Extracting primordial density fluctuations

Science

Volumn 280, Issue 5368, 1998, Pages 1405-1411

  Gawiser, Eric ^a   Silk, Joseph ^a  

^a UNIVERSITY OF CALIFORNIA   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ANISOTROPY; ARTICLE; COSMOS; DENSITY; GEOMETRY; POWER SPECTRUM; PRIORITY JOURNAL; THEORY;

EID: 0032577390     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.280.5368.1405     Document Type: Article

References (129)

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19. The primordial power spectrum does not have to be an exact power law; inflationary models predict slight variation of the power-law index with scale. Allowing this spectral index to vary freely makes it more difficult to constrain cosmological models, as shown by E. Gawiser and J. Silk, in Proceedings, Particle Physics and the Early Universe Conference (1997), available at http://www.mrao.cam.ac.uk/ppeuc/proceedings; E. Gawiser, in Proceedings of the 18th Texas Symposium on Relativistic Astrophysics, Chicago, IL, December 1996, A. Olinto, J. Frieman, D. N. Schramm, Eds. (World Scientific, Singapore, in press).
20. The primordial power spectrum does not have to be an exact power law; inflationary models predict slight variation of the power-law index with scale. Allowing this spectral index to vary freely makes it more difficult to constrain cosmological models, as shown by E. Gawiser and J. Silk, in Proceedings, Particle Physics and the Early Universe Conference (1997), available at http://www.mrao.cam.ac.uk/ppeuc/proceedings; E. Gawiser, in Proceedings of the 18th Texas Symposium on Relativistic Astrophysics, Chicago, IL, December 1996, A. Olinto, J. Frieman, D. N. Schramm, Eds. (World Scientific, Singapore, in press).
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30. For the TCDM model, see M. White, D. Scott, J. Silk, M. Davis, Mon. Not. R. Astron. Soc. 276, L69 (1995); for the CHDM model, see M. Davis, F. J. Summers, D. Schlegel, Nature 359, 393 (1992); A. Klypin, J. Holtzman, J. Primack, E. Regos, Astrophys. J. 416, 1 (1993); D. Y. Pogosyan and A. A. Starobinsky, Mon. Not. R. Astron. Soc. 265, 507 (1993); E. Choi and D. Ryu, ibid., in press (available at http://xxx.lanl.gov/ abs/astro-ph/9710078).
31. 2 eV = 4.7 eV.
32. v = 0.3 by a small margin. The parameters for CHDM and TCDM are within the range found acceptable by (6) and (7).
33. P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1998). Several other types of scalar fields have been proposed recently [R. R. Caldwell, R. Dave, P. J. Steinhardt, ibid. 80, 1586 (1998); P. T. P. Viana and A. R. Liddle, Phys. Rev. D 57, 674 (1998); M. S. Turner and M. White, ibid. 56, R4439 (1997); K. Coble, S. Dodelson, J. A. Frieman, ibid. 55, 1851 (1997)]. φCDM is a scalar field model that seems to agree well with the observations.
34. P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1998). Several other types of scalar fields have been proposed recently [R. R. Caldwell, R. Dave, P. J. Steinhardt, ibid. 80, 1586 (1998); P. T. P. Viana and A. R. Liddle, Phys. Rev. D 57, 674 (1998); M. S. Turner and M. White, ibid. 56, R4439 (1997); K. Coble, S. Dodelson, J. A. Frieman, ibid. 55, 1851 (1997)]. φCDM is a scalar field model that seems to agree well with the observations.
35. P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1998). Several other types of scalar fields have been proposed recently [R. R. Caldwell, R. Dave, P. J. Steinhardt, ibid. 80, 1586 (1998); P. T. P. Viana and A. R. Liddle, Phys. Rev. D 57, 674 (1998); M. S. Turner and M. White, ibid. 56, R4439 (1997); K. Coble, S. Dodelson, J. A. Frieman, ibid. 55, 1851 (1997)]. φCDM is a scalar field model that seems to agree well with the observations.
36. P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1998). Several other types of scalar fields have been proposed recently [R. R. Caldwell, R. Dave, P. J. Steinhardt, ibid. 80, 1586 (1998); P. T. P. Viana and A. R. Liddle, Phys. Rev. D 57, 674 (1998); M. S. Turner and M. White, ibid. 56, R4439 (1997); K. Coble, S. Dodelson, J. A. Frieman, ibid. 55, 1851 (1997)]. φCDM is a scalar field model that seems to agree well with the observations.
37. P. G. Ferreira and M. Joyce, Phys. Rev. Lett. 79, 4740 (1998). Several other types of scalar fields have been proposed recently [R. R. Caldwell, R. Dave, P. J. Steinhardt, ibid. 80, 1586 (1998); P. T. P. Viana and A. R. Liddle, Phys. Rev. D 57, 674 (1998); M. S. Turner and M. White, ibid. 56, R4439 (1997); K. Coble, S. Dodelson, J. A. Frieman, ibid. 55, 1851 (1997)]. φCDM is a scalar field model that seems to agree well with the observations.
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74. -1, which is confirmed by the likelihood analysis of S. Zaroubi, I. Zehavi, A. Dekel, Y. Hoffman, and T. Kolatt [ibid. 486, 21 (1997)]. A full discussion of peculiar velocity data is given by M. Gramann [ibid. 493, 28 (1998)].
75. -1, which is confirmed by the likelihood analysis of S. Zaroubi, I. Zehavi, A. Dekel, Y. Hoffman, and T. Kolatt [ibid. 486, 21 (1997)]. A full discussion of peculiar velocity data is given by M. Gramann [ibid. 493, 28 (1998)].
76. -1, which is confirmed by the likelihood analysis of S. Zaroubi, I. Zehavi, A. Dekel, Y. Hoffman, and T. Kolatt [ibid. 486, 21 (1997)]. A full discussion of peculiar velocity data is given by M. Gramann [ibid. 493, 28 (1998)].
77. -1 to avoid possible artifacts of the survey window function at higher k.
78. -1 to avoid possible artifacts of the survey window function at higher k.
79. -1 to avoid possible artifacts of the survey window function at higher k.
80. -1 to avoid possible artifacts of the survey window function at higher k.
81. -1 Mpc version of the SSRS2+CfA2 survey to avoid the luminosity bias present in the deeper sample noted by C. Park, M. S. Vogeley, M. J. Geller, and J. P. Huchra [Astrophys. J. 431, 569 (1994)].
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84. 8 are also bias-independent.
85. 8 are also bias-independent.
86. 8 are also bias-independent.
87. 8 are also bias-independent.
88. -1 Mpc and twice that for the higher one. This systematic uncertainty in the pairwise velocity dispersion makes the corrected real-space power spectrum somewhat unreliable on smaller scales. For the cluster power spectrum, we used only the scale-independent Kaiser distortion term to correct for redshift distortions as the clusters are engaged in coherent infall onto superclusters. The APM galaxy power spectrum was corrected for bias only, as it does not have redshift distortions.
89. -1 Mpc and twice that for the higher one. This systematic uncertainty in the pairwise velocity dispersion makes the corrected real-space power spectrum somewhat unreliable on smaller scales. For the cluster power spectrum, we used only the scale-independent Kaiser distortion term to correct for redshift distortions as the clusters are engaged in coherent infall onto superclusters. The APM galaxy power spectrum was corrected for bias only, as it does not have redshift distortions.
90. -1 Mpc and twice that for the higher one. This systematic uncertainty in the pairwise velocity dispersion makes the corrected real-space power spectrum somewhat unreliable on smaller scales. For the cluster power spectrum, we used only the scale-independent Kaiser distortion term to correct for redshift distortions as the clusters are engaged in coherent infall onto superclusters. The APM galaxy power spectrum was corrected for bias only, as it does not have redshift distortions.
91. -1 Mpc and twice that for the higher one. This systematic uncertainty in the pairwise velocity dispersion makes the corrected real-space power spectrum somewhat unreliable on smaller scales. For the cluster power spectrum, we used only the scale-independent Kaiser distortion term to correct for redshift distortions as the clusters are engaged in coherent infall onto superclusters. The APM galaxy power spectrum was corrected for bias only, as it does not have redshift distortions.
92. -1.
93. -1. At smaller k, the linearization preserves the shape of the observed nonlinear P(k) while sliding the data points to smaller k; its main effect is to shrink the error bars slightly.
94. -1.
95. Defined by G. Efstathiou, J. R. Bond, and S. D. M. White [Mon. Not. R. Astron. Soc. 258, 1P (1992)].
96. C. B. Netterfield et al., Astrophys. J. 474, 47 (1997). We used the recalibration of SK from E. Leitch [thesis, California Institute of Technology (1997)].
97. J. A. Peacock, Mon. Not. R. Astron. Soc. 284, 885 (1997) and (48) also found good agreement between the linearized observations and linear theory under the CHDM model.
98. P. F. S. Scott et al., Astrophys. J. 461, L1 (1996); J. C. Baker, in Proceedings, Particle Physics and the Early Universe Conference (1997), available at http:// www.mrao.cam.ac.uk/ppeuc/proceedings.
99. P. F. S. Scott et al., Astrophys. J. 461, L1 (1996); J. C. Baker, in Proceedings, Particle Physics and the Early Universe Conference (1997), available at http:// www.mrao.cam.ac.uk/ppeuc/proceedings.
100. We averaged the predictions of the matter power spectrum over the window function of the observations to take into account the possible smoothing of these oscillations during observation. To make the linearization procedure work smoothly, we fixed the local slope of the linear power spectrum.
101. This is roughly consistent with the bias ratios found by (41).
102. See D. M. Goldberg and M. A. Strauss, Astrophys. J. 495, 29 (1998) for the future prospects of this constraint.
103. If the APM Galaxy P(k) were ignored, OCDM, ΛCDM, and φCDM would become much better fits but would still be ruled out at the 95% confidence level.
104. φ = 0.08. The PBH BDM model has 30% of critical density in primordial black holes, which act like CDM but actually contain baryonic matter.
105. σ8 column and a total of 69 degrees of freedom.
106. The error bars include uncertainties due to instrument noise, calibration uncertainty, sample variance from observing only part of the sky, and cosmic variance from observing at only one location in the universe. The calibration errors were added in quadrature. Although calibration errors are correlated for multiple observations by the same instrument, they have been treated as independent, which is a good approximation after the recalibration of SK by Leitch (52).
107. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
108. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
109. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
110. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
111. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
112. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et
113. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
114. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
115. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
116. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
117. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
118. CMB anisotropy observations are compiled by G. F. Smoot and D. Scott, Rev. Part. Prop., [on-line] (available at http://xxx.lanl.gov/abs/astro-ph/9711069) and at http://www.sns.ias.edu/~max/cmb/experiments.html. Shown here are observations from COBE (M. Tegmark and A. Hamilton, http://xxx.lanl. gov/abs/astro-ph/9702019), FIRS [K. Ganga, L. Page, E. Cheng., S. Meyers, Astrophys. J. 432, L15 (1993)], Tenerife [C. M. Gutierrez et al., ibid. 480, L83 (1997)]. the South Pole [J. O. Gundersen et al., ibid. 443, L57, (1994)], BAM [G. S. Tucker et al., ibid. 475, L74 (1997)], ARGO [S. Masi et al., ibid. 463, L47 (1996)], Python [S. R. Platt et al., ibid. 475, L1 (1997)], MAX (Microwave Anisotropy Experiment) [M. Lim et al., ibid. 469, L69 (1996); S. T. Tanaka et al., ibid. 468, L81 (1996)], MSAM (Medium-Scale Anisotropy Measurement) [E. S. Cheng et al., ibid. 488, L59 (1997)], SK (52), and CAT (54).
119. m.
120. -1.
121. 8 follow the local shape of each model's P(k) to indicate they are a model-dependent averaging of the power over a range of k.
122. 2 distribution [A. Stirling, thesis, University of Edinburgh (1998)].
123. It is possible that the linearization procedure needs to be adjusted to account for non-Gaussianity in the matter distribution, but the reduced power of this model weakens the effects of nonlinear evolution.
124. Microwave anisotropy probe (MAP) and Planck parameters were taken from J. R. Bond, G. Efstathiou, and M. Tegmark [Mon. Not. R. Astron. Soc. 291, L33 (1997)]. The Sloan Digital Sky Survey (SDSS) data are from M. Vogeley (personal communication), and the 2-Degree Field (2DF) Survey data are from S. Cole, S. Hatton, D. Weinberg, C. S. Frenk, http:// xxx.lanl.gov/abs/astro-ph/9801250. No attempt has been made in Fig. 4D to account for redshift distortions or nonlinear evolution. The overlap in scale between CMB anisotropy detections and large-scale structure observations should increase tremendously in the next several years, and the errors in these measurements should decrease significantly.
125. Microwave anisotropy probe (MAP) and Planck parameters were taken from J. R. Bond, G. Efstathiou, and M. Tegmark [Mon. Not. R. Astron. Soc. 291, L33 (1997)]. The Sloan Digital Sky Survey (SDSS) data are from M. Vogeley (personal communication), and the 2-Degree Field (2DF) Survey data are from S. Cole, S. Hatton, D. Weinberg, C.S. Frenk, http://xxx.lanl.gov/abs/astro-ph/9801250. No attempt has been made in Fig. 4D to account for redshift distortions or nonlinear evolution. The overlap in scale between CMB anisotropy detections and large-scale structure observations should increase tremendously in the next several years, and the errors in these measurements should decrease significantly.
126. v can be determined by SDSS observations, and
127. Y. Wang, D. N. Spergel, and M. A. Strauss (in preparation; available at http:// xxx.lanl.gov/abs/astro-ph/9802231) discuss the ability of combined MAP and SDSS observations to constrain cosmological parameters.
128. We gratefully acknowledge the contributions of U. Seljak and M. Zaldarriaga (CMBFAST). P. Ferreira (φCDM), J. Peebles (ICDM), N. Sugiyama (PBH BDM), J. Robinson (strings + Λ), H. Tadros (APM cluster analysis for various cosmologies), and the efforts of hundreds of observers who gathered the data. This work benefited from conversations with H. Tadros, M. White, M. Vogeley, P. Viana, A. Taylor, A. Stirling, J. Robinson, J. Peebles, J. Peacock, A. Liddle, A. Jaffe, W. Hu, A. Heavens, G. Evrard, C. Baugh, and W. Ballinger. We thank L. Moustakas for comments on a draft of this paper. E.G. acknowledges the support of an NSF Graduate Fellowship. We thank the Institut d'Astrophysique de Paris for hospitality during the completion of this research. Our data compilation and full-size figures are available at http://cfpa.berkeley.edu/ home.html.
129. We gratefully acknowledge the contributions of U. Seljak and M. Zaldarriaga (CMBFAST). P. Ferreira (φCDM), J. Peebles (ICDM), N. Sugiyama (PBH BDM), J. Robinson (strings + Λ), H. Tadros (APM cluster analysis for various cosmologies), and the efforts of hundreds of observers who gathered the data. This work benefited from conversations with H. Tadros, M. White, M. Vogeley, P. Viana, A. Taylor, A. Stirling, J. Robinson, J. Peebles, J. Peacock, A. Liddle, A. Jaffe, W. Hu, A. Heavens, G. Evrard, C. Baugh, and W. Ballinger. We thank L. Moustakas for comments on a draft of this paper. E.G. acknowledges the support of an NSF Graduate Fellowship. We thank the Institut d'Astrophysique de Paris for hospitality during the completion of this research. Our data compilation and full-size figures are available at http://cfpa.berkeley.edu/ home.html.