The Sunyaev-Zel'dovich angular power spectrum as a probe of cosmological parameters

By E. Komatsu, Uros Seljak. 2002

356 citations recorded by the source corpus.

The angular power spectrum of the Sunyaev–Zel'dovich (SZ) effect is a powerful probe of cosmology. It is easier to detect than individual clusters in the field, is insensitive to observational selection effects and does not require a calibration between cluster mass and flux, reducing the systematic errors that dominate the cluster-counting constraints. It receives a dominant contribution from virialized cluster region between 20 and 40 per cent of the virial radius and is thus relatively insensitive to the poorly known gas physics in the cluster centre, such as cooling or (pre)heating. In this paper we derive a refined analytic prediction for the SZ angular power spectrum using the universal gas density and temperature profile and the dark matter halo mass function. The predicted power spectrum has no free parameters and fits all of the published hydrodynamic simulation results to better than a factor of 2 for 2000 < l < 10 000. We find that the angular power spectrum Cl scales as Cl∝σ78(Ωbh)2 and is almost independent of all of the other cosmological parameters. This differs from the local cluster abundance studies, which give a relation between σ8 and Ωm. We also compute the covariance matrix of Cl using the halo model and find a good agreement relative to the simulations. We argue that the best constraint from the SZ power spectrum comes from l∼ 3000, where the sampling variance is sufficiently small and the spectrum is dominated by massive clusters above 1014h−1 M⊙ for which cooling, heating and details of star formation are not very important. We estimate how well we can determine σ8(Ωbh)2/7 with sampling-variance-limited observations and find that for a several-square-degree survey with arcmin resolution one should be able to determine σ8 to within a few per cent, with the remaining uncertainty dominated by theoretical modelling. If the recent excess of the cosmic microwave background power on small scales reported by Cosmic Background Imager (CBI) and Berkeley Illinois Maryland Association (BIMA) experiments is due to the SZ effect, then we find σ8(Ωbh/0.035)0.29= 1.04 ± 0.12 at 95 per cent confidence level (statistical) and with a residual 10 per cent systematic (theoretical) uncertainty.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/99b80ae8ef906c8afd0c2cf2082ca832036706a6

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Citations in the corpus

Halo Substructure and the Power Spectrum (2002, result): “While many analyses continue to measure “high” values for σ8 ∼ 1 (Van Waerbeke et al. 2002; Komatsu & Seljak 2002; Bahcall & Bode 2003; where σ8 is the linear, rms fluctuation amplitude on a length scale of 8 h−1 Mpc ), numerous recent studies relying on similar techniques, advocate rather “low”…”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM (2010, methodology): “In Fowler et al. (2010) we assumed a seventh power scaling, with AtSZ ∝ σ 7 8 (Komatsu & Seljak 2002), giving an upper limit of σSZ8 < 0.84 at 95% CL, for AtSZ < 1.6.”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, methodology): “The anisotropy power due to the tSZ effect is highly sensitive to the normalization of the matter power spectrum, commonly parametrized by the RMS of the z = 0 mass distribution on 8 Mpc/h scales, σ8 (Komatsu & Seljak 2002).”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, methodology): “…authors, we have ignored the small contribution to the TT data expected to arise from the Sunyaev-Z’eldovich (SZ) effect in clusters and groups (e.g. Komatsu & Seljak 2002) and do not account for gravitational lensing of the CMB (Lewis & Challinor 2006), which has a negligible effect on the…”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, methodology): “This can be calculated assuming spherical symmetry using (Bracewell 2000; Komatsu & Seljak 2002): ỹ(M, z, ℓ) = 4πrc ℓ2c ∫ ∞ 0 dxx2Py(M, z, x) sin(ℓx/ℓc) ℓx/ℓc , (3) where x = r/rc, ℓc = DA(z)/rc, rc is a characteristic scale radius of the profile, DA(z) is the angular diameter distance to redshift…”
SIMULATIONS OF THE MICROWAVE SKY (2009, methodology): “The green line shows the comparison with the thermal SZ power spectrum derived analyticlly from Komatsu & Seljak (2002) and taken from the WMAP LAMBDA website (http://lambda.gsfc.nasa.gov/product/map/current/). perature at frequencyν in the direction̂n is given by ∆T TCMB (n̂) = ∫ [ θe(Y0 + θeY1 +…”
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, background): “Next, we define the characteristic temperature of the halo (Komatsu & Seljak 2002) as kT200 = GM200µmp 3R200 = µmp 3 [10GH0M200E(z)] 2/3 , (12) so we can write the total thermal energy of the halo with Eq.”
Observable Spectra of Induced Gravitational Waves from Inflation (2012, background): “[7]), bounds from Ultra compact Mini Halos [8–12] and the astrophysical bounds on the production of Primordial Black Holes (PBHs) [13, 14].”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, background): “This is an important effect as lower mass systems (< 1014 M ) contribute as much to the SZ power spectrum at l ∼ 3000 as systems at higher mass (Komatsu & Seljak 2002; Trac et al. 2011).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “(12) Adding halo spatial correlations gives a small correction to this estimate (Komatsu & Seljak 2002).”
Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology (2006, unknown): “Since the WMAP spectral coverage is not sufficient to be able to distinguish CMB fluctuations from SZ fluctuations (see discussion in Hinshaw et al. 2007), we marginalize over its amplitude using the Komatsu & Seljak (2002) analytical model for the shape of the SZ fluctuations.”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, background): “The higher redshift and lower mass groups that make an important contribution to the tSZ signal ([6, 37, 69]) are also likely to host dusty galaxies.”
Planck 2015 results: XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation (2015, unknown): “…computed using the Fourier trans- form of the projected profiles of signals A and B weighted by the mass function and the A and B emission (see, e.g., Komatsu & Seljak 2002, for a derivation of the tSZ angular power spectrum): CAB,1h ` = 4π ∫ dz dV dzdΩ ∫ dM d2N dMdV WA,1hWB,1h, (10) where…”