MASSIVE HALOS IN MILLENNIUM GAS SIMULATIONS: MULTIVARIATE SCALING RELATIONS

By R. Stanek, E. Rasia, August E. Evrard, Frazer R. Pearce, L. Gazzola. 2009

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The joint likelihood of observable cluster signals reflects the astrophysical evolution of the coupled baryonic and dark matter components in massive halos, and its knowledge will enhance cosmological parameter constraints in the coming era of large, multiwavelength cluster surveys. We present a computational study of intrinsic covariance in cluster properties using halo populations derived from Millennium Gas Simulations (MGS). The MGS are re-simulations of the original 500 h−1 Mpc Millennium Simulation performed with gas dynamics under two different physical treatments: shock heating driven by gravity only (GO) and a second treatment with cooling and preheating (PH). We examine relationships among structural properties and observable X-ray and Sunyaev–Zel'dovich (SZ) signals for samples of thousands of halos with M200 ⩾ 5 × 1013 h−1 M☉ and z < 2. While the X-ray scaling behavior of PH model halos at low redshift offers a good match to local clusters, the model exhibits non-standard features testable with larger surveys, including weakly running slopes in hot gas observable–mass relations and ∼10% departures from self-similar redshift evolution for 1014 h−1 M☉ halos at redshift z ∼ 1. We find that the form of the joint likelihood of signal pairs is generally well described by a multivariate, log-normal distribution, especially in the PH case which exhibits less halo substructure than the GO model. At fixed mass and epoch, joint deviations of signal pairs display mainly positive correlations, especially the thermal SZ effect paired with either hot gas fraction (r = 0.88/0.69 for PH/GO at z = 0) or X-ray temperature (r = 0.62/0.83). The levels of variance in X-ray luminosity, temperature, and gas mass fraction are sensitive to the physical treatment, but offsetting shifts in the latter two measures maintain a fixed 12% scatter in the integrated SZ signal under both gas treatments. We discuss halo mass selection by signal pairs, and find a minimum mass scatter of 4% in the PH model by combining thermal SZ and gas fraction measurements.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b4e9634c27f0f13ef3f11851dee55b3c96940f95

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THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “Interestingly, the pseudo-evolution is not apparent in the actual evolution of cluster scaling relations, such as theM − T relation (see, e.g.,Nagai 2006; Stanek et al. 2010).”
COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2016, background): “…X-ray data, integrated cluster pressure is predicted and measured to track cluster mass with low scatter (e.g., Motl et al. 2005; Nagai et al. 2007; Stanek et al. 2010; Kravtsov et al. 2006), but its relation to true cluster mass can be complicated by non-thermal pressure support in clusters…”
Scaling Properties of a Complete X-ray Selected Galaxy Group Sample (2014, methodology): “M-YX and LX -YX relations The YX parameter defined by Kravtsov et al. (2006) is considered one of the less scattered mass proxies, although this is still a matter of debate (see Stanek et al. 2010).”
Towards a realistic population of simulated galaxy groups and clusters (2013, result): “This is consistent with the findings of previous simulation studies, such as those of Bhattacharya et al. (2008), Puchwein et al. (2008), Short & Thomas (2009), Fabjan et al. (2010), Stanek et al. (2010) and Planelles et al. (2013).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, background): “We note, however, that the preheating simulations of Stanek et al. (2010) do suggest a lower level of kinetic energy in bulk motions than in simulations without preheating.”
GALAXY CLUSTERS SELECTED WITH THE SUNYAEV–ZEL'DOVICH EFFECT FROM 2008 SOUTH POLE TELESCOPE OBSERVATIONS (2010, background): “%) uncertainty in the mass function normalization, Stanek et al. (2010) have demonstrated that the inclusion of non-gravitational baryon physics in cosmological simulations can modify cluster masses in the range of the SPT sample by ∼ ± 10% relative to gravityonly hydrodynamical simulations.”
The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics (2013, methodology): “Examples of such mass proxies are the total thermal content of the intra–cluster plasma, measured from either X–ray (e.g., Kravtsov et al. 2006; Stanek et al. 2010; Fabjan et al. 2010) or Sunyaev-Zel’dovich (e.g. Arnaud et al. 2010; Williamson et al. 2011; Kay et al. 2012) observations, the optical…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “…does not necessarily imply departure from self-similar evolution with redshift; for example, the high-mass halos in the preheated simulations of Stanek et al. (2010) have X-ray luminosities that evolve within 10% of the self-similar expectation at z ≤ 1, despite having a slope with mass that…”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, background): “…there is a non-zero covariance which reflects common sensitivities to halo structure, orientation, environment and foreground/background superposition – surrogates which are similarly sensitive to these factors are expected to exhibit a high degree of correlation (see also Stanek et al. 2010).”
COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY (2011, background): “Numerical simulations have also led to a better understanding of systematic biases in cluster mass estimates derived from a broad range of cluster observables (e.g., Kravtsov et al. 2006; Jeltema et al. 2008; Stanek et al. 2010; Becker & Kravtsov 2011).”
Formation of Galaxy Clusters (2012, methodology): “This is evidenced by deviations of scaling relation evolution from these predictions in hydrodynamical simulations of cluster formation even in the absence of any physical processes that can break self-similarity (e.g., Nagai 2006, Stanek et al. 2010).”
ON THE CLUSTER PHYSICS OF SUNYAEV–ZEL'DOVICH AND X-RAY SURVEYS. I. THE INFLUENCE OF FEEDBACK, NON-THERMAL PRESSURE, AND CLUSTER SHAPES ON Y–M SCALING RELATIONS (2011, methodology): “Hence in order to improve upon the determination of cosmological parameters, a better understanding of the mass proxies and their scatter is needed (Nagai 2006; Shaw et al. 2008; Stanek et al. 2010; Yang et al. 2010; Krause et al. 2011).”
Observational probes of cosmic acceleration (2012, background): “%) on the total mass within a high overdensity threshold (e.g., the ∆ = 500ρcrit threshold frequently adopted in X-ray analyses; see Stanek et al. 2009).”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, background): “…to have the smallest variation with mass or redshift, and the smallest intrinsic scatter (Eke et al. 1998; Kay et al. 2004; Crain et al. 2007; Nagai et al. 2007; Stanek et al. 2010; Young et al. 2011; Borgani & Kravtsov 2011; Battaglia et al. 2013; Planelles et al. 2013; Sembolini et al. 2013).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, background): “…temperature, gas mass and lensing mass measured for a given cluster, due to e.g. asphericity or dynamical state, are similarly thought to be small (see e.g. calculations by Gavazzi 2005 and Buote & Humphrey 2012, hydrodynamical simulations by Stanek et al. 2010, and further discussion in WtG V).”