Effects of Preheating on X-Ray Scaling Relations in Galaxy Clusters

By J. Bialek, August E. Evrard, Joseph J. Mohr. 2000

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The failure of purely gravitational and gasdynamical models of X-ray cluster formation to reproduce basic observed properties of the local cluster population suggests the need for one or more additional physical processes operating on the intracluster medium (ICM). We present results from 84 moderate-resolution gasdynamic simulations designed to investigate systematically the effects of preheating (an early elevated ICM adiabat) on the resultant, local X-ray size-temperature, luminosity-temperature, and ICM mass-temperature relations. Seven sets of 12 simulations are performed for a ΛCDM cosmology, each set characterized by a different initial entropy level Si. The slopes of the observable relations steepen monotonically as Si is increased. Observed slopes for all three relations are reproduced by models with Si ∈ 55-150 keV cm2, levels that compare favorably to empirical determinations of core ICM entropy by Lloyd-Davies, Ponman, & Cannon. The redshift evolution for the case of a locally successful model with Si = 106 keV cm2 is presented. At temperatures kT ≳ 3 keV, little or no evolution in physical isophotal sizes or bolometric luminosities is expected to z ≲ 1. The ICM and total masses at fixed T are lower at higher z, as expected from the virial theorem. ICM mass fractions show a mild T dependence. Clusters with kT ≲ 3 keV contain ICM mass fractions depressed by modest amounts (≲25%) below the cosmic mean baryon fraction Ωb/Ωm; hot clusters subject to preheating remain good tracers of the cosmic mix of clustered mass components at redshifts z ≲ 1.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/561860fd4b97aa03025dcb235b0990d589580926

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THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, background): “…works (e.g. Cavaliere et al. 1998, Balogh et al. 1999, Wu et al. 2000; Tozzi et al. 2001) and numerical simulations (e.g. Navarro et al. 1995, Brighenti & Mathews 2001, Bialek et al. 2001, Borgani et al. 2001a) converge to indicate that ∼ 1 keV per gas particle of extra energy is required.”
Simulations of AGN Feedback in Galaxy Clusters and Groups: Impact on Gas Fractions and the LX-T Scaling Relation (2008, background): “Several attempts have been made to tackle these problems with so-called ‘preheating’ schemes (e.g. Bialek et al. 2001; Borgani et al. 2005), that are meant to mimic more energetic astrophysical processes than the relatively inefficient supernovae feedback.”
SIMULATIONS OF THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM WITH ACTIVE GALACTIC NUCLEUS FEEDBACK (2010, background): “Pre-heating (e.g. Bialek et al. 2001) and AGN feedback (e.g. Sijacki et al. 2007, 2008; Puchwein et al. 2008) help solve the over-cooling problem and improve agreement with observed cluster properties.”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, background): “These trends are naturally expected in scenarios where self–similarity is broken by extra heating (e.g., Bialek et al. 2001), which prevents gas from reaching high density in central regions.”
Galaxy Clusters in Hubble Volume Simulations: Cosmological Constraints from Sky Survey Populations (2001, background): “The preheated cluster simulations of Bialek et al. (2001) produce low redshift scaling relations for X–ray luminosity, isophotal size and ICM mass versus temperature that simultaneously match local observations and exhibit little evolution in the LX–”
Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3 (2003, methodology): “…either by episodes of non-gravitational heating due to supernovae and AGN (e.g., Evrard & Henry 1991; Cavaliere et al. 1999; Tozzi & Norman 2001; Bialek et al. 2001; Brighenti & Mathews 2001; Babul et al. 2002; Borgani et al. 2002), or by selective removal of low-entropy gas through cooling…”
Temperature Profiles of Nearby Clusters of Galaxies (2001, background): “Their profile is the average of twelve cluster simulations performed for a Λ-CDM cosmology (Ω = 0.3, Λ = 0.7) characterized by an initial entropy level of 105.9 keV cm−2 (entropy level S3 in Bialek et al. 2001), and it is normalized to match our observed core temperature.”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, background): “Explanations for this invoke physical processes which lower fb in clusters relative to the universal fraction (see e.g. Bialek et al. 2001; He et al. 2006), baryon components that fail detection by standard X-ray and/or optical techniques (see Ettori 2003; Lin & Mohr 2004), or a systematic…”
Sample Variance Considerations for Cluster Surveys (2002, background): “Extensive simulations of cluster formation have shed light onto the role of non-gravitational processes such as galactic feedback (e.g., Metzler & Evrard 1994; Navarro et al. 1995; Bialek et al. 2001; Holder & Carlstrom 2001) and radiative cooling (e.g., Muanwong et al. 2001).”
Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality (2008, background): “2 Tight intrinsic correlations between X-ray, SZ, and optical observables and cluster mass are expected theoretically (e.g., Bialek et al. 2001; da Silva et al. 2004; Motl et al. 2005; Nagai 2006; Kravtsov et al. 2006) and were shown to exist observationally (e.g., Mohr et al. 1999; Lin et al.…”