
Contents
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8.1 Why Is the CMB So Smooth? 8.1 Why Is the CMB So Smooth?
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8.2 The Counterexample: CDM 8.2 The Counterexample: CDM
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8.3 CDM and Structure Formation 8.3 CDM and Structure Formation
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8.4 Variations on the Theme 8.4 Variations on the Theme
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8.4.1 TCDM 8.4.1 TCDM
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8.4.2 DDM and MDM 8.4.2 DDM and MDM
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8.4.3 ΛCDM and τCDM 8.4.3 ΛCDM and τCDM
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8.4.4 Other Thoughts 8.4.4 Other Thoughts
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8.5 How Might It All Fit Together? 8.5 How Might It All Fit Together?
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Eight The Age of Abundance of Cosmological Models
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Published:June 2020
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Abstract
This chapter examines why in the early 1980s cosmologists co-opted the astronomers' subluminal mass and the particle physicists' nonbaryonic matter in what became known as the standard cold dark matter, or sCDM, cosmological model. The letter “s” might be taken to mean that the model was designed to be simple (as it was) but it instead signified “standard,” not because it was established but because it came first. A large part of the cosmology community soon adopted variants of the sCDM model as bases for exploration of how galaxies might have formed in the observed patterns of their space distribution and motions, and for analyses of the effect of galaxy formation on the angular distribution of the sea of thermal radiation. This widespread adoption was arguably overenthusiastic, because it was easy to devise other models, less simple to be sure, that fit what we knew at the time. And it was complicated by the nonempirical feeling that space sections surely are flat.
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