The evolution of galaxies, clusters, and AGN in the BAHAMAS - - PowerPoint PPT Presentation

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the evolution of galaxies clusters and agn in the bahamas
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The evolution of galaxies, clusters, and AGN in the BAHAMAS - - PowerPoint PPT Presentation

Nov 16, 2022 293 likes •533 views

The evolution of galaxies, clusters, and AGN in the BAHAMAS simulations Ian G. McCarthy Liverpool JMU Collaborators: Joop Schaye (Leiden) Simeon Bird (Johns Hopkins) Amandine Le Brun (CEA Saclay) IGM+2011 Role of hydro simulations Allows

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The evolution of galaxies, clusters, and AGN in the BAHAMAS simulations

Ian G. McCarthy Liverpool JMU

Collaborators: Joop Schaye (Leiden) Simeon Bird (Johns Hopkins) Amandine Le Brun (CEA Saclay)

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Role of hydro simulations

  • Allows one to make self-consistent predictions for galaxies,

gas, total matter.

  • Can make synthetic observations useful for testing
  • bservational methods and simple models.

BUT!:

Our trust of sims linked to their realism. Finite resolution limits us to simplified treatments of important processes that occur on small scales. Simulations cannot robustly predict stellar or gas content of dark matter haloes CALIBRATION IGM+2011

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BAHAMAS: BAryons and HAloes of MAssive Systems

First hydro simulations to reproduce the observed baryon content of collapsed

  • structures. Realistically captures suppression of matter power spectrum.

Distribution of stellar masses Hot gas masses

IGM+2016, MNRAS

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Stellar mass fractions: centrals and satellites

Reproduces SHAM and HOD modelling results fairly well.

fstar-M200 for centrals cents vs. sats: fstar,tot

IGM+2016, MNRAS

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Spatial distribution of stellar mass

Stellar density profile: clusters Stellar mass autocorrelation function IGM+2016, MNRAS

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X-ray scaling relations

Simulations processed through synthetic X-ray pipeline. Comparison to local X-ray-selected

  • systems. Simulations reproduce Lx-M500 and Yx-M500 relations automatically.

LX-M500 YX-M500

IGM+2016, MNRAS

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SZ scaling relations

Compute SZ fluxes in an observational manner (within correct aperture; stacking in bins of stellar mass in right panel). Simulations reproduce well.

SZ-M500 SZ-Mstar

IGM+2016, MNRAS

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Spatial distribution of hot gas in clusters

Also reproduce the detailed thermodynamic profiles over a wide range of radii and halo masses.

Gas density

IGM+2016, MNRAS

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Evolution of galaxies

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Evolution of cosmic stellar mass density

IGM+2016, MNRAS

  • Broadly reproduces data

when using

  • bservationally-

motivated aperture

  • Diffuse light becomes

important at late times

  • Completeness an issue

for observations at z≈2

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Evolution of galaxy stellar mass function

IGM+2016, MNRAS Qualitatively agrees with observed evolution (Muzzin+2013). Low-mass galaxies are

  • verabundant (stellar masses too high), due to resolution. Slight underestimate of masses of

most-massive galaxies at z > 2.

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Evolution of cosmic SFR density

IGM+2016, MNRAS

  • Qualitatively sensible, but
  • verpredicts late-time SFRd

and slightly underpredicts peak.

  • Similar level of agreement

as EAGLE.

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Evolution of sSFR-stellar mass relation

IGM+2016, MNRAS

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Evolution of clusters

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Evolution of abundance of clusters

Mummery+2016, in prep

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Aside: A better way to do cluster counts?

Velocity dispersion function (NFOF > 5) Velocity dispersion counts (NFOF > 5, σv > 300 km/s) Caldwell, IGM, et al. 2016, MNRAS

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Evolution of hot gas scaling relations

Barnes+2016, MNRAS Mgas-M500 TX-M500 YX-M500 LX-M500

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Evolution of hot gas profiles

Barnes+2016, MNRAS Pressure profiles Gas density profiles

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Dynamics of satellite systems

Caldwell+2016, MNRAS IGM+2016, MNRAS

  • Satellites evolve self-similarly.
  • But have negative velocity bias with respect

to DM.

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Evolution of AGN

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Quasar luminosity function

IGM+2016, MNRAS

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Summary

  • BAHAMAS is a first attempt to bring the calibration philosophy to larger systems, with

particular emphasis on large-scale structure cosmology applications.

  • Calibration is done at z=0 on the GSMF and the gas fractions of groups and clusters. A

very simple physical model. No examination of evolution during calibration.

  • We have 12 different 400 h-1 Mpc boxes with different cosmologies. Light cones with

synthetic X-ray, SZ, cosmic shear, CMB lensing maps and corresponding galaxy and cluster catalogs are already complete. Cross-correlations with galaxies?

  • BAHAMAS qualitatively recovers observed evolution of massive galaxies and groups and

clusters, even though its aim was mainly focused on LSS applications. There are differences in detail (especially SFR evolution), which an be used to be further constrain feedback model (and/or higher resolution required).

  • Hot gas properties of clusters, and especially groups, do not scale self-similarly in general

(see Amandine’s talk next). But the dynamics of satellite population do.

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Title