Cosmic microwave background: Past, future and present

International Journal of Modern Physics A

Volumn 15, Issue 17, 2000, Pages 2629-2644

  Dodelson, Scott ^a  

^a NASA HEADQUARTERS   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ACCURACY; ANISOTROPY; COSMIC RADIATION; COSMOLOGICAL PHENOMENA; COSMOS; MICROWAVE RADIATION; PHOTON; REVIEW; SPECTROSCOPY; THEORY; VACUUM;

EID: 0034631712     PISSN: 0217751X     EISSN: None     Source Type: Journal    
DOI: 10.1142/S0217751X00001154     Document Type: Review

References (87)

1. Some nice recent reviews of perturbations generated by inflation are: E. Stewart and D. Lyth, Phys. Lett. B302, 171 (1993); L. Wang, V. Mukhanov and P. Steinhardt, Phys. Lett. B414, 18 (1997); I. Grivell and A. Liddle, Phys. Rev. D54, 7191 (1996); J. Lidsey et al., Rev. Mod. Phys. 69, 373 (1997); D. Lyth and A. Riotto, Phys. Rep. 314, 1 (1999).
2. Some nice recent reviews of perturbations generated by inflation are: E. Stewart and D. Lyth, Phys. Lett. B302, 171 (1993); L. Wang, V. Mukhanov and P. Steinhardt, Phys. Lett. B414, 18 (1997); I. Grivell and A. Liddle, Phys. Rev. D54, 7191 (1996); J. Lidsey et al., Rev. Mod. Phys. 69, 373 (1997); D. Lyth and A. Riotto, Phys. Rep. 314, 1 (1999).
3. Some nice recent reviews of perturbations generated by inflation are: E. Stewart and D. Lyth, Phys. Lett. B302, 171 (1993); L. Wang, V. Mukhanov and P. Steinhardt, Phys. Lett. B414, 18 (1997); I. Grivell and A. Liddle, Phys. Rev. D54, 7191 (1996); J. Lidsey et al., Rev. Mod. Phys. 69, 373 (1997); D. Lyth and A. Riotto, Phys. Rep. 314, 1 (1999).
4. Some nice recent reviews of perturbations generated by inflation are: E. Stewart and D. Lyth, Phys. Lett. B302, 171 (1993); L. Wang, V. Mukhanov and P. Steinhardt, Phys. Lett. B414, 18 (1997); I. Grivell and A. Liddle, Phys. Rev. D54, 7191 (1996); J. Lidsey et al., Rev. Mod. Phys. 69, 373 (1997); D. Lyth and A. Riotto, Phys. Rep. 314, 1 (1999).
5. Some nice recent reviews of perturbations generated by inflation are: E. Stewart and D. Lyth, Phys. Lett. B302, 171 (1993); L. Wang, V. Mukhanov and P. Steinhardt, Phys. Lett. B414, 18 (1997); I. Grivell and A. Liddle, Phys. Rev. D54, 7191 (1996); J. Lidsey et al., Rev. Mod. Phys. 69, 373 (1997); D. Lyth and A. Riotto, Phys. Rep. 314, 1 (1999).
6. See e.g. W. Hu and N. Sugiyama, Astrophys. J. 444, 489 (1995).
7. G. Smoot et al., Astrophys. J. 396, L1 (1992).
8. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
9. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
10. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
11. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
12. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
13. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
14. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
15. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
16. Some of the many people who have computed the evolution of perturbations in an expanding universe include P. J. E. Peebles and J. T. Yu, Astrophys. J. 162, 815 (1970); M. L. Wilson and J. Silk, Astrophys. J. 243, 14 (1981); P. J. E. Peebles, Astrophys. J. 248, 885 (1981); J. R. Bond and A. Szalay, Astrophys. J. 274, 443 (1983); J. R. Bond and G. Efstathiou, Astrophys. J. 285, L45 (1984); J. R. Bond and G. Efstathiou, Mon. Not. R. Astron. Soc. 226, 655 (1987); S. Dodelson and J. Jubas, Phys. Rev. Lett. 70, 2224 (1993); R. Crittenden et al., Phys. Rev. Lett. 71, 324 (1993); W. Hu, D. Scott, N. Sugiyama and M. White, Phys. Rev. D52, 5498 (1995).
17. U. Seljak and M. Zaldarriaga, Astrophys. J. 469, 437 (1996).
18. J. Peterson et al., submitted to Astrophys. J. Lett. astro-ph/9910503.
19. E. Torbet et al., Astrophys. J., in press, astro-ph/9905100; A. D. Miller et al., Astrophys. J., in press, astro-ph/9906421.
20. E. Torbet et al., Astrophys. J., in press, astro-ph/9905100; A. D. Miller et al., Astrophys. J., in press, astro-ph/9906421.
21. E. Cheng et al., Astrophys. J. 422, L37 (1994); E. Cheng et al., Astrophys. J. 456, L71 (1996); E. Cheng et al., Astrophys. J. 488, L59 (1997); G. Wilson et al., Astrophys. J. in press, astro-ph/9902047.
22. E. Cheng et al., Astrophys. J. 422, L37 (1994); E. Cheng et al., Astrophys. J. 456, L71 (1996); E. Cheng et al., Astrophys. J. 488, L59 (1997); G. Wilson et al., Astrophys. J. in press, astro-ph/9902047.
23. E. Cheng et al., Astrophys. J. 422, L37 (1994); E. Cheng et al., Astrophys. J. 456, L71 (1996); E. Cheng et al., Astrophys. J. 488, L59 (1997); G. Wilson et al., Astrophys. J. in press, astro-ph/9902047.
24. E. Cheng et al., Astrophys. J. 422, L37 (1994); E. Cheng et al., Astrophys. J. 456, L71 (1996); E. Cheng et al., Astrophys. J. 488, L59 (1997); G. Wilson et al., Astrophys. J. in press, astro-ph/9902047.
25. P. Mauskopf et al., astro-ph/9911444; A. Melchiorri, astro-ph/9911445.
26. K. Coble et al., Astrophys. J. Lett. 519, 5 (1999).
27. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
28. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
29. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
30. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
31. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
32. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
33. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
34. The numbers shown in Fig. 4 come from the latest and most accurate set of predictions, D. Eisenstein, W. Hu and M. Tegmark, Astrophys. J. 518, 2 (1999). These follow a string of similar papers, starting from J. R. Bond et al., Phys. Rev. Lett. 72, 13 (1994), continuing to the ground breaking work of L. Knox, Phys. Rev. D52, 4307 (1995) and G. Jungman et al., Phys. Rev. 54, 1332 (1996). Other attempts along the way include S. Dodelson, W. Kinney and E. Kolb, Phys. Rev. D36, 3207 (1997), M. Zaldarriaga, D. Spergel and U. Seljak, Astrophys. J. 488, 1 (1997); J. R. Bond, G. Efstathiou and M. Tegmark, Mon. Not. R. Astron. Soc. 291, L33 (1997); R. Lopez et al., Phys. Rev. Lett. 82, 3952 (1999)
35. See e.g. W. Freedman, in Conf. Proc. 18th Texas Symposium (Chicago, December 1996), eds. A. Olinto, J. Friemann and D. Schramm (World Scientific, Singapore, 1998).
36. S. Buries and D. Tytler, Astrophys. J. 499, 699 (1998).
37. Y. Fukuda et al. (Super-Kamiokande collaboration), Phys. Rev. Lett. 81, 1562 (1998).
38. C. Athanassopoulos (LSND Collaboration), Phys. Rev. Lett. 81, 1774 (1998).
39. W. Hu, D. Eisenstein and M. Tegmark, Astrophys. J. 80, 5255 (1998).
40. W. Hu and M. Tegmark, Phys. Rev. Lett. 514, L65 (1999).
41. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
42. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
43. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
44. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
45. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
46. Modern computations of polarization within the framework of inflation include M. Kamionkowski, A. Kosowsky and A. Stebbins, Phys. Rev. Lett. 78, 2058 (1997); M. Zaldarriaga and U. Seljak, Phys. Rev. D55, 1830 (1997); and W. Hu and M. White, New Astron. 2, 323 (1997). The power of polarization to test inflation has been pointed out in D. Spergel and M. Zaldarriaga, Phys. Rev. Lett. 79, 2180 (1997) and W. Kinney, Phys. Rev. D58, 123506 (1998) among other places. Using these arguments, the CMB Future Missions Working Group recently argued for a post-Planck polarization mission, J. Peterson et al., astro-ph/9907276.
47. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
48. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
49. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
50. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
51. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
52. For models of reionization, see e.g. B. J. Carr, J. R. Bond and W. D. Arnett, Astrophys. J. 277, 445 (1984); H. M. P. Couchman and M. J. Rees, Mon. Not. R. Astron. Soc. 221, 53 (1986); M. Fukugita and M. Kawasaki, Mon. Not. R. Astron. Soc. 269, 563 (1994); P. R. Shapiro, M. L. Giroux and A. Babul, Astrophys. J. 427, 25 (1994); M. Tegmark, J. Silk and A. Blanchard, Astrophys. J. 434, 395 (1995); J. P. Ostriker and Y. N. Gnedin, Astrophys. J. 486, 581 (1997); and Z. Haiman and A. Loeb, Astrophys. J. 483, 21 (1997).
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