Cosmological evolution of gas and supermassive black holes in idealized isolated halos

Abstract

We study the evolution of baryonic gas in cosmologically growing dark matter halos. To accurately model both the inner and outer regions of the halos, we use a dark matter density profile that transitions smoothly from the NFW profile within the virial radius to a more realistic flat profile far beyond the halo. We construct a dark matter gravitational potential consistent with this density profile, and we use a "cosmological" potential that accounts for gas evolution consistent with Hubble expansion at large radii. Gas is initialized with a density $\approx$ 0.2 times the dark matter density, consistent with the universal baryon fraction ${\rho }_{\mathrm{g}}/({\rho }_{\mathrm{g}}+{\rho }_{\mathrm{DM}})\approx 0.17$. We study the formation of the virial shock and evolution of the baryon fraction, including the effects of radiative cooling and AGN jet feedback. The feedback is powered by the accretion of cold gas onto a central supermassive black hole (SMBH). The cores of the halo exhibit heating and cooling cycles, whose strength and duration depend on the feedback efficiency and the halo mass. The central SMBH initially grows exponentially with time in the early quasar phase, but the growth slows down at later times. The baryon fraction in the core decreases with increasing feedback efficiency and decreasing halo mass. While the halo outskirts evolve self-similarly, the core density is non-evolving, in agreement with cluster observations. We analyze the correlations between the properties of the gas and the central SMBH, and explore the existence of a fundamental plane.

18 pages, 19 figures; this is the MNRAS accepted version of the paper. The codes associated with the paper are available at https://github.com/shashankd98/Semi_Cosmo

References in corpus (24)

• Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology
• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• PLUTO: a Numerical Code for Computational Astrophysics
• A Semi-Analytic Model for the Co-evolution of Galaxies, Black Holes, and Active Galactic Nuclei
• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• A unified model for AGN feedback in cosmological simulations of structure formation
• Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations
• Cosmological Simulations of Intergalactic Medium Enrichment from Galactic Outflows
• A census of baryons in the Universe from localized fast radio bursts
• Direct cosmological simulations of the growth of black holes and galaxies
• Rotation-Dependent Catastrophic Disruption of Gravitational Aggregates
• Unification of the Fundamental Plane and Super-Massive Black Holes Masses
• How AGN Jets Heat the Intracluster Medium -- Insights from Hydrodynamic Simulations
• The baryon fraction of LambdaCDM haloes
• AGN self-regulation in cooling flow clusters
• Molecular Gas in the X-ray Bright Group NGC 5044 as Revealed by ALMA
• Cooling flow solutions for the circumgalactic medium
• ALMA observations of massive molecular gas filaments encasing radio bubbles in the Phoenix cluster
• Supermassive black holes as the regulators of star formation in central galaxies
• Coming of Age in the Dark Sector: How Dark Matter Haloes grow their Gravitational Potential Wells
• The Need for Speed: Escape velocity and dynamical mass measurements of the Andromeda galaxy
• Hot Extended Galaxy Halos Around Local L* Galaxies From Sunyaev-Zeldovich Measurements
• Host galaxies of high-redshift quasars: supermassive black hole growth and feedback
• A shock near the virial radius of the Perseus Cluster