LEADER 04637nam 2200613Ia 450 001 9910741173903321 005 20200520144314.0 010 $a3-319-00309-7 024 7 $a10.1007/978-3-319-00309-2 035 $a(CKB)2670000000371080 035 $a(EBL)1205647 035 $a(SSID)ssj0000908087 035 $a(PQKBManifestationID)11469057 035 $a(PQKBTitleCode)TC0000908087 035 $a(PQKBWorkID)10897053 035 $a(PQKB)11499745 035 $a(DE-He213)978-3-319-00309-2 035 $a(MiAaPQ)EBC1205647 035 $a(PPN)16913749X 035 $a(EXLCZ)992670000000371080 100 $a20130315d2013 uy 0 101 0 $aeng 135 $aur|n|---||||| 181 $ctxt 182 $cc 183 $acr 200 10$aNon-linear data analysis on the sphere $ethe quest for anomalies in the cosmic microwave background /$fGregor Rossmanith 205 $a1st ed. 2013. 210 $aNew York $cSpringer$d2013 215 $a1 online resource (126 p.) 225 1 $aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 300 $aDescription based upon print version of record. 311 $a3-319-03337-9 311 $a3-319-00308-9 320 $aIncludes bibliographical references. 327 $aSupervisor's Foreword; Preface; Contents; 1 Introduction and Theoretical Background; 1.1 A Short Sketch of the Standard Model of Cosmology; 1.2 The Role of Inflation; 1.2.1 Inflation as an Improvement of the Standard Model; 1.2.2 Basic Concept of Inflation; 1.3 The Cosmic Microwave Background Radiation; 1.3.1 Origin; 1.3.2 Characteristics; 1.3.3 Notations; 1.4 The Challenge of Anomalies in the CMB; References; 2 Methods for Testing the Non-Gaussianity of the CMB; 2.1 Statistical Tests for Non-Gaussianity; 2.1.1 Basic Framework; 2.1.2 Surrogates on the Complete Sky 327 $a2.1.3 Surrogates on an Incomplete Sky2.2 Measures for Non-Gaussianity; 2.2.1 Overview Over Currently Used Measures; 2.2.2 The Scaling Index Method; References; 3 Observations of the CMB with the WMAP Satellite; 3.1 Framework of the Observation; 3.2 Foreground and Systematic Effects; 3.2.1 Origin and Characteristics; 3.2.2 Methods of Foreground Reduction; References; 4 Scaling Indices Applied to the WMAP 5-Year Data; 4.1 Introduction; 4.2 WMAP Data and Simulations; 4.3 Weighted Scaling Index Method; 4.3.1 Formalism; 4.3.2 Coping with Boundary Effects; 4.4 Results 327 $a4.4.1 Band-wise and Co-added Map Analysis4.4.2 Local Features; 4.5 Summary; 4.6 Conclusions; References; 5 Surrogates and Scaling Indices Applied to the WMAP 7-Year Data; References; 6 Extending the Analysis of the WMAP 7-Year Data; 6.1 Introduction; 6.2 Data Sets; 6.3 Generating Surrogate Maps; 6.4 Weighted Scaling Indices and Test Statistics; 6.5 Results; 6.6 Conclusions; References; 7 Applying the Surrogate Approach to Incomplete Skies; References; 8 Conclusions; AppendixSimplifications of the Cut Sky Approach; A.1...Constant Latitude CutsSimplifications of the Cut Sky Approach 327 $aA.2...The Householder TransformationReferences 330 $aThis work deals with the search for signatures of non-Gaussianities in the cosmic microwave background (CMB). Probing Gaussianity in the CMB addresses one of the key questions in modern cosmology because it allows us to discriminate between different models of inflation, and thus concerns a fundamental part of the standard cosmological model.     The basic goal here is to adapt complementary methods stemming from the field of complexity science to CMB data analysis. Two key concepts, namely the method of surrogates and estimators for local scaling properties, are applied to CMB data analysis.     All results show strong non-Gaussianities and pronounced asymmetries. The consistency of the full sky and cut sky results shows convincingly for the first time that the influence of the Galactic plane is not responsible for these deviations from Gaussianity and isotropy. The findings seriously call into question predictions of isotropic cosmologies based on the widely accepted single field slow roll inflation model. 410 0$aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 606 $aCosmology 606 $aCosmic background radiation 615 0$aCosmology. 615 0$aCosmic background radiation. 676 $a523.10285 700 $aRossmanith$b Gregor$01424810 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910741173903321 996 $aNon-linear Data Analysis on the Sphere$93554345 997 $aUNINA