Euclid preparation I. The Euclid Wide Survey

被引：192

作者：

Scaramella, R. ^{[1
,2
]}

Amiaux, J. ^{[3
]}

Mellier, Y. ^{[4
,5
]}

Burigana, C. ^{[6
,7
,8
]}

Carvalho, C. S. ^{[9
]}

Cuillandre, J-C ^{[3
]}

Da Silva, A. ^{[10
,11
]}

Derosa, A. ^{[12
]}

Dinis, J. ^{[10
,11
]}

Maiorano, E. ^{[12
]}

Maris, M. ^{[13
,14
]}

Tereno, I ^{[9
,10
]}

Laureijs, R. ^{[15
]}

Boenke, T. ^{[15
]}

Buenadicha, G. ^{[16
]}

Dupac, X. ^{[16
]}

Venancio, L. M. Gaspar ^{[15
]}

Gomez-Alvarez, P. ^{[16
,17
]}

Hoar, J. ^{[16
]}

Alvarez, J. Lorenzo ^{[15
]}

Racca, G. D. ^{[15
]}

Saavedra-Criado, G. ^{[15
]}

Schwartz, J. ^{[18
]}

Vavrek, R. ^{[16
]}

Schirmer, M. ^{[19
]}

Aussel, H. ^{[3
,5
]}

Azzollini, R. ^{[20
]}

Cardone, V. F. ^{[1
,2
]}

Cropper, M. ^{[20
]}

Ealet, A. ^{[21
]}

Garilli, B. ^{[22
]}

Gillard, W. ^{[23
]}

Granett, B. R. ^{[24
]}

Guzzo, L. ^{[24
,25
,26
]}

Hoekstra, H. ^{[27
]}

Jahnke, K. ^{[19
]}

Kitching, T. ^{[20
]}

Maciaszek, T. ^{[28
]}

Meneghetti, M. ^{[12
,29
]}

Miller, L. ^{[30
]}

Nakajima, R. ^{[31
]}

Niemi, S. M. ^{[15
]}

Pasian, F. ^{[14
]}

Percival, W. J. ^{[32
,33
,34
]}

Pottinger, S. ^{[20
]}

Sauvage, M. ^{[3
]}

Scodeggio, M. ^{[22
]}

Wachter, S. ^{[35
]}

Zacchei, A. ^{[14
]}

Aghanim, N. ^{[36
]}

机构：

[1] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy

[2] Ist Nazl Fis Nucl, Dipartimento Fis, Sez Roma, Piazzale Aldo Moro 2,Edificio G Marconi, I-00185 Rome, Italy

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

[4] CEA Saclay, DFR IRFU, Serv Astrophys, Bat 709, F-91191 Gif Sur Yvette, France

[5] Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France

[6] INFN Bologna, Via Irnerio 46, I-40126 Bologna, Italy

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

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

[9] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1349018 Lisbon, Portugal

[10] Univ Lisbon, Fac Ciencias, Dept Fis, Edificio C8, P-1749016 Lisbon, Portugal

[11] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1749016 Lisbon, Portugal

[12] INAF Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

[13] Inst Fundamental Phys Universe, IFPU, Via Beirut 2, I-34151 Trieste, Italy

[14] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy

[15] European Space Agcy ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[16] ESAC ESA, Camino Bajo del Castillo S-N, Madrid 28692, Spain

[17] Fractal SLNE, Calle Tulipan 2,Portal 13 1A, Las Rozas De Madrid 28231, Spain

[18] European Space Agcy ESOC, Robert Bosch Str 5, D-64293 Darmstadt, Germany

[19] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[20] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[21] Univ Lyon, Univ Claude Bernard Lyon 1, IP2I Lyon, CNRS IN2P3,UMR 5822, F-69622 Villeurbanne, France

[22] INAF IASF Milano, Via Alfonso Corti 12, I-20133 Milan, Italy

[23] Aix Marseille Univ, CPPM, CNRS IN2P3, Marseille, France

[24] INAF Osservatorio Astron Brera, Via Brera 28, I-20122 Milan, Italy

[25] Univ Milan, Dipartimento Fis Aldo Pontremoli, Via Celoria 16, I-20133 Milan, Italy

[26] Ist Nazl Fis Nucl, Sez Milano, Via Celoria 16, I-20133 Milan, Italy

[27] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

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

[29] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[30] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England

[31] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[32] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada

[33] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[34] Univ Waterloo, Ctr Astrophys, Waterloo, ON N2L 3G1, Canada

[35] Carnegie Observ, Pasadena, CA 91101 USA

[36] Univ Paris Saclay, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France

[37] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[38] INAF Osservatorio Astron Padova, Via Osservatorio 5, I-35122 Padua, Italy

[39] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

[40] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[41] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy

[42] Ist Nazl Fis Nucl, Sez Roma Tre, Via Vasca Navale 84, I-00146 Rome, Italy

[43] Roma Tre Univ, Dept Math & Phys, Via Vasca Navale 84, I-00146 Rome, Italy

[44] Univ Toulouse, Inst Rech Astrophys & Planetol IRAP, CNRS, UPS,CNES, 14 Av Edouard Belin, F-31400 Toulouse, France

[45] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy

[46] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada

[47] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, Barcelona 08193, Spain

[48] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain

[49] Inst Estudis Espacials Catalunya IEEC, Carrer Gran Capita 2-4, Barcelona 08034, Spain

[50] Univ Federico II, Dept Phys E Pancini, Via Cinthia 6, I-80126 Naples, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 662卷

基金：

美国国家航空航天局;

关键词：

space vehicles; surveys; methods; numerical; dark energy; dark matter; POWER SPECTRUM; SPACE MISSION; SKY; MAGNITUDES; BRIGHTNESS; UNIVERSE; MODEL; LSST;

D O I：

10.1051/0004-6361/202141938

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 deg(2) of extragalactic sky in six years. The wide-field telescope and instruments are optimised for pristine point spread function and reduced stray light, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, deep fields, and calibration fields, as well as spacecraft movements followed by Euclid as it operates in a step-and-stare mode from its orbit around the Lagrange point L2. Each EWS pointing has four dithered frames; we simulated the dither pattern at the pixel level to analyse the effective coverage. We used up-to-date models for the sky background to define the Euclid region-of-interest (RoI). The building of the reference survey is highly constrained from calibration cadences, spacecraft constraints, and background levels; synergies with ground-based coverage were also considered. Via purposely built software, we first generated a schedule for the calibrations and deep fields observations. On a second stage, the RoI was tiled and scheduled with EWS observations, using an algorithm optimised to prioritise the best sky areas, produce a compact coverage, and ensure thermal stability. The result is the optimised reference survey RSD_2021A, which fulfils all constraints and is a good proxy for the final solution. The current EWS covers approximate to 14 & x2006;500 deg(2). The limiting AB magnitudes (5 sigma point-like source) achieved in its footprint are estimated to be 26.2 (visible band I-E) and 24.5 (for near infrared bands Y-E, J(E), H-E); for spectroscopy, the H alpha line flux limit is 2 x 10(-16) erg(-1) cm(-2) s(-1) at 1600 nm; and for diffuse emission, the surface brightness limits are 29.8 (visible band) and 28.4 (near infrared bands) mag arcsec(-2).

引用

页数：41

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