On the Mass Loading of AGN-driven Outflows in Elliptical Galaxies and Clusters

• Published in: The Astrophysical journal 2021-12, Vol.923 (2), p.256
• Main Authors: Qiu, Yu, McNamara, Brian R., Bogdanović, Tamara, Inayoshi, Kohei, Ho, Luis C.
• Format: Article
• Language: English
• Subjects: Accretion disks; Active galactic nuclei; Astrophysics; Black holes; Cold gas; Cooling flows; Deceleration; Deposition; Elliptical galaxies; Galactic clusters; Intracluster medium; Jets; Outflow; Parameters; Perseus Cluster; Stars & galaxies; Supermassive black holes; Thermal simulation; Velocity distribution; Virgo Cluster; X-ray astronomy
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac2ede

Outflows driven by active galactic nuclei (AGNs) are an important channel for accreting supermassive black holes (SMBHs) to interact with their host galaxies and clusters. Properties of the outflows are however poorly constrained due to the lack of kinetically resolved data of the hot plasma that permeates the circumgalactic and intracluster space. In this work, we use a single parameter, outflow-to-accretion mass-loading factor m = M ̇ jet / M ̇ BH , to characterize the outflows that mediate the interaction between SMBHs and their hosts. By modeling both M87 and Perseus, and comparing the simulated thermal profiles with the X-ray observations of these two systems, we demonstrate that m can be constrained between 200 and 500. This parameter corresponds to a bulk flow speed between 4000 and 7000 km s −1 at around 1 kpc, and a thermalized outflow temperature between 10 8.7 and 10 9 K. Our results indicate that the dominant outflow speeds in giant elliptical galaxies and clusters are much lower than in the close vicinity of the SMBH, signaling an efficient coupling with and deceleration by the surrounding medium on length scales below 1 kpc. Consequently, AGNs may be efficient at launching outflows ∼10 times more massive than previously uncovered by measurements of cold, obscuring material. We also examine the mass and velocity distribution of the cold gas, which ultimately forms a rotationally supported disk in simulated clusters. The rarity of such disks in observations indicates that further investigations are needed to understand the evolution of the cold gas after it forms.