nucleus 1, with a mass of MSMBH = 1.54–0.15+0.18 x 108 M. In the second nucleus, which is 500 pc offset from the main nucleus, we also find a clear signal for a SMBH with a mass of MBH = 6.33–1.40+3.32 x 106 M. Both SMBHs are detected at high significance. The off-axis nature of Nucleus 2 makes modeling the system challenging; however, a number of robustness tests suggest that a black hole is required to explain the observed 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 MBH - MBulge scaling relation. This confirms it as the surviving nuclear star cluster of a galaxy that has merged with NGC 7727. 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 27.4 Mpc. 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. 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.

Abstract Copyright: © K. T. Voggel et al. 2022

Journal keyword(s): galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: active - quasars: supermassive black holes

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 M 96 GiP 10 46 45.744 +11 49 11.78 10.42 10.15 9.25 8.99   ~ 790 1
2 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4321 3
3 NGC 5139 GlC 13 26 47.28 -47 28 46.1           ~ 3299 0
4 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1590 2
5 [SSW2018] NGC 7727 Nucleus 2 PoG 23 39 53.6887676568 -12 17 30.962063364           ~ 6 0
6 [SSW2018] NGC 7727 Nucleus 1 PoG 23 39 53.8038745368 -12 17 34.180069632           ~ 2 0
7 NGC 7727 GiP 23 39 53.870 -12 17 34.84   11   10.55   ~ 168 0

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2023.02.01-21:03:41

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