Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement

R. Stompor; M. Abroe; P. Ade; A. Balbi; D. Barbosa; J. Bock; J. Borrill; A. Boscaleri; P. De Bernardis; P. G. Ferreira; S. Hanany; V. Hristov; A. H. Jaffe; A. T. Lee; E. Pascale; B. Rabii; P. L. Richards; G. F. Smoot; C. D. Winant; J. H.P. Wu

doi:10.1086/324438

Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement

R. Stompor, M. Abroe, P. Ade, A. Balbi, D. Barbosa, J. Bock, J. Borrill, A. Boscaleri, P. De Bernardis, P. G. Ferreira, S. Hanany, V. Hristov, A. H. Jaffe, A. T. Lee, E. Pascale, B. Rabii, P. L. Richards, G. F. Smoot, C. D. Winant, J. H.P. Wu

Physics and Astronomy (Twin Cities)

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Abstract

We discuss the cosmological implications of the new constraints on the power spectrum of the cosmic microwave background (CMB) anisotropy derived from a new high-resolution analysis of the MAXIMA-1 measurement. The power spectrum indicates excess power at l ∼ 860 over the average level of power at 411 ≤ l ≤ 785. This excess is statistically significant at the ∼95% confidence level. Its position coincides with that of the third acoustic peak, as predicted by generic inflationary models selected to fit the first acoustic peak as observed in the data. The height of the excess power agrees with the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments. Our results therefore lend support for inflationary models and more generally for the dominance of adiabatic coherent perturbations in the structure formation of the universe. At the same time, they seem to disfavor a large variety of the nonstandard (but inflation-based) models that have been proposed to improve the quality of fits to the CMB data and the consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE/Differential Microwave Radiometer data give best-fit values and 95% confidence limits for the baryon density, Ω_bh² ≃ 0.033 ± 0.013, and the total density, Ω = 0.9_-0.16^+0.18. The primordial spectrum slope (n_s) and the optical depth to the last scattering surface (τ_c) are found to be degenerate and to obey the relation n_s ≃ (0.99 ± 0.14) + 0.46τ_c, for τ_c ≤ 0.5 (all at 95% confidence levels).

Original language	English (US)
Pages (from-to)	L7-L10
Journal	Astrophysical Journal
Volume	561
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/324438
State	Published - Nov 1 2001

Bibliographical note

Funding Information:
This work was supported by NASA grants NAG5-3941 (R. S., S. H.), NAG5-6552 (J. H. P. W., A. H. J.), S00-GSRP-032, and S00-GSRP-031 (B. R., C. D. W.); NSF KDI grant 9872979 (J. H. P. W., A. H. J.); and the Royal Society (P. G. F.). Computing resources were provided by the Minnesota Supercomputing Institute and the National Energy Research Computing Center at Lawrence Berkeley National Laboratory. MAXIMA is supported by NASA grant NAG5-4454 and by the NSF through the Center for Particle Astrophysics at UC Berkeley, NSF cooperative agreement AST 91-20005. The likelihood from SN data was kindly provided by S. Jha and the High-Z SN Search Team.

Keywords

Cosmic microwave background
Cosmology: observations

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Stompor, R., Abroe, M., Ade, P., Balbi, A., Barbosa, D., Bock, J., Borrill, J., Boscaleri, A., De Bernardis, P., Ferreira, P. G., Hanany, S., Hristov, V., Jaffe, A. H., Lee, A. T., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Winant, C. D., & Wu, J. H. P. (2001). Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement. Astrophysical Journal, 561(1 PART 2), L7-L10. https://doi.org/10.1086/324438

Stompor, R, Abroe, M, Ade, P, Balbi, A, Barbosa, D, Bock, J, Borrill, J, Boscaleri, A, De Bernardis, P, Ferreira, PG, Hanany, S, Hristov, V, Jaffe, AH, Lee, AT, Pascale, E, Rabii, B, Richards, PL, Smoot, GF, Winant, CD & Wu, JHP 2001, 'Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement', Astrophysical Journal, vol. 561, no. 1 PART 2, pp. L7-L10. https://doi.org/10.1086/324438

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title = "Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement",

abstract = "We discuss the cosmological implications of the new constraints on the power spectrum of the cosmic microwave background (CMB) anisotropy derived from a new high-resolution analysis of the MAXIMA-1 measurement. The power spectrum indicates excess power at l ∼ 860 over the average level of power at 411 ≤ l ≤ 785. This excess is statistically significant at the ∼95% confidence level. Its position coincides with that of the third acoustic peak, as predicted by generic inflationary models selected to fit the first acoustic peak as observed in the data. The height of the excess power agrees with the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments. Our results therefore lend support for inflationary models and more generally for the dominance of adiabatic coherent perturbations in the structure formation of the universe. At the same time, they seem to disfavor a large variety of the nonstandard (but inflation-based) models that have been proposed to improve the quality of fits to the CMB data and the consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE/Differential Microwave Radiometer data give best-fit values and 95% confidence limits for the baryon density, Ωbh2 ≃ 0.033 ± 0.013, and the total density, Ω = 0.9-0.16+0.18. The primordial spectrum slope (ns) and the optical depth to the last scattering surface (τc) are found to be degenerate and to obey the relation ns ≃ (0.99 ± 0.14) + 0.46τc, for τc ≤ 0.5 (all at 95% confidence levels).",

keywords = "Cosmic microwave background, Cosmology: observations",

author = "R. Stompor and M. Abroe and P. Ade and A. Balbi and D. Barbosa and J. Bock and J. Borrill and A. Boscaleri and {De Bernardis}, P. and Ferreira, {P. G.} and S. Hanany and V. Hristov and Jaffe, {A. H.} and Lee, {A. T.} and E. Pascale and B. Rabii and Richards, {P. L.} and Smoot, {G. F.} and Winant, {C. D.} and Wu, {J. H.P.}",

note = "Funding Information: This work was supported by NASA grants NAG5-3941 (R. S., S. H.), NAG5-6552 (J. H. P. W., A. H. J.), S00-GSRP-032, and S00-GSRP-031 (B. R., C. D. W.); NSF KDI grant 9872979 (J. H. P. W., A. H. J.); and the Royal Society (P. G. F.). Computing resources were provided by the Minnesota Supercomputing Institute and the National Energy Research Computing Center at Lawrence Berkeley National Laboratory. MAXIMA is supported by NASA grant NAG5-4454 and by the NSF through the Center for Particle Astrophysics at UC Berkeley, NSF cooperative agreement AST 91-20005. The likelihood from SN data was kindly provided by S. Jha and the High-Z SN Search Team.",

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doi = "10.1086/324438",

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T1 - Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement

AU - Stompor, R.

AU - Abroe, M.

AU - Ade, P.

AU - Balbi, A.

AU - Barbosa, D.

AU - Bock, J.

AU - Borrill, J.

AU - Boscaleri, A.

AU - De Bernardis, P.

AU - Ferreira, P. G.

AU - Hanany, S.

AU - Hristov, V.

AU - Jaffe, A. H.

AU - Lee, A. T.

AU - Pascale, E.

AU - Rabii, B.

AU - Richards, P. L.

AU - Smoot, G. F.

AU - Winant, C. D.

AU - Wu, J. H.P.

N1 - Funding Information: This work was supported by NASA grants NAG5-3941 (R. S., S. H.), NAG5-6552 (J. H. P. W., A. H. J.), S00-GSRP-032, and S00-GSRP-031 (B. R., C. D. W.); NSF KDI grant 9872979 (J. H. P. W., A. H. J.); and the Royal Society (P. G. F.). Computing resources were provided by the Minnesota Supercomputing Institute and the National Energy Research Computing Center at Lawrence Berkeley National Laboratory. MAXIMA is supported by NASA grant NAG5-4454 and by the NSF through the Center for Particle Astrophysics at UC Berkeley, NSF cooperative agreement AST 91-20005. The likelihood from SN data was kindly provided by S. Jha and the High-Z SN Search Team.

PY - 2001/11/1

Y1 - 2001/11/1

N2 - We discuss the cosmological implications of the new constraints on the power spectrum of the cosmic microwave background (CMB) anisotropy derived from a new high-resolution analysis of the MAXIMA-1 measurement. The power spectrum indicates excess power at l ∼ 860 over the average level of power at 411 ≤ l ≤ 785. This excess is statistically significant at the ∼95% confidence level. Its position coincides with that of the third acoustic peak, as predicted by generic inflationary models selected to fit the first acoustic peak as observed in the data. The height of the excess power agrees with the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments. Our results therefore lend support for inflationary models and more generally for the dominance of adiabatic coherent perturbations in the structure formation of the universe. At the same time, they seem to disfavor a large variety of the nonstandard (but inflation-based) models that have been proposed to improve the quality of fits to the CMB data and the consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE/Differential Microwave Radiometer data give best-fit values and 95% confidence limits for the baryon density, Ωbh2 ≃ 0.033 ± 0.013, and the total density, Ω = 0.9-0.16+0.18. The primordial spectrum slope (ns) and the optical depth to the last scattering surface (τc) are found to be degenerate and to obey the relation ns ≃ (0.99 ± 0.14) + 0.46τc, for τc ≤ 0.5 (all at 95% confidence levels).

AB - We discuss the cosmological implications of the new constraints on the power spectrum of the cosmic microwave background (CMB) anisotropy derived from a new high-resolution analysis of the MAXIMA-1 measurement. The power spectrum indicates excess power at l ∼ 860 over the average level of power at 411 ≤ l ≤ 785. This excess is statistically significant at the ∼95% confidence level. Its position coincides with that of the third acoustic peak, as predicted by generic inflationary models selected to fit the first acoustic peak as observed in the data. The height of the excess power agrees with the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments. Our results therefore lend support for inflationary models and more generally for the dominance of adiabatic coherent perturbations in the structure formation of the universe. At the same time, they seem to disfavor a large variety of the nonstandard (but inflation-based) models that have been proposed to improve the quality of fits to the CMB data and the consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE/Differential Microwave Radiometer data give best-fit values and 95% confidence limits for the baryon density, Ωbh2 ≃ 0.033 ± 0.013, and the total density, Ω = 0.9-0.16+0.18. The primordial spectrum slope (ns) and the optical depth to the last scattering surface (τc) are found to be degenerate and to obey the relation ns ≃ (0.99 ± 0.14) + 0.46τc, for τc ≤ 0.5 (all at 95% confidence levels).

KW - Cosmic microwave background

KW - Cosmology: observations

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U2 - 10.1086/324438

DO - 10.1086/324438

M3 - Article

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VL - 561

SP - L7-L10

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JF - Astrophysical Journal

IS - 1 PART 2

ER -

Cosmological implications of the maxima-1 high-resolution cosmic microwave background anisotropy measurement

Abstract

Bibliographical note

Keywords

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