Planck 2018 results: XI. Polarized dust foregrounds

被引：106

作者：

Akrami, Y. ^{[46
,48
]}

Ashdown, M. ^{[4
,55
]}

Aumont, J. ^{[83
]}

Baccigalupi, C. ^{[69
]}

Ballardini, M. ^{[17
,32
]}

Banday, A. J. ^{[7
,83
]}

Barreiro, R. B. ^{[50
]}

Bartolo, N. ^{[22
,51
]}

Basak, S. ^{[75
]}

Benabed, K. ^{[44
,82
]}

Bernard, J. -P. ^{[7
,83
]}

Bersanelli, M. ^{[25
,36
]}

Bielewicz, P. ^{[7
,66
,69
]}

Bond, J. R. ^{[6
]}

Borrill, J. ^{[10
,80
]}

Bouchet, F. R. ^{[44
,78
]}

Boulanger, F. ^{[43
,44
,77
]}

Bracco, A. ^{[45
,67
,68
]}

Bucher, M. ^{[2
,5
]}

Burigana, C. ^{[23
,35
,37
]}

Calabrese, E. ^{[73
]}

Cardoso, J. -F. ^{[44
]}

Carron, J. ^{[18
]}

Chiang, H. C. ^{[5
,20
]}

Combet, C. ^{[58
]}

Crill, B. P. ^{[9
,52
]}

de Bernardis, P. ^{[24
]}

de Zotti, G. ^{[33
,69
]}

Delabrouille, J. ^{[2
]}

Delouis, J. -M. ^{[44
,82
]}

Di Valentino, E. ^{[53
]}

Dickinson, C. ^{[53
]}

Diego, J. M. ^{[50
]}

Ducout, A. ^{[56
]}

Dupac, X. ^{[28
]}

Efstathiou, G. ^{[47
,55
]}

Elsner, F. ^{[63
]}

Ensslin, T. A. ^{[63
]}

Falgarone, E. ^{[77
]}

Fantaye, Y. ^{[3
,15
]}

Ferriere, K. ^{[7
,83
]}

Finelli, F. ^{[32
,37
]}

Forastieri, F. ^{[23
,38
]}

Frailis, M. ^{[34
]}

Fraisse, A. A. ^{[20
]}

Franceschi, E. ^{[32
]}

Frolov, A. ^{[76
]}

Galeotta, S. ^{[34
]}

Galli, S. ^{[54
]}

Ganga, K. ^{[2
]}

机构：

[1] Univ Paris Saclay, Univ Paris Diderot, Sorbonne Paris Cite, AIM,CEA,CNRS, F-91191 Gif Sur Yvette, France

[2] Univ Paris Diderot, AstroParticule & Cosmol, CNRS, IN2P3,CEA Irfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France

[3] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa

[4] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England

[5] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa

[6] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada

[7] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[8] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

[9] CALTECH, Pasadena, CA 91125 USA

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

[11] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland

[12] Univ La Laguna ULL, Dept Astrofis, Tenerife 38206, Spain

[13] Univ Oviedo, Dept Fis, C Federico Garcia Lorca 18, Oviedo, Spain

[14] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands

[15] Univ Stellenbosch, Dept Math, ZA-7602 Stellenbosch, South Africa

[16] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada

[17] Univ Western Cape, Dept Phys & Astron, ZA-7535 Cape Town, South Africa

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

[19] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki, Finland

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

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

[22] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy

[23] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy

[24] Univ Roma La Sapienza, Dipartimento Fis, Ple A Moro 2, Rome, Italy

[25] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy

[26] Univ Trieste, Dipartimento Fis, Via A Valerio 2, Trieste, Italy

[27] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, Rome, Italy

[28] European Space Agcy, ESAC, Planck Sci Off, Caminobajo Castillo S-N, Madrid, Spain

[29] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[30] INFN, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy

[31] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki, Finland

[32] Ist Nazl Astrofis Osservatorio Astrofis & Sci Spa, INAF OAS Bologna, Area Ric, CNR, Via Gobetti 101, I-40129 Bologna, Italy

[33] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, Padua, Italy

[34] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, Trieste, Italy

[35] Ist Radioastron, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy

[36] IASF Milano, INAF, Via E Bassini 15, Milan, Italy

[37] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[38] INFN, Sez Ferrara, Via Saragat 1, I-44122 Ferrara, Italy

[39] INFN, Sez Milano, Via Celoria 16, Milan, Italy

[40] Univ Roma Sapienza, INFN, Sez Roma 1, Piazzale Aldo Moro 2, I-00185 Rome, Italy

[41] Univ Roma Tor Vergata, INFN, Sez Roma 2, Via Ric Sci 1, Rome, Italy

[42] Imperial Coll London, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England

[43] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France

[44] CNRS, UMR7095, Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France

[45] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France

[46] Leiden Univ, Inst Lorentz, POB 9506, NL-2300 RA Leiden, Netherlands

[47] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[48] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway

[49] Inst Astrofis Canarias, C Via Lactea S-N, Tenerife, Spain

[50] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, Santander, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 641卷

基金：

英国科学技术设施理事会;

关键词：

dust; extinction; ISM: magnetic fields; ISM: structure; cosmic background radiation; polarization; submillimeter: diffuse background; PROBE WMAP OBSERVATIONS; STATISTICAL PROPERTIES; INFLATIONARY UNIVERSE; COMPONENT SEPARATION; MICROWAVE EMISSION; INTERSTELLAR DUST; MAGNETIC-FIELDS; POWER SPECTRA; RADIATION; HELICITY;

D O I：

10.1051/0004-6361/201832618

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The study of polarized dust emission has become entwined with the analysis of the cosmic microwave background (CMB) polarization in the quest for the curl-like B-mode polarization from primordial gravitational waves and the low-multipole E-mode polarization associated with the reionization of the Universe. We used the new Planck PR3 maps to characterize Galactic dust emission at high latitudes as a foreground to the CMB polarization and use end-to-end simulations to compute uncertainties and assess the statistical significance of our measurements. We present PlanckEE, BB, and TE power spectra of dust polarization at 353 GHz for a set of six nested high-Galactic-latitude sky regions covering from 24 to 71% of the sky. We present power-law fits to the angular power spectra, yielding evidence for statistically significant variations of the exponents over sky regions and a difference between the values for the EE and BB spectra, which for the largest sky region are alpha (EE)=-2.42 +/- 0.02 and alpha (BB)=-2.54 +/- 0.02, respectively. The spectra show that the TE correlation and E/B power asymmetry discovered by Planck extend to low multipoles that were not included in earlier Planck polarization papers due to residual data systematics. We also report evidence for a positive TB dust signal. Combining data from Planck and WMAP, we have determined the amplitudes and spectral energy distributions (SEDs) of polarized foregrounds, including the correlation between dust and synchrotron polarized emission, for the six sky regions as a function of multipole. This quantifies the challenge of the component-separation procedure that is required for measuring the low-l reionization CMB E-mode signal and detecting the reionization and recombination peaks of primordial CMB B modes. The SED of polarized dust emission is fit well by a single-temperature modified black-body emission law from 353 GHz to below 70 GHz. For a dust temperature of 19.6 K, the mean dust spectral index for dust polarization is beta (P)(d) = 1.53 +/- 0.02 beta d P = 1.53 +/- 0.02 . The difference between indices for polarization and total intensity is beta (P)(d)-beta (I)(d) = 0.05 +/- 0.03 beta d P - beta d I =0.05 +/- 0.03 . By fitting multi-frequency cross-spectra between Planck data at 100, 143, 217, and 353 GHz, we examine the correlation of the dust polarization maps across frequency. We find no evidence for a loss of correlation and provide lower limits to the correlation ratio that are tighter than values we derive from the correlation of the 217- and 353 GHz maps alone. If the Planck limit on decorrelation for the largest sky region applies to the smaller sky regions observed by sub-orbital experiments, then frequency decorrelation of dust polarization might not be a problem for CMB experiments aiming at a primordial B-mode detection limit on the tensor-to-scalar ratio r similar or equal to 0.01 at the recombination peak. However, the Planck sensitivity precludes identifying how difficult the component-separation problem will be for more ambitious experiments targeting lower limits on r.

引用

页数：33

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