Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations
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Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations Olivier Forni IAS-CNRS, Universit´e Paris Sud, Bˆatiment 121, 91405 Orsay Cedex, France Email: [email protected]
Nabila Aghanim IAS-CNRS, Universit´e Paris Sud, Bˆatiment 121, 91405 Orsay Cedex, France Email: [email protected] Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 30 May 2004; Revised 11 December 2004 In this first attempt to extract a map of the kinetic Sunyaev-Zel’dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of 0.78 on average, and an error on the standard deviation of the reconstructed KSZ map of only 5% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel’dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the CMB + KSZ map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise. Keywords and phrases: cosmic microwave background, data analysis.
1. INTRODUCTION The cosmic microwave background (CMB) temperature anisotropies field encloses so-called primary anisotropies, directly related to the initial density fluctuations at early stages of the universe, and so-called secondary anisotropies generated after matter and radiation decoupled. The secondary anisotropies arise from the interaction of the CMB photons with gravitational potential wells or with ionised gas along their way towards us. More “local” contributions to the CMB signal are due to foreground emissions from our galaxy and from distant galaxies. One of the major goals of observational cosmology is to use the CMB anisotr
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