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GianlucaGianlucaPolentaRenzi, A.A.RenziRomelli, E.E.RomelliRosset, C.C.RossetSureau, F.F.SureauTenti, M.M.TentiVassallo, T.T.VassalloZucca, E.E.ZuccaBaccigalupi, C.C.BaccigalupiBalaguera-Antolínez, A.A.Balaguera-AntolínezBattaglia, P.P.BattagliaBiviano, A.A.BivianoBorgani, S.S.BorganiBozzo, E.E.BozzoCabanac, R.R.CabanacCappi, A.A.CappiCasas, S.S.CasasCastignani, G.G.CastignaniColodro-Conde, C.C.Colodro-CondeCoupon, J.J.CouponCourtois, H.M.H.M.CourtoisCuby, J.J.CubyDe La Torre, S.S.De La TorreDesai, S.S.DesaiDole, H.H.DoleFabricius, M.M.FabriciusFarina, M.M.FarinaFerreira, P.G.P.G.FerreiraFinelli, F.F.FinelliFlose-Reimberg, P.P.Flose-ReimbergFotopoulou, S.S.FotopoulouGanga, K.K.GangaGozaliasl, G.G.GozaliaslHook, I.M.I.M.HookKeihanen, E.E.KeihanenKirkpatrick, C.C.C.C.KirkpatrickLiebing, P.P.LiebingLindholm, V.V.LindholmMainetti, G.G.MainettiMartinelli, M.M.MartinelliMartinet, N.N.MartinetMaturi, M.M.MaturiMcCracken, H.J.H.J.McCrackenMetcalf, R.B.R.B.MetcalfMorgante, G.G.MorganteNightingale, J.J.NightingaleNucita, A.A.NucitaPatrizii, L.L.PatriziiPotter, D.D.PotterRiccio, G.G.RiccioSánchez, A.G.A.G.SánchezSapone, D.D.SaponeSchewtschenko, J.A.J.A.SchewtschenkoSchultheis, M.M.SchultheisScottez, V.V.ScottezTeyssier, R.R.TeyssierTutusaus, I.I.TutusausValiviita, J.J.ValiviitaViel, M.M.VielVriend, W.W.VriendWhittaker, L.L.Whittaker2022-09-012022-09-012022-06-28https://hdl.handle.net/20.500.13025/6278Open AccessEuclid 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 deg2 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 ∼14.500 deg2. The limiting AB magnitudes (5ρpoint-like source) achieved in its footprint are estimated to be 26.2 (visible band IE) and 24.5 (for near infrared bands YE, JE, HE); for spectroscopy, the Hα line flux limit is 2.10-16 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. © ESO 2022.enjournal article10.1051/0004-6361/202141938https://www.aanda.org/articles/aa/full_html/2022/06/aa41938-21/aa41938-21.html