COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE

被引：127

作者：

Zahn, O. ^{[1
,2
]}

Reichardt, C. L.

Shaw, L. ^{[3
]}

Lidz, A. ^{[4
]}

Aird, K. A.

Benson, B. A. ^{[5
,6
]}

Bleem, L. E. ^{[5
,7
]}

Carlstrom, J. E. ^{[5
,6
,7
,8
,9
]}

Chang, C. L. ^{[5
,6
,9
]}

Cho, H. M. ^{[10
]}

Crawford, T. M. ^{[5
,8
]}

Crites, A. T. ^{[5
,8
]}

de Haan, T. ^{[11
]}

Dobbs, M. A. ^{[11
]}

Dore, O. ^{[12
]}

Dudley, J. ^{[11
]}

George, E. M. ^{[3
]}

Halverson, N. W. ^{[13
,14
]}

Holder, G. P. ^{[11
]}

Holzapfel, W. L. ^{[3
]}

Hoover, S. ^{[5
,7
]}

Hou, Z. ^{[15
]}

Hrubes, J. D.

Joy, M. ^{[16
]}

Keisler, R. ^{[5
,7
]}

Knox, L. ^{[15
]}

Lee, A. T. ^{[3
,17
]}

Leitch, E. M. ^{[5
,8
]}

Lueker, M. ^{[12
]}

Luong-Van, D.

McMahon, J. J. ^{[18
]}

Mehl, J. ^{[5
]}

Meyer, S. S. ^{[5
,6
,7
,8
]}

Millea, M. ^{[15
]}

Mohr, J. J. ^{[19
,20
,21
]}

Montroy, T. E. ^{[22
]}

Natoli, T. ^{[5
,7
]}

Padin, S. ^{[5
,8
,12
]}

Plagge, T. ^{[5
,8
]}

Pryke, C. ^{[5
,6
,8
,23
]}

Ruhl, J. E. ^{[22
]}

Schaffer, K. K. ^{[5
,6
,24
]}

Shirokoff, E.

Spieler, H. G.

Staniszewski, Z. ^{[23
]}

Stark, A. A. ^{[25
]}

Story, K. ^{[5
,7
]}

van Engelen, A. ^{[11
]}

Vanderlinde, K. ^{[11
]}

Vieira, J. D. ^{[12
]}

机构：

[1] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA

[2] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[3] Yale Univ, Dept Phys, New Haven, CT 06520 USA

[4] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[5] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[6] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[7] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

[8] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[9] Argonne Natl Lab, Argonne, IL 60439 USA

[10] NIST Quantum Devices Grp, Boulder, CO 80305 USA

[11] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[12] CALTECH, Pasadena, CA 91125 USA

[13] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[14] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[15] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[16] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA

[17] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA

[18] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[19] Univ Munich, Dept Phys, D-81679 Munich, Germany

[20] Excellence Cluster Universe, D-85748 Garching, Germany

[21] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[22] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA

[23] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA

[24] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA

[25] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 756卷 / 01期

基金：

美国国家科学基金会;

关键词：

cosmology: theory; intergalactic medium; large-scale structure of universe; PROBE WMAP OBSERVATIONS; LY-ALPHA EMITTERS; RADIATIVE-TRANSFER SIMULATIONS; NEUTRAL HYDROGEN; BUBBLE-GROWTH; HII-REGIONS; IONIZING EMISSIVITY; POWER SPECTRA; QUASAR; EPOCH;

D O I：

10.1088/0004-637X/756/1/65

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The epoch of reionization is a milestone of cosmological structure formation, marking the birth of the first objects massive enough to yield large numbers of ionizing photons. However, the mechanism and timescale of reionization remain largely unknown. Measurements of the cosmic microwave background (CMB) Doppler effect from ionizing bubbles embedded in large-scale velocity streams-known as the patchy kinetic Sunyaev-Zel'dovich (kSZ) effect-can be used to constrain the duration of reionization. When combined with large-scale CMB polarization measurements, the evolution of the ionized fraction, (x) over bar (e), can be inferred. Using new multi-frequency data from the South Pole Telescope (SPT), we show that the ionized fraction evolved relatively rapidly. For our basic foreground model, we find the kSZ power sourced by reionization at l = 3000 to be D-3000(patchy) <= 2.1 mu K-2 at 95% confidence. Using reionization simulations, we translate this to a limit on the duration of reionization of Delta z equivalent to z((x) over bare-0.20) - z((x) over bare-0.99) <= 4.4 (95% confidence). We find that this constraint depends on assumptions about the angular correlation between the thermal SZ power and the cosmic infrared background (CIB). Introducing the degree of correlation as a free parameter, we find that the limit on kSZ power weakens to D-3000(patchy) <= 4.9 mu K-2, implying Delta z <= 7.9 (95% confidence). We combine the SPT constraint on the duration of reionization with the Wilkinson Microwave Anisotropy Probe measurement of the integrated optical depth to probe the cosmic ionization history. We find that reionization ended with 95% confidence at z > 7.2 under the assumption of no tSZ-CIB correlation, and z > 5.8 when correlations are allowed. Improved constraints from the full SPT data set in conjunction with upcoming Herschel and Planck data should detect extended reionization at >95% confidence provided Delta z >= 2. These CMB observations complement other observational probes of the epoch of reionization such as the redshifted 21 cm line and narrowband surveys for Ly alpha-emitting galaxies.

引用

页数：15

共 111 条

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