Planck 2018 results: III. High Frequency Instrument data processing and frequency maps

被引：163

作者：

Aghanim, N. ^{[48
]}

Akrami, Y. ^{[50
,52
]}

Ashdown, M. ^{[6
,59
]}

Aumont, J. ^{[88
]}

Baccigalupi, C. ^{[73
]}

Ballardini, M. ^{[20
,36
]}

Banday, A. J. ^{[9
,88
]}

Barreiro, R. B. ^{[54
]}

Bartolo, N. ^{[25
,55
]}

Basak, S. ^{[80
]}

Benabed, K. ^{[49
,87
]}

Bernard, J. -P. ^{[9
,88
]}

Bersanelli, M. ^{[28
,40
]}

Bielewicz, P. ^{[9
,72
,73
]}

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

Borrill, J. ^{[13
,85
]}

Bouchet, F. R. ^{[49
,82
]}

Boulanger, F. ^{[48
,49
,62
]}

Bucher, M. ^{[3
,7
]}

Burigana, C. ^{[26
,39
,42
]}

Calabrese, E. ^{[77
]}

Cardoso, J. -F. ^{[49
]}

Carron, J. ^{[21
]}

Challinor, A. ^{[12
,51
,59
]}

Chiang, H. C. ^{[7
,23
]}

Colombo, L. P. L. ^{[28
]}

Combet, C. ^{[64
]}

Couchot, F. ^{[60
]}

Crill, B. P. ^{[11
,56
]}

Cuttaia, F. ^{[36
]}

de Bernardis, P. ^{[27
]}

de Rosa, A. ^{[36
]}

de Zotti, G. ^{[37
,73
]}

Delabrouille, J. ^{[3
]}

Delouis, J. -M. ^{[49
,87
]}

Di Valentino, E. ^{[57
]}

Diego, J. M. ^{[54
]}

Dore, O. ^{[11
,56
]}

Douspis, M. ^{[48
]}

Ducout, A. ^{[47
,49
]}

Dupac, X. ^{[31
]}

Efstathiou, G. ^{[51
,59
]}

Elsner, F. ^{[69
]}

Ensslin, T. A. ^{[69
]}

Eriksen, H. K. ^{[52
]}

Falgarone, E. ^{[61
]}

Fantaye, Y. ^{[4
,18
]}

Finelli, F. ^{[36
,42
]}

Frailis, M. ^{[38
]}

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

机构：

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

[2] Univ Paris Diderot, AIM, Sorbonne Paris Cite, F-91191 Gif Sur Yvette, France

[3] 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

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

[5] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

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

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

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

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

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

[11] CALTECH, Pasadena, CA 91125 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[31] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo del Castillo S-N, Madrid, Spain

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 641卷

关键词：

cosmology: observations; cosmic background radiation; surveys; methods: data analysis; LATITUDE MOLECULAR GAS; SKY MAPS; SEPARATION; SPECTRUM; MODEL;

D O I：

10.1051/0004-6361/201832909

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This paper presents the High Frequency Instrument (HFI) data processing procedures for the Planck 2018 release. Major improvements in mapmaking have been achieved since the previous Planck 2015 release, many of which were used and described already in an intermediate paper dedicated to the Planck polarized data at low multipoles. These improvements enabled the first significant measurement of the reionization optical depth parameter using Planck-HFI data. This paper presents an extensive analysis of systematic effects, including the use of end-to-end simulations to facilitate their removal and characterize the residuals. The polarized data, which presented a number of known problems in the 2015 Planck release, are very significantly improved, especially the leakage from intensity to polarization. Calibration, based on the cosmic microwave background (CMB) dipole, is now extremely accurate and in the frequency range 100-353 GHz reduces intensity-to-polarization leakage caused by calibration mismatch. The Solar dipole direction has been determined in the three lowest HFI frequency channels to within one arc minute, and its amplitude has an absolute uncertainty smaller than 0.35 mu K, an accuracy of order 10(-4). This is a major legacy from the Planck HFI for future CMB experiments. The removal of bandpass leakage has been improved for the main high-frequency foregrounds by extracting the bandpass-mismatch coefficients for each detector as part of the mapmaking process; these values in turn improve the intensity maps. This is a major change in the philosophy of "frequency maps", which are now computed from single detector data, all adjusted to the same average bandpass response for the main foregrounds. End-to-end simulations have been shown to reproduce very well the relative gain calibration of detectors, as well as drifts within a frequency induced by the residuals of the main systematic effect (analogue-to-digital convertor non-linearity residuals). Using these simulations, we have been able to measure and correct the small frequency calibration bias induced by this systematic effect at the 10(-4) level. There is no detectable sign of a residual calibration bias between the first and second acoustic peaks in the CMB channels, at the 10(-3) level.

引用

页数：50

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