Planck intermediate results XXIV. Constraints on variations in fundamental constants

被引：93

作者：

Ade, P. A. R. ^{[74
]}

Aghanim, N. ^{[50
]}

Arnaud, M. ^{[62
]}

Ashdown, M. ^{[5
,59
]}

Aumont, J. ^{[50
]}

Baccigalupi, C. ^{[73
]}

Banday, A. J. ^{[9
,81
]}

Barreiro, R. B. ^{[56
]}

Battaner, E. ^{[82
,83
]}

Benabed, K. ^{[51
,80
]}

Benoit-Levy, A. ^{[21
,51
,80
]}

Bernard, J. -P. ^{[9
,81
]}

Bersanelli, M. ^{[29
,42
]}

Bielewicz, P. ^{[9
,73
,81
]}

Bond, J. R. ^{[8
]}

Borrill, J. ^{[12
,76
]}

Bouchet, F. R. ^{[51
,80
]}

Burigana, C. ^{[27
,41
]}

Butler, R. C. ^{[41
]}

Calabrese, E. ^{[78
]}

Chamballu, A. ^{[14
,50
,62
]}

Chiang, H. C. ^{[6
,24
]}

Christensen, P. R. ^{[32
,70
]}

Clements, D. L. ^{[47
]}

Colombo, L. P. L. ^{[20
,57
]}

Couchot, F. ^{[60
]}

Curto, A. ^{[5
,56
]}

Cuttaia, F. ^{[41
]}

Danese, L. ^{[73
]}

Davies, R. D. ^{[58
]}

Davis, R. J. ^{[58
]}

de Bernardis, P. ^{[28
]}

de Rosa, A. ^{[41
]}

de Zotti, G. ^{[38
,73
]}

Delabrouille, J. ^{[1
]}

Diego, J. M. ^{[56
]}

Dole, H. ^{[49
,50
]}

Dore, O. ^{[10
,57
]}

Dupac, X. ^{[35
]}

Ensslin, T. A. ^{[67
]}

Eriksen, H. K. ^{[54
]}

Fabre, O. ^{[51
]}

Finelli, F. ^{[41
,43
]}

Forni, O. ^{[9
,81
]}

Frailis, M. ^{[40
]}

Franceschi, E. ^{[41
]}

Galeotta, S. ^{[40
]}

Galli, S. ^{[51
]}

Ganga, K. ^{[1
]}

Giard, M. ^{[9
,81
]}

机构：

[1] Univ Paris Diderot, APC, Observ Paris, Sorbonne Paris Cite,CNRS IN2P3,CEA IRFU, F-75205 Paris 13, France

[2] African Inst Math Sci, ZA-7950 Cape Town, South Africa

[3] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy

[4] Agenzia Spaziale Italiana, I-00198 Rome, Italy

[5] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[6] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[7] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago, Chile

[8] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

[9] IRAP, CNRS, F-31028 Toulouse 4, France

[10] CALTECH, Pasadena, CA 91125 USA

[11] CEFCA, Teruel 44001, Spain

[12] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[13] CSIC, E-28049 Madrid, Spain

[14] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[15] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[16] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[17] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain

[18] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[19] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[20] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA

[21] UCL, Dept Phys & Astron, London WC1E 6BT, England

[22] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[23] Univ Helsinki, Dept Phys, Helsinki, Finland

[24] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[25] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[26] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[27] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[28] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[29] Univ Milan, Dipartimento Fis, Milan, Italy

[30] Univ Trieste, Dipartimento Fis, Trieste, Italy

[31] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy

[32] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[33] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

[34] ESO Vitacura, European So Observ, Santiago, Chile

[35] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain

[36] European Space Agcy, Estec, NL-2201 Noordwijk, Netherlands

[37] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland

[38] Osserv Astron Padova, INAF, Padua, Italy

[39] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[40] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

[41] INAF IASF Bologna, Bologna, Italy

[42] INAF IASF Milano, Milan, Italy

[43] INFN, Sez Bologna, I-40126 Bologna, Italy

[44] Univ Roma La Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy

[45] INFN Natl Inst Nucl Phys, I-34127 Trieste, Italy

[46] Univ Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France

[47] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England

[48] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA

[49] Inst Univ France, F-75005 Paris, France

[50] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 580卷

关键词：

cosmology: observations; cosmic background radiation; cosmological parameters; atomic data; FINE-STRUCTURE CONSTANT; BARYON ACOUSTIC-OSCILLATIONS; TIME-VARIATION; PHYSICAL CONSTANTS; ANISOTROPY; ALPHA; TELESCOPE; RADIATION; UNIVERSE; M(E);

D O I：

10.1051/0004-6361/201424496

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Any variation in the fundamental physical constants, more particularly in the fine structure constant, a, or in the mass of the electron, me, affects the recombination history of the Universe and cause an imprint on the cosmic microwave background angular power spectra. We show that the Planck data allow one to improve the constraint on the time variation of the fine structure constant at redshift z - 10(3) by about a factor of 5 compared to WMAP data, as well as to break the degeneracy with the Hubble constant, H-0. In addition to a, we can set a constraint on the variation in the mass of the electron, me, and in the simultaneous variation of the two constants. We examine in detail the degeneracies between fundamental constants and the cosmological parameters, in order to compare the limits obtained from Planck and WMAP and to determine the constraining power gained by including other cosmological probes. We conclude that independent time variations of the fine structure constant and of the mass of the electron are constrained by Planck to Delta alpha/alpha = (3.6 +/- 3.7) x 10(-3) and Delta m(e)/m(e) = (4 +/- 11) x 10(-3) at the 68% confidence level. We also investigate the possibility of a spatial variation of the fine structure constant. The relative amplitude of a dipolar spatial variation in a (corresponding to a gradient across our Hubble volume) is constrained to be delta alpha/alpha = (-2.4 +/- 3.7) x 10(-2).

引用

页数：25

共 117 条

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