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SUMMARY:The Formation and Co-Evolution of Galaxies and Supermassive Black 
 Holes - Yohan Dubois (Institut d’Astrophysique de Paris)
DTSTART:20250605T150000Z
DTEND:20250605T160000Z
UID:TALK233023@talks.cam.ac.uk
CONTACT:Matthew Grayling
DESCRIPTION:Cosmological hydrodynamical simulations are becoming increasin
 gly realistic by incorporating a wider range of physical processes\, highe
 r spatial resolution\, and larger statistical samples. Despite ongoing tra
 de-offs between resolution and volume\, recent advances now allow for simu
 lations that resolve the multiphase interstellar medium and capture the cl
 umpy nature of star formation in galaxies. In this context\, I will presen
 t how such simulations shed light on the coupled evolution of galaxies and
  their central supermassive black holes. At high redshift\, galaxies tend 
 to be gas-rich\, turbulent\, and star-bursting\, often exhibiting irregula
 r\, compact\, and disturbed morphologies. As internal turbulence subsides\
 , many systems transition into stable\, rotating disc galaxies\, typically
  once they reach stellar masses around 1e10 Msun. Simultaneously\, black h
 ole growth is tightly linked to the dynamical state of the host galaxy. In
  low-mass\, turbulent systems\, stellar feedback can suppress nuclear gas 
 inflows\, delaying black hole growth. Only when galaxies become sufficient
 ly massive and dynamically settled can gas efficiently reach galactic cent
 ers to fuel sustained accretion. These processes also have important impli
 cations for the spin evolution of black holes or how fast they coalesce\, 
 which can reflect the varying modes of accretion and feedback across cosmi
 c time.
LOCATION:Hoyle Lecture Theatre\, Institute of Astronomy
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