Cold dark matter

Science

Volumn 274, Issue 5284, 1996, Pages 69-75

  Dodelson, Scott ^a   Gates, Evalyn I ^a,b   Turner, Michael S ^a,b  

^a NASA FERMILAB ASTROPHYSICS CENTER   (United States)

^b UNIVERSITY OF CHICAGO   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ANISOTROPY; COSMOS; MATHEMATICAL MODEL; MICROWAVE RADIATION; PARTICLE RADIATION; PRIORITY JOURNAL; QUANTUM THEORY; REVIEW;

EID: 0029742523     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.274.5284.69     Document Type: Review

References (138)

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15. n. Scale invariance corresponds to n = 1. A is a numerical constant that depends on the model of inflation and its value sets the overall level of inhomogeneity.
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44. In spite of the fact that it is difficult to find inflationary models that predict precisely n = 1, this choice was taken for simplicity.
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52. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
53. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
54. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
55. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
56. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
57. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
58. Computation of both the CBR anisotropy and the level of inhomogeneity today depends on the invisible-matter content and the cosmological parameters and requires that the distribution of matter and radiation be evolved numerically. We have carried out these calculations by integrating the coupled Einstein and Boltzmann equations. For details see, for example, P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, ibid. 243, 14 (1981); J. R. Bond and G. Efstathiou, ibid. 285, L45 (1984); J. A. Holtzman, Astrophys. J. Suppl. 71, 1 (1989); A. van Dalen and R. K. Schaefer, Astrophys. J. 398, 33 (1992); N. Sugiyama and N. Gouda, Prog. Theor. Phys. 88, 803 (1992); S. Dodelson and J, M. Jubas, Phys. Rev. Lett. 70, 2224 (1993).
59. There are now a variety of tests based on numerical simulations that confront models with data on scales that have become nonlinear (73). They represent an important step in testing models, but because the simulations are so time consuming, they are not very useful in spanning the large sets of parameters we are interested in here.
60. 0. Such surveys are called red shift surveys.
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