IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM

By L. Shaw, D. Nagai, Suman Bhattacharya, E. Lau. 2010

179 citations recorded by the source corpus.

We use an analytic model to investigate the theoretical uncertainty on the thermal Sunyaev–Zel'dovich (SZ) power spectrum due to astrophysical uncertainties in the thermal structure of the intracluster medium. Our model accounts for star formation and energy feedback (from supernovae and active galactic nuclei) as well as radially dependent non-thermal pressure support due to random gas motions, the latter calibrated by recent hydrodynamical simulations. We compare the model against X-ray observations of low-redshift clusters, finding excellent agreement with observed pressure profiles. Varying the levels of feedback and non-thermal pressure support can significantly change both the amplitude and shape of the thermal SZ power spectrum. Increasing the feedback suppresses power at small angular scales, shifting the peak of the power spectrum to lower ℓ. On the other hand, increasing the non-thermal pressure support has the opposite effect, significantly reducing power at large angular scales. In general, including non-thermal pressure at the level measured in simulations has a large effect on the power spectrum, reducing the amplitude by 50% at angular scales of a few arcminutes compared to a model without a non-thermal component. Our results demonstrate that measurements of the shape of the power spectrum can reveal useful information on important physical processes in groups and clusters, especially at high redshift where there exists little observational data. Comparing with the recent South Pole Telescope measurements of the small-scale cosmic microwave background power spectrum, we find our model reduces the tension between the values of σ8 measured from the SZ power spectrum and from cluster abundances.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ae950cf072c0d6ca40bcab9e0224d4a1523791db

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Citations in the corpus

THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, background): “These processes have a much larger impact on lower mass clusters and groups where the gravitational potential is not strong enough to tightly bind the cluster gas (e.g., Battaglia et al. 2010; Shaw et al. 2010; Trac et al. 2011).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, background): “The 2-point function is a potentially-powerful probe of σ8 (Komatsu & Seljak 2002); however, it is sensitive to the low-mass end of the Y (M) scaling relation for clusters, which is subject to astrophysical corrections (Shaw et al. 2010; Battaglia et al. 2010, 2012a).”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND DAMPING TAIL FROM THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2012, methodology): “The shape of the thermal SZ spectrum is taken from Shaw et al. (2010) with an amplitude taken from Reichardt et al. (2012).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “In W11 a scaling relation based on the SPT signal to noise ratio and calibrated to the models of [100] is used to obtain SZ based mass estimates.”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL’DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY (2012, methodology): “The tSZ map is drawn from a 4000 deg2 simulation by Shaw 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): “(A1) andPkin/Ptot, split by different mass bin which have been scaled byM1/5200, i.e. nM = 1/5, that minimizes our χ2.”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, methodology): “The SZ component uses the thermal SZ template of Sehgal et al. (2010a), which has a shape similar to the templates from more recent models (Trac et al. 2011; Shaw et al. 2010; Battaglia et al. 2010), normalized to D` = 5.5 µK 2 at ` = 3000.”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM (2010, methodology): “In this analysis we consider four thermal SZ templates, from Sehgal et al. (2010a), Trac, Bode, & Ostriker (2010), Battaglia et al. (2010), and Shaw et al. (2010).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “If the distortion pattern from a single halo of mass M at redshift z is described by an angular Fourier transform, ỹ(M, z, ℓ), then the full halo population will generate a fluctuation spectrum (Shaw et al. 2010) Cℓ ∝ ∫ dz dV dz ∫ d lnM dn d lnM ỹ2(M, z, ℓ).”
COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE (2011, methodology): “We make new predictions for the tSZ-CIB correlation by combining the tSZ model of Shaw et al. (2010) with the halo model based CIB calculations of Shang et al. (2012).”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, background): “…spectrum from independent simulations and analytical models (e.g., Komatsu & Seljak 2002; Shaw et al. 2009; Sehgal et al. 2010; Trac et al. 2011; Shaw et al. 2010; Battaglia et al. 2012a; Efstathiou & Migliaccio 2012), and the expected amplitude for ﬁxed cosmological model varies depending on…”
JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES (2012, background): “Numerical simulation studies suggest that this bias is due to incomplete thermalization of the hot diffuse intracluster medium (ICM) (Evrard 1990; Rasia et al. 2006; Nagai et al. 2007; Shaw et al. 2010; Rasia et al. 2012).”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, methodology): “A significant fraction of the total tSZ power is contributed by groups and clusters of mass M500 < 2 × 1014h−1 M and redshift z > 0.65 (Trac et al. 2011; Battaglia et al. 2011b; Shaw et al. 2010).”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “We adopt the baseline model from Shaw et al. (2010) as the baseline model in this work.”
CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg2 SPT-SZ SURVEY (2012, background): “…+DSZ3000f SZ l (1) where DPS3000, D CL 3000, and D SZ 3000 are the amplitudes at l = 3000 for the Poisson point source power, clustered point source power, and total SZ power spectrum respectively, and fSZl gives the l-dependence of the SZ power spectrum as modeled in Shaw et al. (2010).”
GALAXY CLUSTERS SELECTED WITH THE SUNYAEV–ZEL'DOVICH EFFECT FROM 2008 SOUTH POLE TELESCOPE OBSERVATIONS (2010, methodology): “…simulations, while reproducing observed low-redshift X-ray observations, may overestimate SZ flux in higher-redshift systems, implying missing physics in the semianalytic gas modeling (for example, a non-negligible amount of non-thermal pressure support at higher redshifts; Shaw et al. 2010b).”
The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, unknown): “3 (Shaw et al. 2010; Trac et al. 2011).”