Euclid Preparation: XIV. The Complete Calibration of the Color-Redshift Relation (C3R2) Survey: Data Release 3
Euclid Collaboration, S. A. Stanford, D. Masters, B. Darvish, D. Stern, J. G. Cohen, P. Capak, N. Hernitschek, I. Davidzon, J. Rhodes, D. B. Sanders, B. Mobashe… 展开作者
Euclid Collaboration, S. A. Stanford, D. Masters, B. Darvish, D. Stern, J. G. Cohen, P. Capak, N. Hernitschek, I. Davidzon, J. Rhodes, D. B. Sanders, B. Mobasher, F. J. Castander, S. Paltani, N. Aghanim, A. Amara, N. Auricchio, A. Balestra, R. Bender, C. Bodendorf, D. Bonino, E. Branchini, J. Brinchmann, V. Capobianco, C. Carbone, J. Carretero, R. Casas, M. Castellano, S. Cavuoti, A. Cimatti, R. Cledassou, C. J. Conselice, L. Corcione, A. Costille, M. Cropper, H. Degaudenzi, M. Douspis, F. Dubath, S. Dusini, P. Fosalba, M. Frailis, E. Franceschi, P. Franzetti, M. Fumana, B. Garilli, C. Giocoli, F. Grupp, S. V. H. Haugan, H. Hoekstra, W. Holmes, F. Hormuth, P. Hudelot, K. Jahnke, A. Kiessling, M. Kilbinger, T. Kitching, B. Kubik, M. Kummel, M. Kunz, H. Kurki-Suonio, R. Laureijs, S. Ligori, P. B. Lilje, I. Lloro, E. Maiorano, O. Marggraf, K. Markovic, R. Massey, M. Meneghetti, G. Meylan, L. Moscardini, S. M. Niemi, C. Padilla, F. Pasian, K. Pedersen, V. Pettorino, S. Pires, M. Poncet, L. Popa, L. Pozzetti, F. Raison, M. Roncarelli, E. Rossetti, R. Saglia, R. Scaramella, P. Schneider, A. Secroun, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, A. N. Taylor, H. I. Teplitz, I. Tereno, R. Toledo-Moreo, E. A. Valentijn, L. Valenziano, G. A. Verdoes Kleijn, Y. Wang, G. Zamorani, J. Zoubian, M. Brescia, G. Congedo, L. Conversi, Y. Copin, S. Kermiche, R. Kohley, E. Medinaceli, S. Mei, M. Moresco, B. Morin, E. Munari, G. Polenta, F. Sureau, P. Tallada Crespí, T. Vassallo, A. Zacchei, S. Andreon, H. Aussel, C. Baccigalupi, A. Balaguera-Antolínez, M. Baldi, S. Bardelli, A. Biviano, E. Borsato, E. Bozzo, C. Burigana, R. Cabanac, S. Camera, A. Cappi, C. S. Carvalho, S. Casas, G. Castignani, C. Colodro-Conde, J. Coupon, H. M. Courtois, J. -G. Cuby, A. Da Silva, S. de la Torre, D. Di Ferdinando, C. A. J. Duncan, X. Dupac, M. Fabricius, M. Farina, S. Farrens, P. G. Ferreira, F. Finelli, P. Flose-Reimberg, S. Fotopoulou, S. Galeotta, K. Ganga, W. Gillard, G. Gozaliasl, J. Graciá-Carpio, E. Keihanen, C. C. Kirkpatrick, V. Lindholm, G. Mainetti, D. Maino, N. Martinet, F. Marulli, M. Maturi, S. Maurogordato, R. B. Metcalf, R. Nakajima, C. Neissner, J. W. Nightingale, A. A. Nucita, L. Patrizii, D. Potter, A. Renzi, G. Riccio, E. Romelli, A. G. Sanchez, D. Sapone, M. Schirmer, M. Schultheis, V. Scottez, L. Stanco, M. Tenti, R. Teyssier, F. Torradeflot, J. Valiviita, M. Viel, L. Whittaker, E. Zucca
备注：
14 pages, 7 figures, 4 tables. Accepted for publication in The Astrophysical Journal Supplement. Survey website with links to the C3R2 redshift catalog and the spectroscopic data hosted by the Keck Observatory Archive can be found at https://sites.google.com/view/c3r2-survey/home
The Complete Calibration of the Color-Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ~ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage IV dark energy projects, particularly Euclid and the Roman Space Telescope, which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B-2019B semesters using the DEIMOS, LRIS, and MOSFIRE multi-object spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < z(phot) < 2.6 range of interest for the Euclid cosmological goals, then with the current data release C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al. 2015) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman.
Euclid is a European Space Agency (ESA) mission 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 in visible and near-infrared bands, covering approximately 15 000 deg2 of the extragalactic sky in six years. Euclid will be equipped with a 1.2 m diameter Silicon Carbide (SiC) mirror telescope feeding two instruments built by the Euclid Consortium: a high-quality panoramic visible imager and a near-infrared photometer and spectrograph. These proceedings briefly descri…
We present a new, updated version of the EuclidEmulator (called EuclidEmulator2), a fast and accurate predictor for the nonlinear correction of the matter power spectrum. Percent-level accurate emulation is now supported in the eight-dimensional parameter space of $w_0w_a$CDM$+\sum m_ν$models between redshift $z=0$ and $z=3$ for spatial scales within the range 0.01 $h$/Mpc $\leq k \leq$ 10 $h$/Mpc. In order to achieve this level of accuracy, we have had to improve the quality of the underlying N-body simulations used as training data: (1) we use self-consistent linear evolution of non-dark mat…
Euclid will be the first space mission to survey most of the extragalactic sky in the 0.95-2.02 $μ$m range, to a 5$σ$ point-source median depth of 24.4 AB mag. This unique photometric data set will find wide use beyond Euclid's core science. In this paper, we present accurate computations of the Euclid Y_E, J_E and H_E passbands used by the Near-Infrared Spectrometer and Photometer (NISP), and the associated photometric system. We pay particular attention to passband variations in the field of view, accounting among others for spatially variable filter transmission, and variations of the angle…
(Abridged) The Euclid mission is expected to discover thousands of z>6 galaxies in three Deep Fields, which together will cover a ~40 deg2 area. However, the limited number of Euclid bands and availability of ancillary data could make the identification of z>6 galaxies challenging. In this work, we assess the degree of contamination by intermediate-redshift galaxies (z=1-5.8) expected for z>6 galaxies within the Euclid Deep Survey. This study is based on ~176,000 real galaxies at z=1-8 in a ~0.7 deg2 area selected from the UltraVISTA ultra-deep survey, and ~96,000 mock galaxies with 25.3$\leq$…
Euclid is an ESA mission 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 (EWS) in visible and near-infrared, covering roughly 15,000 square degrees of extragalactic sky on six years. The wide-field telescope and instruments are optimized for pristine PSF and reduced straylight, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, Deep fields, Auxiliary fields for calibrations, and spacecraf…
The Euclid space telescope will measure the shapes and redshifts of galaxies to reconstruct the expansion history of the Universe and the growth of cosmic structures. Estimation of the expected performance of the experiment, in terms of predicted constraints on cosmological parameters, has so far relied on different methodologies and numerical implementations, developed for different observational probes and for their combination. In this paper we present validated forecasts, that combine both theoretical and observational expertise for different cosmological probes. This is presented to provi…
The accuracy of photometric redshifts (photo-zs) particularly affects the results of the analyses of galaxy clustering with photometrically-selected galaxies (GCph) and weak lensing. In the next decade, space missions like Euclid will collect photometric measurements for millions of galaxies. These data should be complemented with upcoming ground-based observations to derive precise and accurate photo-zs. In this paper, we explore how the tomographic redshift binning and depth of ground-based observations will affect the cosmological constraints expected from Euclid. We focus on GCph and exten…
The combination and cross-correlation of the upcoming $Euclid$ data with cosmic microwave background (CMB) measurements is a source of great expectation since it will provide the largest lever arm of epochs, ranging from recombination to structure formation across the entire past light cone. In this work, we present forecasts for the joint analysis of $Euclid$ and CMB data on the cosmological parameters of the standard cosmological model and some of its extensions. This work expands and complements the recently published forecasts based on $Euclid$-specific probes, namely galaxy clustering, we…
The Complete Calibration of the Color-Redshift Relation survey (C3R2) is a spectroscopic programme designed to empirically calibrate the galaxy color-redshift relation to the Euclid depth (I_E=24.5), a key ingredient for the success of Stage IV dark energy projects based on weak lensing cosmology. A spectroscopic calibration sample as representative as possible of the galaxies in the Euclid weak lensing sample is being collected, selecting galaxies from a self-organizing map (SOM) representation of the galaxy color space. Here, we present the results of a near-infrared H- and K-bands spectrosc…
Forthcoming large photometric surveys for cosmology require precise and accurate photometric redshift (photo-z) measurements for the success of their main science objectives. However, to date, no method has been able to produce photo-$z$s at the required accuracy using only the broad-band photometry that those surveys will provide. An assessment of the strengths and weaknesses of current methods is a crucial step in the eventual development of an approach to meet this challenge. We report on the performance of 13 photometric redshift code single value redshift estimates and redshift probabilit…
Aims. We validate a semi-analytical model for the covariance of real-space 2-point correlation function of galaxy clusters. Methods. Using 1000 PINOCCHIO light cones mimicking the expected Euclid sample of galaxy clusters, we calibrate a simple model to accurately describe the clustering covariance. Then, we use such a model to quantify the likelihood analysis response to variations of the covariance, and investigate the impact of a cosmology-dependent matrix at the level of statistics expected for the Euclid survey of galaxy clusters. Results. We find that a Gaussian model with Poissonian sho…
We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer's Infrared Array Camera (IRAC). We have combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11% of the total Spitzer mission time. The resulting mosaics cover a total of approximately 71.5deg$^2$ in the 3.6 and 4.5um bands, and approximately 21.8deg$^2$ in the 5.8 and 8um bands. They reach at least 24 AB magnitude (measured to…
We investigate the importance of lensing magnification for estimates of galaxy clustering and its cross-correlation with shear for the photometric sample of Euclid. Using updated specifications, we study the impact of lensing magnification on the constraints and the shift in the estimation of the best fitting cosmological parameters that we expect if this effect is neglected. We follow the prescriptions of the official Euclid Fisher matrix forecast for the photometric galaxy clustering analysis and the combination of photometric clustering and cosmic shear. The slope of the luminosity function…
Euclid preparation: The flat-sky approximation for the clustering of Euclid's photometric galaxies
Université de Genève, Département de Physique Théorique and Centre for Astroparticle Physics（日内瓦大学理论物理系与天体粒子物理中心）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；Dipartimento di Fisica, Università degli Studi di Torino（都灵大学物理系）；INFN-Sezione di Torino（意大利国家核物理研究院都灵分部）；INAF-Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（西班牙高等科学研究理事会））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES（天体物理学与行星学研究所以及图卢兹大学、法国国家科学研究中心、图卢兹第三大学、法国国家太空研究中心）；ESAC/ESA（欧洲空间应用中心/欧洲空间局）；School of Mathematics and Physics, University of Surrey（萨里大学数学与物理学院）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
Euclid preparation. Cosmology Likelihood for Observables in Euclid (CLOE). 5. Extensions beyond the standard modelling of theoretical probes and systematic effects
The analysis of weak gravitational lensing in wide-field imaging surveys is considered to be a major cosmological probe of dark energy. Our capacity to constrain the dark energy equation of state relies on the accurate knowledge of the galaxy mean redshift $\langle z \rangle$. We investigate the possibility of measuring $\langle z \rangle$ with an accuracy better than $0.002\,(1+z)$, in ten tomographic bins spanning the redshift interval $0.2<z<2.2$, the requirements for the cosmic shear analysis of Euclid. We implement a sufficiently realistic simulation to understand the advantages, compleme…
Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesi…
This work considers which higher-order effects in modelling the cosmic shear angular power spectra must be taken into account for Euclid. We identify which terms are of concern, and quantify their individual and cumulative impact on cosmological parameter inference from Euclid. We compute the values of these higher-order effects using analytic expressions, and calculate the impact on cosmological parameter estimation using the Fisher matrix formalism. We review 24 effects and find the following potentially need to be accounted for: the reduced shear approximation, magnification bias, source-le…
Euclid preparation. Calibrated intrinsic galaxy alignments in the Euclid Flagship simulation
Institute of Space Sciences (ICE, CSIC)（空间科学研究所（欧洲宇宙学中心，西班牙国家科学研究委员会））；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理、物质与辐射相互作用实验室）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）；Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT)（能源、环境和技术研究中央中心）；Port d’Informació Científica（科学信息港）；Institute for Theoretical Physics, Utrecht University（乌得勒支大学理论物理研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Institut de Física d’Altes Energies (IFAE)（高能物理研究所）；The Barcelona Institute of Science and Technology（巴塞罗那科学技术研究院）；Instituto de Astronomia Teorica y Experimental (IATE-CONICET)（理论与实验天文学研究所（阿根廷国家科学研究委员会））；Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University（斯德哥尔摩大学物理系奥斯卡·克莱因宇宙粒子物理中心）；Astrophysics Group, Blackett Laboratory, Imperial College（帝国理工学院布莱克特实验室天体物理学组）
Euclid preparation. CIV. Impact of galaxy intrinsic alignment modelling choices on Euclid 3x2pt cosmology
Leiden University（莱顿大学）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚太空研究学院（IEEC））；Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse（天体物理学与行星学研究所（IRAP），图卢兹大学）；Université Paris-Saclay（巴黎萨克雷大学）；University College London（伦敦大学学院）
评估星系内禀对准模型选择对 Euclid 3x2pt 分析的影响，发现红移依赖的 TATT 模型在灵活性和约束力上最优。
The Complete Calibration of the Colour-Redshift Relation survey (C3R2) is a spectroscopic effort involving ESO and Keck facilities designed to empirically calibrate the galaxy colour-redshift relation - P(z|C) to the Euclid depth (i_AB=24.5) and is intimately linked to upcoming Stage IV dark energy missions based on weak lensing cosmology. The aim is to build a spectroscopic calibration sample that is as representative as possible of the galaxies of the Euclid weak lensing sample. In order to minimise the number of spectroscopic observations to fill the gaps in current knowledge of the P(z|C),…
Euclid preparation. Simulating thousands of Euclid spectroscopic skies
Università di Trieste（的里雅斯特大学）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据和量子计算国家研究中心）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（西班牙高等科学研究委员会））；Dipartimento di Fisica, Università degli studi di Genova（热那亚大学物理系）；INFN-Sezione di Genova（意大利国家核物理研究所热那亚分部）；SISSA, International School for Advanced Studies（国际高等研究学院）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）
Euclid preparation. CosmoPostProcess: A simulation calibrated framework for weak lensing selection bias in richness-selected galaxy clusters
Università di Trieste（的里雅斯特大学）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所(IFPU)）；INAF-Osservatorio Astronomico di Trieste（的里雅斯特天文台(INAF)）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Department of Mathematical Physics, Institute of Physics, University of São Paulo（圣保罗大学物理学院数学物理系）；ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据与量子计算国家研究中心(ICSC)）
Euclid preparation. XCI. Validation method for the detections in the Euclid Catalogue of Galaxy Clusters using external data
Université Paris-Saclay（巴黎萨克雷大学）；CEA（法国原子能和替代能源委员会）；University of California, Davis（加州大学戴维斯分校）；Université Paris Cité（巴黎西岱大学）；CNRS（法国国家科学研究中心）；Observatorio Astronómico Nacional, IGN（国家天文学观测台，西班牙地理与统计研究所）；CNRS-UCB International Research Laboratory, Centre Pierre Binétruy（CNRS-加州大学伯克利分校国际研究实验室，皮埃尔·比内特鲁中心）；IRFU（核物理研究研究所）；Universität Bonn（波恩大学）；Argelander-Institut für Astronomie（阿尔加登天文研究所）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）
Universität Innsbruck（因斯布鲁克大学）；Aix-Marseille Université（艾克斯-马赛大学）；Leiden University（莱顿大学）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（斯坦福直线加速器中心）；University of Edinburgh（爱丁堡大学）
Euclid preparation. XCII. Controlling angular systematics in the Euclid spectroscopic galaxy sample
Università di Trieste（的里雅斯特大学）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据和量子计算国家研究中心）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
Euclid preparation. Impact of redshift distribution uncertainties on the joint analysis of photometric galaxy clustering and weak gravitational lensing
Ruhr University Bochum（鲁尔大学波鸿分校）；Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT)（能源、环境和技术中心研究所）；Aix-Marseille Université（艾克斯-马赛大学）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto（波尔图大学太空科学与天体物理研究所）；Faculdade de Ciências da Universidade do Porto（波尔图大学理学院）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（西班牙高等科学研究理事会））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse（图卢兹大学天体物理学和行星学研究所在）
Euclid preparation. XCV. Cosmology Likelihood for Observables in Euclid (CLOE). 2. Code implementation
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT)（能源、环境和技术中心）；Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）；Waterloo Centre for Astrophysics, University of Waterloo（滑铁卢大学天体物理中心）；Department of Physics and Astronomy, University of Waterloo（滑铁卢大学物理与天文系）；European Space Agency/ESTEC（欧洲空间局/欧洲空间研究与技术中心）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学Kavli宇宙粒子与宇宙学起源研究所数据驱动发现中心）；Laboratoire Univers et Théorie, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS（巴黎天文台宇宙与理论实验室）；INAF-IASF Milano（意大利国家天体物理研究所米兰天文物理研究所）；Dipartimento di Fisica, Università degli Studi di Torino（都灵大学物理系）；INFN-Sezione di Torino（意大利国家核物理研究所都灵分部）；INAF-Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
Euclid preparation XCVII. Cosmology Likelihood for Observables in Euclid (CLOE). 4: Validation and performance
INAF-Osservatorio Astronomico di Roma（罗马国家天体物理研究所天文台）；INFN-Sezione di Roma（罗马国家核物理研究所分会）；INAF-Osservatorio Astronomico di Brera（布雷拉国家天体物理研究所天文台）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli宇宙起源与演化粒子物质统一研究前沿中心）；Laboratoire Univers et Théorie, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS（巴黎天文台宇宙与理论实验室）；INAF-IASF Milano（米兰国家天体物理研究所天体物理与星际介质研究所）；Waterloo Centre for Astrophysics, University of Waterloo（滑铁卢大学天体物理中心）；Dipartimento di Fisica, Università degli Studi di Torino（都灵大学物理系）；INFN-Sezione di Torino（都灵国家核物理研究所分会）；INAF-Osservatorio Astrofisico di Torino（都灵国家天体物理研究所天文台）；European Space Agency/ESTEC（欧洲空间局/欧洲空间研究与技术中心）
Euclid preparation. Testing analytic models of galaxy intrinsic alignments in the Euclid Flagship simulation
Université Paris-Saclay, Université Paris Cité（巴黎萨克雷大学、巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；Centre National d’Etudes Spatiales – Centre spatial de Toulouse（法国国家空间研究中心图卢兹航天中心）；University College London（伦敦大学学院）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）；Institut de Recherche en Astrophysique et Planétologie (IRAP)（天体物理学与行星学研究所在）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Northeastern University（东北大学）；University of Zurich（苏黎世大学）；ESAC/ESA（欧洲空间应用中心/欧洲空间局）
Euclid preparation. XXXIV. The effect of linear redshift-space distortions in photometric galaxy clustering and its cross-correlation with cosmic shear
