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Euclid preparation: I. The Euclid Wide Survey

R. Scaramella 1 J. Amiaux 2 Y. Mellier 2 C. Burigana 3 C. S. Carvalho 4 J. -C. Cuillandre A. da Silva A. Derosa J. Dinis E. Maiorano M. Maris I. Tereno R. Laureijs T. Boenke G. Buenadicha X. Dupac L. M. Gaspar Venancio P. Gómez-Álvarez J. Hoar J. Lorenzo Alvarez G. D. Racca G. Saavedra-Criado J. Schwartz R. Vavrek M. Schirmer H. Aussel R. Azzollini V. F. Cardone M. Cropper A. Ealet B. Garilli W. Gillard B. R. Granett L. Guzzo H. Hoekstra K. Jahnke T. Kitching M. Meneghetti L. Miller R. Nakajima S. M. Niemi F. Pasian W. J. Percival M. Sauvage M. Scodeggio S. Wachter A. Zacchei N. Aghanim A. Amara T. Auphan N. Auricchio S. Awan A. Balestra R. Bender C. Bodendorf D. Bonino E. Branchini S. Brau-Nogue M. Brescia G. P. Candini V. Capobianco C. Carbone R. G. Carlberg J. Carretero R. Casas F. J. Castander M. Castellano S. Cavuoti A. Cimatti R. Cledassou G. Congedo C. J. Conselice L. Conversi Y. Copin L. Corcione A. Costille F. Courbin H. Degaudenzi M. Douspis F. Dubath C. A. J. Duncan S. Dusini S. Farrens S. Ferriol P. Fosalba N. Fourmanoit M. Frailis E. Franceschi P. Franzetti M. Fumana B. Gillis C. Giocoli A. Grazian F. Grupp S. V. H. Haugan W. Holmes F. Hormuth P. Hudelot S. Kermiche A. Kiessling M. Kilbinger R. Kohley B. Kubik M. Kümmel M. Kunz H. Kurki-Suonio S. Ligori P. B. Lilje I. Lloro O. Mansutti O. Marggraf K. Markovic F. Marulli R. Massey S. Maurogordato 5 M. Melchior E. Merlin G. Meylan J. J. Mohr M. Moresco B. Morin L. Moscardini E. Munari R. C. Nichol C. Padilla S. Paltani J. Peacock K. Pedersen V. Pettorino S. Pires M. Poncet L. Popa L. Pozzetti F. Raison R. Rebolo J. Rhodes H. -W. Rix M. Roncarelli E. Rossetti R. Saglia P. Schneider T. Schrabback A. Secroun G. Seidel S. Serrano C. Sirignano G. Sirri J. Skottfelt L. Stanco J. L. Starck P. Tallada-Crespí D. Tavagnacco A. N. Taylor H. I. Teplitz R. Toledo-Moreo F. Torradeflot M. Trifoglio E. A. Valentijn L. Valenziano G. A. Verdoes Kleijn Y. Wang N. Welikala J. Weller M. Wetzstein G. Zamorani J. Zoubian S. Andreon M. Baldi S. Bardelli A. Boucaud S. Camera G. Fabbian R. Farinelli J. Graciá-Carpio D. Maino E. Medinaceli S. Mei C. Neissner G. Polenta A. Renzi E. Romelli C. Rosset F. Sureau M. Tenti T. Vassallo E. Zucca C. Baccigalupi A. Balaguera-Antolínez P. Battaglia A. Biviano S. Borgani E. Bozzo R. Cabanac A. Cappi S. Casas G. Castignani C. Colodro-Conde J. Coupon H. M. Courtois J. Cuby S. de la Torre S. Desai D. Di Ferdinando H. Dole M. Fabricius M. Farina P. G. Ferreira F. Finelli P. Flose-Reimberg S. Fotopoulou S. Galeotta K. Ganga G. Gozaliasl I. M. Hook E. Keihanen C. C. Kirkpatrick P. Liebing V. Lindholm G. Mainetti M. Martinelli N. Martinet M. Maturi H. J. Mccracken R. B. Metcalf G. Morgante J. Nightingale A. Nucita L. Patrizii D. Potter G. Riccio A. G. Sánchez D. Sapone J. A. Schewtschenko M. Schultheis V. Scottez R. Teyssier I. Tutusaus J. Valiviita M. Viel W. Vriend L. Whittaker
Abstract : 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 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 simulate the dither pattern at pixel level to analyse the effective coverage. We use 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 are also considered. Via purposely-built software optimized to prioritize best sky areas, produce a compact coverage, and ensure thermal stability, we generate a schedule for the Auxiliary and Deep fields observations and schedule the RoI with EWS transit observations. The resulting reference survey RSD_2021A fulfills all constraints and is a good proxy for the final solution. Its wide survey covers 14,500 square degrees. The limiting AB magnitudes ($5\sigma$ point-like source) achieved in its footprint are estimated to be 26.2 (visible) and 24.5 (near-infrared); for spectroscopy, the H$_\alpha$ line flux limit is $2\times 10^{-16}$ erg cm$^{-2}$ s$^{-1}$ at 1600 nm; and for diffuse emission the surface brightness limits are 29.8 (visible) and 28.4 (near-infrared) mag arcsec$^{-2}$.
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Preprints, Working Papers, ...
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https://hal-cnrs.archives-ouvertes.fr/hal-03451665
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Submitted on : Friday, November 26, 2021 - 3:34:10 PM
Last modification on : Tuesday, January 4, 2022 - 6:44:18 AM

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  • HAL Id : hal-03451665, version 1
  • ARXIV : 2108.01201

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R. Scaramella, J. Amiaux, Y. Mellier, C. Burigana, C. S. Carvalho, et al.. Euclid preparation: I. The Euclid Wide Survey. 2021. ⟨hal-03451665⟩

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