Table of Contents
Preface and Acknowledgments xiii
Chapter 1 Introduction 1
1.1 The Science and Philosophy of Cosmology 2
1.2 An Overview 6
Chapter 2 The Homogeneous Universe 12
2.1 Einstein's Cosmological Principle 12
2.2 Early Evidence of Inhomogeneity 16
2.3 Early Evidence of Homogeneity: Isotropy 18
2.4 Early Evidence of Homogeneity: Counts and Redshifts 22
2.5 The Universe as a Stationary Random Process 25
2.6 A Fractal Universe 31
2.7 Concluding Remarks 34
Chapter 3 Cosmological Models 36
3.1 Discovery of the Relativistic Expanding Universe 36
3.2 The Relativistic Big Bang Cosmology 45
3.3 The Steady-State Cosmology 50
3.4 Empirical Assessments of the Steady-State Cosmology 51
3.5 Nonempirical Assessments of the Big Bang Model 56
3.5.1 Early Thinking 56
3.5.2 Cosmological Inflation 62
3.5.3 Biasing 66
3.6 Empirical Assessments of the Big Bang Model 69
3.6.1 Time Scales 71
3.6.2 Cosmological Tests in the 1970s 74
3.6.3 Mass Density Measurements: Introduction 77
3.6.4 Mass Density Measurements: Hubble to the Revolution 82
3.6.5 Mass Density Measurements: Assessments 105
3.7 Concluding Remarks 111
Chapter 4 Fossils: Microwave Radiation and Light Elements 114
4.1 Thermal Radiation in an Expanding Universe 115
4.2 Gamow's Scenario 122
4.2.1 Gamow's 1948 Papers 123
4.2.2 Predicting the Present CMB Temperature 130
4.2.3 The Alpher, Bethe, and Gamow Paper 133
4.3 Helium and Deuterium from the Hot Big Bang 139
4.3.1 Recognition of Fossil Helium 139
4.3.2 Helium in a Cold Universe 143
4.3.3 Developments in 1964 and 1965 146
4.4 Sources of Microwave Radiation 151
4.4.1 Interstellar Cyanogen 153
4.4.2 Detection at Bell Laboratories 156
4.4.3 Zel'dovich's Group 158
4.4.4 Dicke's Group 160
4.4.5 Recognition of the CMB 162
4.5 Measuring the CMB Intensity Spectrum 164
4.5.1 The Situation in the 1970s 164
4.5.2 Alternative Interpretations 166
4.5.3 The Submillimeter Anomalies 169
4.5.4 Establishing the CMB Thermal Spectrum 171
4.6 Nucleosynthesis and the Baryon Mass Density 174
4.7 Why Was the Hot Big Bang Cosmology Reinvented? 182
Chapter 5 How Cosmic Structure Grew 184
5.1 The Gravitational Instability Picture 186
5.1.1 Lemaître's Solution 193
5.1.2 Lifshitz's Perturbation Analyses 198
5.1.3 Nongravitational Interaction of Baryons and the CMB 202
5.1.4 The Jeans Mass 208
5.2 Scenarios 210
5.2.1 Chaos and Order 210
5.2.2 Primeval Turbulence 213
5.2.3 Gravitational Origin of Galaxy Rotation 216
5.2.4 Explosions 221
5.2.5 Spontaneously Broken Homogeneity 223
5.2.6 Initial Conditions 229
5.2.7 Bottom-Up or Top-Down Structure Formation 233
5.3 Concluding Remarks 236
Chapter 6 Subluminal Mass 239
6.1 Clusters of Galaxies 240
6.2 Groups of Galaxies 245
6.3 Galaxy Rotation Curves 247
6.3.1 The Andromeda Nebula 248
6.3.2 NGC 3115 255
6.3.3 NGC 300 257
6.3.4 NGC 2403 258
6.3.5 The Burbidges's Program 260
6.3.6 Challenges 260
6.4 Stabilizing Spiral Galaxies 265
6.5 Recognizing Subluminal Matter 272
6.6 What Is the Nature of the Subluminal Matter? 276
Chapter 7 Nonbaryonic Dark Matter 279
7.1 Hot Dark Matter 280
7.1.1 Apparent Detection of a Neutrino Rest Mass 285
7.2 Cold Dark Matter 289
7.2.1 What Happened in 1977 290
7.2.2 The Situation in the Early 1980s 295
7.2.3 The Search for Dark Matter Detection 297
Chapter 8 The Age of Abundance of Cosmological Models 300
8.1 Why Is the CMB So Smooth? 301
8.2 The Counterexample: CDM 302
8.3 CDM and Structure Formation 307
8.4 Variations on the Theme 311
8.4.1 TCDM 312
8.4.2 DDM and MDM 313
8.4.3 ΛCDM and τCDM 314
8.4.4 Other Thoughts 315
8.5 How Might It All Fit Together? 316
Chapter 9 The 1998-2003 Revolution 323
9.1 The Redshift-Magnitude Test 323
9.2 The CMB Temperature Anisotropy 332
9.3 What Happened at the Turn of the Century 335
9.4 The Future of Physical Cosmology 340
Chapter 10 The Ways of Research 343
10.1 Technology 343
10.2 Human Behavior 344
10.3 Roads Not Taken 345
10.4 The Social Construction of Science 348
References 355
Index 399
