Planck intermediate results XLVII. Planck constraints on reionization history

被引：350

作者：

Adam, R. ^{[69
]}

Aghanim, N. ^{[54
]}

Ashdown, M. ^{[8
,64
]}

Aumont, J. ^{[54
]}

Baccigalupi, C. ^{[78
]}

Ballardini, M. ^{[29
,46
,49
]}

Banday, A. J. ^{[11
,87
]}

Barreiro, R. B. ^{[59
]}

Bartolo, N. ^{[28
,60
]}

Basak, S. ^{[62
]}

Battye, R. ^{[62
]}

Benabed, K. ^{[55
,86
]}

Bernard, J. -P. ^{[11
,87
]}

Bersanelli, M. ^{[32
,47
]}

Bielewicz, P. ^{[11
,75
,78
]}

Bock, J. J. ^{[12
,61
]}

Bonaldi, A. ^{[62
]}

Bonavera, L. ^{[17
]}

Bond, J. R. ^{[10
]}

Borrill, J. ^{[13
,84
]}

Bouchet, F. R. ^{[55
,82
]}

Boulanger, F. ^{[54
]}

Bucher, M.

Burigana, C. ^{[30
,46
,49
]}

Calabrese, E. ^{[2
,3
]}

Cardoso, J. -F. ^{[55
,67
,68
]}

Carron, J. ^{[22
]}

Chiang, H. C. ^{[9
,24
]}

Colombo, L. P. L. ^{[20
,61
]}

Combet, C. ^{[69
]}

Comis, B. ^{[69
]}

Couchot, F. ^{[65
]}

Coulais, A. ^{[66
]}

Crill, B. P. ^{[12
,61
]}

Curto, A. ^{[8
,59
,64
]}

Cuttaia, F. ^{[46
]}

Davis, R. J. ^{[62
]}

de Bernardis, P. ^{[31
]}

de Rosa, A. ^{[46
]}

de Zotti, G. ^{[43
,78
]}

Delabrouille, J.

Di Valentino, E. ^{[55
,82
]}

Dickinson, C. ^{[62
]}

Diego, J. M. ^{[59
]}

Dore, O. ^{[12
,61
]}

Douspis, M. ^{[54
]}

Ducout, A. ^{[32
,55
]}

Dupac, X. ^{[36
]}

Elsner, F. ^{[21
,55
,86
]}

Ensslin, T. A. ^{[73
]}

机构：

[1] Univ Paris Diderot, Sorbonne Paris Cite,CEA lrfu, Observ Paris,CNRS IN2P3, APC AstroParticule & Cosmol, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland

[3] Dept Radio Sci & Engn, Aalto 00076, Finland

[4] African Inst Math Sci, ZA-7945 Cape Town, South Africa

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

[6] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[7] Aix Marseille Univ, Ctr Phys Theor, F-13288 Marseille, France

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

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

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

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

[12] CALTECH, Pasadena, CA 91125 USA

[13] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[14] Tech Univ Denmark, Space Natl Space Inst, DTU, Lyngby, Denmark

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

[16] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

[17] Univ Oviedo, Dept Fis, Oviedo 33003, Spain

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

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

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

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

[22] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England

[23] Univ Helsinki, Dept Phys, Helsinki 00560, Finland

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

[25] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[26] Univ Calif Davis, Dept Phys, Davis, CA 95064 USA

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

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

[29] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy

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

[31] Univ Roma La Sapienza, Dipartimento Fis, I-00133 Rome, Italy

[32] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[33] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

[34] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy

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

[36] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain

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

[38] Gran Sasso Sci Inst, INFN, I-67100 Laquila, Italy

[39] HGSFP, D-69120 Heidelberg, Germany

[40] Heidelberg Univ, Dept Theoret Phys, D-69120 Heidelberg, Germany

[41] Haverford Coll, Dept Astron, Haverford, PA 19041 USA

[42] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki 00560, Finland

[43] INAF Osservatorio Astron Padova, I-35131 Padua, Italy

[44] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[45] INAF Osservatorio Astron Trieste, I-34127 Trieste, Italy

[46] INAF IASF Bologna, I-40127 Bologna, Italy

[47] INAF IASF Milano, I-20133 Milan, Italy

[48] INFN CNAF, I-40127 Bologna, Italy

[49] INFN, Sez Bologna, I-40127 Bologna, Italy

[50] INFN, Sez Ferrara, I-44122 Ferrara, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 596卷

关键词：

cosmic background radiation; dark ages; reionization; first stars; polarization; PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPIES; STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; LY-ALPHA-EMITTERS; COSMIC REIONIZATION; INTERGALACTIC MEDIUM; LUMINOSITY FUNCTION; NEUTRAL HYDROGEN; OPTICAL DEPTH;

D O I：

10.1051/0004-6361/201628897

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate constraints on cosmic reionization extracted from the Planck cosmic microwave background (CMB) data. We combine the Planck CMB anisotropy data in temperature with the low-multipole polarization data to fit Lambda CDM models with various parameterizations of the reionization history. We obtain a Thomson optical depth tau = 0.058 +/- 0.012 for the commonly adopted instantaneous reionization model. This confirms, with data solely from CMB anisotropies, the low value suggested by combining Planck 2015 results with other data sets, and also reduces the uncertainties. We reconstruct the history of the ionization fraction using either a symmetric or an asymmetric model for the transition between the neutral and ionized phases. To determine better constraints on the duration of the reionization process, we also make use of measurements of the amplitude of the kinetic Sunyaev-Zeldovich (kSZ) effect using additional information from the high-resolution Atacama Cosmology Telescope and South Pole Telescope experiments. The average redshift at which reionization occurs is found to lie between z = 7.8 and 8.8, depending on the model of reionization adopted. Using kSZ constraints and a redshift-symmetric reionization model, we find an upper limit to the width of the reionization period of Delta z < 2.8. In all cases, we find that the Universe is ionized at less than the 10% level at redshifts above z similar or equal to 10. This suggests that an early onset of reionization is strongly disfavoured by the Planck data. We show that this result also reduces the tension between CMB-based analyses and constraints from other astrophysical sources.

引用

页数：19

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