MEASUREMENTS OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH THE SOUTH POLE TELESCOPE

By M. Lueker, C. Reichardt, K. Schaffer, Oliver Zahn, P. Ade, K. Aird, B. Benson, L. Bleem, J. Carlstrom, C. Chang and 34 more. 2009

165 citations recorded by the source corpus.

We report cosmic microwave background (CMB) power-spectrum measurements from the first 100 deg2 field observed by the South Pole Telescope (SPT) at 150 and 220 GHz. On angular scales where the primary CMB anisotropy is dominant, ℓ ≲ 3000, the SPT power spectrum is consistent with the standard ΛCDM cosmology. On smaller scales, we see strong evidence for a point-source contribution, consistent with a population of dusty, star-forming galaxies. After we mask bright point sources, anisotropy power on angular scales of 3000 < ℓ < 9500 is detected with a signal-to-noise ratio ≳50 at both frequencies. We combine the 150 and 220 GHz data to remove the majority of the point-source power and use the point-source-subtracted spectrum to detect Sunyaev–Zel'dovich (SZ) power at 2.6σ. At ℓ = 3000, the SZ power in the subtracted bandpowers is 4.2 ± 1.5 μK2, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. This discrepancy may suggest that contemporary galaxy cluster models overestimate the thermal pressure of intracluster gas. Alternatively, this result can be interpreted as evidence for lower values of σ8. When combined with an estimate of the kinetic SZ contribution, the measured SZ amplitude shifts σ8 from the primary CMB anisotropy derived constraint of 0.794 ± 0.028 down to 0.773 ± 0.025. The uncertainty in the constraint on σ8 from this analysis is dominated by uncertainties in the theoretical modeling required to predict the amplitude of the SZ power spectrum for a given set of cosmological parameters.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/42aae670db4c9ee48095dacea49a2f37957ec9b1

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Citations in the corpus

A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, background): “…2007) have sufficient sensitivity, angular resolution, and frequency coverage to measure the power spectrum of the thermal SZ (tSZ) effect and to place increasingly strong upper limits on contributions from the kinetic SZ (kSZ) effect (Lueker et al. 2010; Shirokoff et al. 2011; Das et al. 2011).”
The evolution of CMB spectral distortions in the early Universe (2011, background): “…E-mail: jchluba@cita.utoronto.ca 1 http://www.esa.int/Planck unprecedented precision, while both ACT (e.g., see Hajian et l. 2010; Dunkley et al. 2010; Das et al. 2011) and SPT (Lueker et al. 2010; Vanderlinde et al. 2010) are pushing the frontier ofTT CMB power spectra at small angular scales.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, result): “Subject to the systematic uncertainties mentioned, their results are broadly in agreement, and are consistent with estimates of σ8 obtained from studies of resolved clusters and the primary CMB (Dunkley et al. 2010; Lueker et al. 2010; Komatsu et al. 2011).”
The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data (2013, methodology): “Along with the damping tail measurements, rapid progress has been made in the measurements and modeling of this high-multipole tail ([26, 37]; [9]; [10, 33]).”
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): “…integrated power spectrum have been long term goals in CMB research, and are reaching fruition through,e.g., the South Pole Telescope, SPT (e.g., Lueker et al. 2010; Shirokoff et al. 2010; Keisler et al. 2011; Vanderlinde et al. 2010), the Atacama Cosmology Telescope, ACT (e.g., Fowler et al.…”
A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA (2012, methodology): “…the dark energy equation of state (Staniszewski et al. 2009; Vanderlinde et al. 2010; Foley et al. 2011; Williamson et al. 2011) and to measure the power spectrum of the mm-wave sky on small angular scales (Lueker et al. 2010; Hall et al. 2010; Shirokoff et al. 2011; K11; Reichardt et al. 2011).”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, methodology): “The method closely follows the approach used by Lueker et al. (2010) and Shirokoff et al. (2011).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, methodology): “Recent SPT measurements of the small-scale CMB temperature anisotropy power spectrum (Lueker et al. 2010) have demonstrated there to be some tension between the value of σ8 implied by the measured amplitude of the tSZ power spectrum at ℓ = 3000 and those derived from WMAP observations of the…”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “The SPT collaboration stacked the SZ maps of 11 known clusters and fitted the stacked SZ radial profile to the above form, finding c500 = 1.0, α = 1.0, β = 5.5, and γ = 0.5 (Plagge et al. 2010).”
Planck2015 results (2015, unknown): “A simple and direct test of the parametric foreground modelling used in the CamSpec and Plik likelihoods is to compare results with a completely different approach in which the lowfrequency maps are “cleaned” using higher frequency maps as foreground templates (see, e.g., Lueker et al. 2010).”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, background): “The power spectrum near l = 3000 has recently been measured by and discussed in Lueker et al. (2010), Das et al. (2011), and Dunkley et al. (2010).”