Planck 2018 results: IV. Diffuse component separation

被引：262

作者：

Akrami, Y. ^{[14
,51
,53
]}

Ashdown, M. ^{[5
,60
]}

Aumont, J. ^{[86
]}

Baccigalupi, C. ^{[72
]}

Ballardini, M. ^{[20
,37
]}

Banday, A. J. ^{[8
,86
]}

Barreiro, R. B. ^{[55
]}

Bartolo, N. ^{[26
,56
]}

Basak, S. ^{[78
]}

Benabed, K. ^{[50
,85
]}

Bersanelli, M. ^{[29
,41
]}

Bielewicz, P. ^{[70
,71
,72
]}

Bond, J. R. ^{[7
]}

Borrill, J. ^{[12
,83
]}

Bouchet, F. R. ^{[50
,81
]}

Boulanger, F. ^{[49
,50
,80
]}

Bucher, M. ^{[2
,6
]}

Burigana, C. ^{[27
,40
,43
]}

Calabrese, E. ^{[76
]}

Cardoso, J. -F. ^{[50
]}

Carron, J. ^{[21
]}

Casaponsa, B. ^{[55
]}

Challinor, A. ^{[11
,52
,60
]}

Colombo, L. P. L. ^{[29
]}

Combet, C. ^{[62
]}

Crill, B. P. ^{[10
,57
]}

Cuttaia, F. ^{[37
]}

de Bernardis, P. ^{[28
]}

de Rosa, A. ^{[37
]}

de Zotti, G. ^{[38
]}

Delabrouille, J. ^{[2
]}

Delouis, J. -M. ^{[50
,85
]}

Di Valentino, E. ^{[58
]}

Dickinson, C. ^{[58
]}

Diego, J. M. ^{[55
]}

Donzelli, S. ^{[29
,41
]}

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

Ducout, A. ^{[61
]}

Dupac, X. ^{[32
]}

Efstathiou, G. ^{[52
,60
]}

Elsner, F. ^{[67
]}

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

Eriksen, H. K. ^{[53
]}

Falgarone, E. ^{[80
]}

Fernandez-Cobos, R. ^{[55
]}

Finelli, F. ^{[37
,43
]}

Forastieri, F. ^{[27
,44
]}

Frailis, M. ^{[39
]}

Fraisse, A. A. ^{[23
]}

Franceschi, E. ^{[37
]}

机构：

[1] Univ Paris Diderot, Univ Paris Saclay, CNRS, AIM,CEA,Sorbonne Paris Cite, 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] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

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

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

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

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

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

[10] CALTECH, Pasadena, CA 91125 USA

[11] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England

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

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

[14] PSL Res Univ, CNRS, Ecole Normale Super, Dept Phys, 24 Rue Lhomond, F-75005 Paris, France

[15] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

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

[17] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, Rua Matao 1371, Sao Paulo, Brazil

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

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

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

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

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

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

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

[25] Univ Illinois, Dept Phys, 1110 West Green St, Urbana, IL USA

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

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

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

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

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

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

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

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

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

[35] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA

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

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

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

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

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

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

[42] CNAF, INFN, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

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

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

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

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

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 641卷

基金：

欧盟地平线“2020”; 英国科学技术设施理事会;

关键词：

ISM: general; cosmology: observations; cosmic background radiation; diffuse radiation; Galaxy: general; POWER SPECTRUM; FULL-SKY; CMB; MAP; VARIANCE; TEMPLATE; GHZ;

D O I：

10.1051/0004-6361/201833881

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present full-sky maps of the cosmic microwave background (CMB) and polarized synchrotron and thermal dust emission, derived from the third set of Planck frequency maps. These products have significantly lower contamination from instrumental systematic effects than previous versions. The methodologies used to derive these maps follow closely those described in earlier papers, adopting four methods (Commander, NILC, SEVEM, and SMICA) to extract the CMB component, as well as three methods (Commander, GNILC, and SMICA) to extract astrophysical components. Our revised CMB temperature maps agree with corresponding products in the Planck 2015 delivery, whereas the polarization maps exhibit significantly lower large-scale power, reflecting the improved data processing described in companion papers; however, the noise properties of the resulting data products are complicated, and the best available end-to-end simulations exhibit relative biases with respect to the data at the few percent level. Using these maps, we are for the first time able to fit the spectral index of thermal dust independently over 3 degrees regions. We derive a conservative estimate of the mean spectral index of polarized thermal dust emission of beta (d)=1.55 +/- 0.05, where the uncertainty marginalizes both over all known systematic uncertainties and different estimation techniques. For polarized synchrotron emission, we find a mean spectral index of beta (s)=-3.1 +/- 0.1, consistent with previously reported measurements. We note that the current data processing does not allow for construction of unbiased single-bolometer maps, and this limits our ability to extract CO emission and correlated components. The foreground results for intensity derived in this paper therefore do not supersede corresponding Planck 2015 products. For polarization the new results supersede the corresponding 2015 products in all respects.

引用

页数：74

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