# Constraints on the High-l Power Spectrum of Millimeter-wave Anisotropies from APEX-SZ

Source: [Constraints on the High-l Power Spectrum of Millimeter-wave Anisotropies from APEX-SZ](<https://www.sota2.com/research/paper/68fa23b52c2a37601939b30e>)

Collection index: [llms.txt](<https://www.sota2.com/research/llms.txt>)

Data updated: 2025-10-28T13:52:37.925Z

Authors: C.L. Reichardt, O. Zahn, P.A.R. Ade, K. Basu, A.N. Bender, F. Bertoldi, H.-M. Cho, G. Chon, M. Dobbs, D. Ferrusca, N.W. Halverson, W.L. Holzapfel, C. Horellou, D. Johansson, B. R. Johnson, J. Kennedy, R. Kneissl, T. Lanting, A. T. Lee, M. Lueker, J. Mehl, K. M. Menten, M. Nord, F. Pacaud, P. L. Richards, R. Schaaf, D. Schwan, H. Spieler, A. Weiss, B. Westbrook

Published: 2009-04-27T17:55:33.000Z

## Abstract

We present measurements of the angular power spectrum of millimeter wave anisotropies with the APEX-SZ instrument. APEX-SZ has mapped 0.8 square degrees of sky at a frequency of 150 GHz with an angular resolution of 1'. These new measurements significantly improve the constraints on anisotropy power at 150 GHz over the range of angular multipoles 3000 \< l \< 10,000, limiting the total astronomical signal in a flat band power to be less than 105 microK^2 at 95% CL. We expect both submillimeter-bright, dusty galaxies and to a lesser extent secondary CMB anisotropies from the Sunyaev-Zel'dovich effect (SZE) to significantly contribute to the observed power. Subtracting the SZE power spectrum expected for sigma\_8=0.8 and masking bright sources, the best fit value for the remaining power is C\_l = 1.1^{+0.9}\_{-0.8} x 10^{-5} micro K^2 (1.7^{+1.4}\_{-1.3} Jy^2 sr^{-1}). This agrees well with model predictions for power due to submillimeter-bright, dusty galaxies. Comparing this power to the power detected by BLAST at 600 GHz, we find the frequency dependence of the source fluxes to be S\_nu ~ nu^{2.6^{+0.4}\_{-0.2}} if both experiments measure the same population of sources. Simultaneously fitting for the amplitude of the SZE power spectrum and a Poisson distributed point source population, we place an upper limit on the matter fluctuation amplitude of sigma\_8 \< 1.18 at 95% confidence.

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## Original sources and implementation

[Original paper](<https://arxiv.org/abs/0904.3939>)

[PDF](<https://arxiv.org/pdf/0904.3939.pdf>)