Euclid will provide deep NIR imaging to sim26.5 AB magnitude over sim59 deg2 in its deep and auxiliary fields. The Cosmic DAWN survey complements the deep Euclid data with matched depth multiwavelength imaging and spectroscopy in the UVIR to provide consistently processed Euclid selected photometric catalogs accurate photometric redshifts and measurements of galaxy properties to a redshift of zsim 10. In this paper we present an overview of the survey including the footprints of the survey fields the existing and planned observations and the primary science goals for the combined data set.
['Astrophysics - Astrophysics of Galaxies']
Euclid preparation. The Cosmic Dawn Survey DAWN of the Euclid Deep and Auxiliary Fields
{'Euclid Preparation. The Cosmic Dawn Survey (DAWN) of the Euclid Deep and Auxiliary Fields': 'Euclid Collaboration: C. J. R. McPartland ⋆ 1 , 2 , 3 , 4 , 5 , L. Zalesky 3 , J. R. Weaver 6 , S. Toft 1 , 2 , D. B. Sanders 3 , B. Mobasher 4 , N. Suzuki 7 , I. Szapudi 3 , I. Valdes 3 , G. Murphree 3 , N. Chartab 8 , N. Allen 1 , S. Taamoli 4 , P. R. M. Eisenhardt 9 , S. Arnouts 10 , H. Atek 11 , J. Brinchmann 12 , M. Castellano 13 , R. Chary 14 , O. Chávez Ortiz 15 , J.-G. Cuby 16 , 10 , S. L. Finkelstein 15 , T. Goto 17 , S. Gwyn 18 , Y. Harikane 19 , A. K. Inoue 20 , 21 , H. J. McCracken 11 , J. J. Mohr 22 , 23 , P. A. Oesch 24 , 2 , 1 , M. Ouchi 25 , 19 , 26 , 27 , M. Oguri 17 , 28 , J. Rhodes 9 , H. J. A. Rottgering 29 , M. Sawicki 30 , R. Scaramella 13 , 31 , C. Scarlata 32 , J. D. Silverman 27 , 33 , 34 , D. Stern 9 , H. I. Teplitz 14 , M. Shuntov 35 , 5 , 2 , B. Altieri 36 , A. Amara 37 , S. Andreon 38 , N. Auricchio 39 , H. Aussel 40 , C. Baccigalupi 41 , 42 , 43 , 44 , M. Baldi 45 , 39 , 46 , S. Bardelli 39 , R. Bender 23 , 22 , D. Bonino 47 , E. Branchini 48 , 49 , 38 , M. Brescia 50 , 51 , 52 , S. Camera 53 , 54 , 47 , V. Capobianco 47 , C. Carbone 55 , J. Carretero 56 , 57 , S. Casas 58 , F. J. Castander 59 , 60 , G. Castignani 61 , 39 , S. Cavuoti 51 , 52 , A. Cimatti 62 , C. Colodro-Conde 63 , G. Congedo 64 , C. J. Conselice 65 , L. Conversi 66 , 36 , Y. Copin 67 , F. Courbin 68 , H. M. Courtois 69 , A. Da Silva 70 , 71 , H. Degaudenzi 24 , G. De Lucia 42 , A. M. Di Giorgio 72 , J. Dinis 70 , 71 , M. Douspis 73 , F. Dubath 24 , X. Dupac 36 , S. Dusini 74 , M. Fabricius 23 , 22 , M. Farina 72 , S. Farrens 40 , S. Ferriol 67 , S. Fotopoulou 75 , M. Frailis 42 , E. Franceschi 39 , M. Fumana 55 , S. Galeotta 42 , B. Garilli 55 , K. George 22 , B. Gillis 64 , C. Giocoli 39 , 76 , A. Grazian 77 , F. Grupp 23 , 22 , L. Guzzo 78 , 38 , H. Hoekstra 29 , W. Holmes 9 , I. Hook 79 , F. Hormuth 80 , A. Hornstrup 81 , 5 , P. Hudelot 11 , K. Jahnke 82 , E. Keihänen 83 , S. Kermiche 84 , A. Kiessling 9 , M. Kilbinger 40 , T. Kitching 85 , B. Kubik 67 , M. Kunz 86 , H. Kurki-Suonio 87 , 88 , P. B. Lilje 89 , V. Lindholm 87 , 88 , I. Lloro 90 , G. Mainetti 91 , E. Maiorano 39 , O. Mansutti 42 , O. Marggraf 92 , K. Markovic 9 , M. Martinelli 13 , 31 , N. Martinet 10 , F. Marulli 61 , 39 , 46 , R. Massey 93 , S. Maurogordato 94 , E. Medinaceli 39 , S. Mei 95 , M. Melchior 96 , Y. Mellier 35 , 11 , M. Meneghetti 39 , 46 , E. Merlin 13 , G. Meylan 68 , M. Moresco 61 , 39 , L. Moscardini 61 , 39 , 46 , E. Munari 42 , R. Nakajima 92 , C. Neissner 56 , 57 , S.-M. Niemi 97 , J. W. Nightingale 98 , 93 , C. Padilla 56 , S. Paltani 24 , F. Pasian 42 , K. Pedersen 99 , W. J. Percival 100 , 101 , 102 , V. Pettorino 97 , G. Polenta 103 , M. Poncet 104 , L. A. Popa 105 , L. Pozzetti 39 , F. Raison 23 , R. Rebolo 63 , 106 , A. Renzi 107 , 74 , G. Riccio 51 , E. Romelli 42 , M. Roncarelli 39 , E. Rossetti 45 , R. Saglia 22 , 23 , Z. Sakr 108 , 109 , 110 , A. G. Sánchez 23 , D. Sapone 111 , B. Sartoris 22 , 42 , M. Schirmer 82 , P. Schneider 92 , T. Schrabback 112 , A. Secroun 84 , G. Seidel 82 , S. Serrano 60 , 59 , 113 , C. Sirignano 107 , 74 , G. Sirri 46 , L. Stanco 74 , J. Steinwagner 23 , C. Surace 10 , P. Tallada-Crespi 114 , 57 , D. Tavagnacco 42 , I. Tereno 70 , 115 , R. Toledo-Moreo 116 , F. Torradeflot 57 , 114 , I. Tutusaus 109 , E. A. Valentijn 117 , L. Valenziano 39 , 118 , T. Vassallo 22 , 42 , A. Veropalumbo 38 , 49 , Y. Wang 14 , J. Weller 22 , 23 , G. Zamorani 39 , J. Zoubian 84 , E. Zucca 39 , A. Biviano 42 , 44 , M. Bolzonella 39 , A. Boucaud 95 , E. Bozzo 24 , C. Burigana 119 , 118 , D. Di Ferdinando 46 , R. Farinelli 39 , J. Gracia-Carpio 23 , N. Mauri 62 , 46 , V. Scottez 35 , 120 , M. Tenti 46 , M. Viel 44 , 42 , 41 , 43 , 121 , M. Wiesmann 89 , Y. Akrami 122 , 123 , V. Allevato 51 , S. Anselmi 74 , 107 , 124 , M. Ballardini 125 , 39 , 126 , M. Bethermin 127 , 10 , S. Borgani 128 , 44 , 42 , 43 , A. S. Borla ff 129 , 130 , S. Bruton 32 , R. Cabanac 109 , A. Calabro 13 , G. Cañas-Herrera 97 , 131 , A. Cappi 39 , 94 , C. S. Carvalho 115 , T. Castro 42 , 43 , 44 , 121 , K. C. Chambers 3 , S. Contarini 23 , 61 , A. R. Cooray 132 , J. Coupon 24 , S. Davini 49 , S. de la Torre 10 , G. Desprez 30 , A. Díaz-Sánchez 133 , S. Di Domizio 48 , 49 , H. Dole 73 , J. A. Escartin Vigo 23 , S. Esco ffi er 84 , A. G. Ferrari 62 , 46 , P. G. Ferreira 134 , I. Ferrero 89 , F. Finelli 39 , 118 , F. Fornari 118 , L. Gabarra 134 , K. Ganga 95 , J. García-Bellido 122 , V. Gautard 135 , E. Gaztanaga 59 , 60 , 136 , F. Giacomini 46 , G. Gozaliasl 137 , 87 , A. Gregorio 128 , 42 , 43 , A. Hall 64 , W. G. Hartley 24 , H. Hildebrandt 138 , J. Hjorth 139 , M. Huertas-Company 63 , 140 , 141 , 142 , O. Ilbert 10 , J. J. E. Kajava 143 , 144 , V. Kansal 145 , 146 , D. Karagiannis 147 , 148 , C. C. Kirkpatrick 83 , L. Legrand 149 , G. Libet 104 , A. Loureiro 150 , 151 , J. Macias-Perez 152 , G. Maggio 42 , M. Magliocchetti 72 , C. Mancini 55 , F. Mannucci 153 , R. Maoli 154 , 13 , C. J. A. P. Martins 155 , 12 , S. Matthew 64 , M. Maturi 108 , 156 , L. Maurin 73 , R. B. Metcalf 61 , 39 , P. Monaco 128 , 42 , 43 , 44 , C. Moretti 41 , 121 , 42 , 44 , 43 , G. Morgante 39 , P. Musi 157 , Nicholas A. Walton 158 , J. Odier 152 , L. Patrizii 46 , M. Pöntinen 87 , V. Popa 105 , C. Porciani 92 , D. Potter 159 , P. Reimberg 35 , I. Risso 160 , P.-F. Rocci 73 , M. Sahlén 161 , A. Schneider 159 , M. Sereno 39 , 46 , P. Simon 92 , A. Spurio Mancini 85 , S. A. Stanford 162 , C. Tao 84 , G. Testera 49 , R. Teyssier 163 , S. Tosi 48 , 38 , 49 , A. Troja 107 , 74 , M. Tucci 24 , C. Valieri 46 , J. Valiviita 87 , 88 , D. Vergani 39 , G. Verza 164 , 165 , and F. Shankar 166  \n(A ffi liations can be found after the references)', 'ABSTRACT': 'Euclid will provide deep NIR imaging to ∼ 26.5 AB magnitude over ∼ 59 deg 2 in its deep and auxiliary fields. The Cosmic DAWN survey complements the deep Euclid data with matched depth multiwavelength imaging and spectroscopy in the UV-IR to provide consistently processed Euclid selected photometric catalogs, accurate photometric redshifts, and measurements of galaxy properties to a redshift of z ∼ 10. In this paper, we present an overview of the survey, including the footprints of the survey fields, the existing and planned observations, and the primary science goals for the combined data set.  \nKey words. Surveys; Catalogs; Galaxies: high-redshift; Galaxies: evolution; Galaxies: luminosity function, mass function', '1. Introduction': "The Euclid mission (Laureijs et al. 2011; Euclid Collaboration: Mellier et al. 2024; Euclid Collaboration: Cropper et al. 2024; Euclid Collaboration: Jahnke et al. 2024) is designed to constrain the properties of dark matter and dark energy through weak lensing, galaxy cluster counts, and clustering measurements. The majority of the six year mission will be spent carrying out a wide area imaging and spectroscopic survey (the Euclid Wide Survey: EWS; Euclid Collaboration: Scaramella et al. 2022) covering roughly 14 000 deg 2 of the extragalactic sky. The EWS will measure the shape and colour of billions of galaxies from imaging observations in a single broad visible band ( I E) and three nearinfrared (NIR) bands ( Y E, J E, H E) with expected depths of 25 AB (10 σ for extended sources) and 24.5 AB (5 σ for point sources) respectively. The spectroscopic component of EWS will measure redshifts for around thirty million galaxies with emission line fluxes of 2 × 10 -16 erg cm -2 s -1 at 1.6 µ m. Redshifts for the remaining galaxies will be measured photometrically by combining ground-based optical photometry with the Euclid data.  \nEuclid will also devote 17% of the primary mission time to obtaining deeper observations needed for calibration, control of systematic e ff ects, and characterising the galaxy sample from the EWS. The six Euclid auxiliary fields (EAFs; CDFS, COSMOS, SXDS, VVDS, AEGIS, and GOODS-N, see Sect. 2 for details) each have extensive UV-NIR imaging observations and large catalogues of spectroscopic redshift measurements. Three large (10-20 deg 2 ) Euclid Deep Fields (EDFs; EDF-North, EDFSouth, and EDF-Fornax) were also selected for observations two mag deeper than the EWS. Consistent processing and photometric measurements from the Euclid and ancillary data in the EAFs and EDFs is essential for calibrating photometric redshift measurements and quantifying biases in shape measurements from the broader EWS.  \nThe Cosmic DAWN Survey (DAWN) is a 59deg 2 multiwavelength imaging survey of the EDFs and EAFs with comparable depth to the Euclid data. Spitzer / IRAC data cover all the DAWN fields at 3.6 and 4.5 µ m (Euclid Collaboration: Moneti et al. 2022) and incorporate the single largest allocation of Spitzer observing time (Capak et al. 2016). The Hawaii Twenty deg 2 Survey (H20; Euclid Collaboration: Zalesky et al. 2024) provides Subaru Hyper Suprime-Cam optical data and CFHT MegaCam UV data for EDF-N and EDF-F. The Hyper SuprimeCam Subaru Strategic Survey (HSC-SSP Aihara et al. 2018a) provides optical data for COSMOS, SXDS, VVDS, and AEGIS. Additional UV-optical data for EDF-F and EDF-S will also be provided by Vera C. Rubin Observatory (Ivezi'c et al. 2019). The CFHT large area U-band deep survey (CLAUDS; Sawicki et al. 2019) and the ongoing Deep Euclid U-band Survey (DEUS) program provide additional CFHT MegaCam UV data in COSMOS, SXDS, EDF-N, and GOODS-N.  \nFig. 1. Illustration of the dark matter overdensity, δ DM ≡ ρ DM / ¯ ρ DM -1, at redshifts 4 . 3 < z < 5 . 3 in a 5 · × 5 · region from the cosmological simulation of Rácz et al. (2021). The large circle encloses a 10 deg 2 region, which is equivalent to the area covered by the smallest EDF. The small rectangles and circle are comparable to the areas of the CANDELS and COSMOS surveys, respectively. The DAWN survey has both the depth and large area coverage needed to study rare overdensity peaks (orange) and cosmic voids (blue) and place strong constraints on the overall cosmological distribution of dark matter. The scale bar shows the angular size for a proper distance of 20 Mpc at z = 5.  \n<!-- image -->  \nThe combination of depth, area, and wavelength coverage makes DAWN an excellent data set for studying galaxy evolution and robustly characterising the z > 4 galaxy population. Deep rest-frame UV-near-IR data are critical for estimating photometric redshifts and physical parameters (e.g., stellar mass, starformation rate) of galaxies. Robustly characterizing the z > 4 galaxy population requires multiwavelength data that cover observed wavelengths from the near-UV (0.3 µ m) to near-IR (35 µ m) and are deep enough to detect faint ( z AB ∼ 26) galaxies. Large fields ( ≳ 10 deg 2 ) are needed to identify rare sources in the high-redshift Universe, probe cosmologically significant volumes ( ∼ 1 Gpc 3 ), and making them contiguous allows one to study the evolution of large-scale structure with cosmic time. Existing deep fields with similar depth and wavelength coverage such as the CANDELS fields (Grogin et al. 2011; Koekemoer et al. 2011) and COSMOS deep field (Scoville 2007) are prone to small number statistics and cosmic variance due to the scale of variations in the underlying dark matter (DM) density field at high redshifts (see Fig. 1).  \nThe COSMOSfield has shown the power of multiwavelength data sets spanning large areas of the sky. The DAWN survey aims to expand on the legacy of COSMOS by providing value added  \nTable 1. The center coordinates (J2000), area coverage, and foreground dust reddening E ( B -V ) of the Euclid Deep and Auxiliary fields.  \n* The provided E ( B -V ) values are evaluated at the field center from Planck Collaboration: Aghanim et al. (2016).  \ncatalogues with consistently measured Euclid selected multiwavelength photometry and physical properties in the EDFs and EAFs; an area 30 × larger than the COSMOS field. By including Spitzer / IRAC data needed to probe the rest-frame optical at z > 4, the DAWN catalogues are optimized for high-redshift and galaxy evolution science and are thus complimentary to the o ffi cial Euclid catalogues. This paper describes the fields, observations, and science goals of the DAWN survey. A companion paper (Euclid Collaboration: Zalesky et al. 2024) provides the first DAWN survey catalogue of the pre-launch data in EDF-N and EDF-F. Future DAWN data releases (including EDF-S and the EAFs) will follow each of the Euclid data releases.  \nSection 2 describes the fields covered by the DAWN survey. Sections 3 and 4 summarise the broad-band imaging and spectroscopic observations (respectively) in each field. The main science goals of the survey are discussed in Section 5 and Section 6 provides a summary of the survey.", '2. Survey fields': 'The DAWN survey covers each of the EDFs and EAFs. The center coordinates and area of each field are presented in Table 1, and Fig. 2 shows their positions on an all-sky map. The following subsections give a brief summary of the EDFs and EAFs. Consult the Euclid overview paper (Euclid Collaboration: Mellier et al. 2024) for more details.', '2.1. Euclid Deep Fields': 'The deepest observations from the Euclid mission focus on three fields: Euclid Deep Field North (EDF-N), Euclid Deep Field Fornax (EDF-F), and Euclid Deep Field South (EDF-S). The locations of EDF-N and EDF-S were strategically chosen to maximise their observability throughout the duration of the Euclid mission. Each field will receive Euclid imaging observations that are 2 mag deeper than the EWS, which is essential for calibration of the bias introduced by noise in weak lensing measurements. The depth and area (see Table 1 & 2) of the EDFs make them the primary fields for galaxy evolution and high-redshift science from the Euclid mission.  \nEDF-N covers a 20 deg 2 circular region centered on the North Ecliptic Pole (NEP) in the constellation Draco. Due to its proximity to the ecliptic pole, EDF-N has perennial visibility by  \nEuclid allowing for regularly repeated observations throughout the mission. EDF-F is a 10 deg 2 circular region in the constellation Fornax. EDF-S covers a 23 deg 2 elongated region in the southern constellation of Horologium.', '2.2. Euclid Auxiliary Fields': 'The EAFs focus on well studied galaxy deep fields (COSMOS, AEGIS, SXDS, VVDS, CDFS, and GOODS-N) and will receive observations from Euclid that are four to five times deeper than the EWS. Due to the large amount of existing multiwavelength data in these fields, the EAFs will be essential for calibrating photometric redshift estimates and the e ff ect of colour gradients in galaxies on shear measurements for the EWS.  \nThe COSMOS EAF (Scoville 2007) has deep multiwavelength observations from X-ray to radio and an extensive spectroscopic database. The COSMOS2020 catalogue (Weaver et al. 2022) provides the most up-to-date compilation of photometry, photoz s, and stellar mass estimates. The Chandra Deep Field South (CDFS) EAF lies within EDF-F and contains one of the deepest observations from by the Chandra X-ray observatory along with complementary observations from UV to radio. Two EAFs lie within the XMM Large Scale Structure (XMM-LSS) Survey field (Clerc et al. 2014): the Subaru / XMM-Newton Deep Survey (SXDS; Sekiguchi et al. 2004) and the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al. 2005a). The SXDS EAF overlaps with the UKIRT Infrared Deep Sky Survey (UKIDSS; Lawrence et al. 2007) UDS field which has extensive spectroscopic coverage from UDSz program (Bradshaw et al. 2013; McLure et al. 2013; Maltby et al. 2016). The VVDS EAF focuses on the VVDS-02h field which includes a total area of 0.61 deg 2 from the VVDS Deep survey and 512 arcmin 2 from the VVDS Ultra-Deep Survey (Le Fèvre et al. 2005b; Le Fevre et al. 2013). The Great Observatories Origins Deep Survey North (GOODS-N; Dickinson et al. 2003) EAF is centered on the Hubble Deep Field which contains some of the deepest observations obtained by HST along with complementary observations from the ground and space. The All-Wavelength Extended Groth Strip International Survey (AEGIS; Davis et al. 2007) EAF is a multiwavelength survey field with low Galactic extinction and observations covering X-ray to radio wavelengths. AEGIS, CDFS, COSMOS, GOODS-N, and SXDS were all targeted as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al. 2011, 0.2 deg 2 in total) and have also been observed by JWST through the CEERS (Bagley et al. 2023, 100 arcmin 2 ), JADES (Eisenstein et al. 2023, 45 arcmin 2 ), PRIMER (Dunlop et al. 2021, 378 arcmin 2 ), NGDEEP (Bagley et al. 2024, 10 arcmin 2 ), and COSMOS-Web (Casey et al. 2023, 0.54 deg 2 ) surveys.', '3. Image data': "The core data set of the DAWN Survey is deep space-based nearIR imaging in the Euclid EDFs and EAFs coupled with deep wide area Spitzer / IRAC data. Figure 3 shows an example of the image data in EDF-N. Figures A.1 and A.2 show the footprints of the UV-near-IR image data in the EDFs and EAFs, respectively. Table 2 provides limiting magnitudes for each band and field and Fig. 4 compares the depths with model spectra of galaxies at a range of redshifts. The rest of this section summarises the UVmid-IR imaging observations and archival data that comprise the DAWN survey data set.  \n-  \nFig. 2. AMollweide projection of the Galactic foreground reddening E ( B -V ) - on the celestial sphere from the Planck Collaboration: Aghanim et al. (2016) generated using the dustmaps Python package (Green 2018). The coordinates of each of the EAFs are indicated with black squares and the EDFs are highlighted with red stars. The solid blue line shows the ecliptic. The dotted blue lines indicate continuous viewing zone (CVZ) for the Euclid mission at ± 87 . · 5. The dot-dashed blue lines indicate ecliptic latitudes of ± 54 · which is the expected boundary for the CVZ of the Roman space telescope (Foley et al. 2018). The dashed blue lines show the CVZ for JWST at ± 85 · . The locations of the north and south ecliptic poles are indicated with the text NEP and SEP, respectively.  \n<!-- image -->  \nFig. 3. An example of the image data quality from the DAWN MegaCam, HSC, IRAC programs in EDF-N. The top panel shows a riz colour image (2 ' × 1 ' ) and the bottom row shows a zoom-in (20 '' × 20 '' ) of the highlighted region in each band of the DAWN data.  \n<!-- image -->  \nTable 2. Expected photometric depths for each of the fields covered by the DAWN survey. Unless noted below, depths are quoted as 5 σ limiting magnitudes (AB) in 2 '' empty apertures.  \nNotes: The Spitzer IRAC depths are average values measured from the image data from Euclid Collaboration: Moneti et al. (2022). Euclid depths are those expected for point sources by the end of the mission. Expected depths for Rubin data from Foley et al. (2018). The u band depths in SXDS and VVDS are from Sawicki et al. (2019) and depths in AEGIS are from Gwyn (2012). Subaru HSC and CFHT MegaCam depths for COSMOS are from Weaver et al. (2022). HSC depths for SXDS, VVDS, and AEGIS are the average over each field provided by Aihara et al. (2022).", '3.1. Euclid Space Telescope observations': "Euclid is a Korsch telescope with a 1.2 m mirror providing an e ff ective collecting area of 1 m 2 (Racca et al. 2016) and two instruments: the Euclid visible imager (VIS; Euclid Collaboration: Cropper et al. 2024) has one broad visible band ( I E) that covers 530-920 nm with a 0 . '' 1 pixel scale; the Near-Infrared Spectrometer and Photometer (NISP; Euclid Collaboration: Jahnke et al. 2024) has three bandsY E, J E, and H E- covering 949.61212.3 nm, 1167.6-1567.0 nm, and 1521.5-2021.4 nm (respectively; Euclid Collaboration: Schirmer et al. 2022) with a pixel scale of 0 . '' 3. VIS and NISP share a common field of view (FoV) of 0.53 deg 2 .  \nEuclid observations in the EDFs and EAFs are the primary motivation for the DAWN survey. The EDFs will each receive more than 40 visits with a final depth that is 2 mag deeper than the EWS. The EAFs will be covered by 1-4 Euclid FoVs with varying depths listed in Table 2.", '3.2. Spitzer/IRAC observations': "The Spitzer Space Telescope (Werner et al. 2004) Infrared Array Camera (IRAC; Fazio et al. 2004) is an imaging camera with four channels centered at 3.6, 4.5, 5.8, and 8.0 µ m(referred to as channels 1-4, respectively). Each channel has a 5 . ' 2 × 5 . ' 2 FoV and a pixel scale of 1 . '' 2.  \nThe DAWN survey covers the Euclid Deep Fields with uniform Spitzer / IRAC imaging data at 3.6 and 4.5 µ m from two dedicated programs: the Euclid / WFIRST Spitzer Legacy Survey (SLS; Capak et al. 2016) that covers EDF-N and EDF-F; and a dedicated program to observe EDF-S (Scarlata et al. 2019). The  \ndedicated observations of the deep fields are supplemented by previous observations extracted from the archive. Observations of the EAFs are also compiled from the archive. All available data in the Euclid fields have been uniformly reduced and are described in detail in Euclid Collaboration: Moneti et al. (2022).", '3.3. HSC optical observations': "Hyper Suprime-Cam (HSC; Miyazaki et al. 2018) is a wide-field optical imaging camera at the prime focus of the 8.2 m Subaru telescope on Maunakea, Hawaii. With a 1 . · 5 diameter FOV and a 0 . '' 168 pixel scale combined with the large collecting area of Subaru, HSC is an e ffi cient instrument for deep surveys covering large areas of the sky.", '3.3.1. H20': "The Hawaii Twenty deg 2 Survey (H20) covers two 10 deg 2 fields in the EDF-N and EDF-F with the Subaru HSC griz bands. Observations of each field were obtained using a seven point flower petal pattern with one central pointing surrounded by the remaining six spread over a circle with a radius of 1.1 deg (see Fig. A.1). Pointings are executed using a standard five point dither pattern with a throw of 120 '' . The target exposure times are 1.1, 2.5, 4.1, and 4.8 hours per pointing for the griz bands, respectively. As these observations are still ongoing, we defer a full accounting of the total number of exposures to a future publication describing the final DAWN data release.  \nFig. 4. Top panel : Throughput curves for the photometric bands in the DAWN survey. Bottom panel : Photometric sensitivity limits for the EDFs at 5 σ with HSC, MegaCam, IRAC, Euclid and Rubin (see Tab. 2 for details). The solid coloured lines show throughputs and depths for EDF-N and EDF-F data from MegaCam, HSC, and IRAC. The dotted lines show the same for EDF-S coverage from Rubin (expected) and IRAC. Euclid NISP depths are shown with solid lines for all three fields since they are identical. The greyscale lines show FSPS (Conroy et al. 2010; Conroy & Gunn 2010) model spectra for galaxies at a range of redshifts (see legend). The model spectra are normalized to stellar masses of M ∗ galaxies at the respective redshift based on Weaver et al. (2023) and Stefanon et al. (2021) which have values of log M ⋆ = 10 . 65 , 10 . 24 , 10 . 0 , 9 . 5 for redshifts z = 4 , 6 , 8 , 10; respectively. All models assume a Chabrier (2003) IMF, a delayed exponential star-formation history with τ = 2 Gyr, Solar metalicity, and Calzetti et al. (2000) dust with A V = 0 . 2.  \n<!-- image -->", '3.3.2. HSC-SSP': "The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP; Aihara et al. 2018a) is a 330 night grizy band imaging survey of the extragalactic sky. HSC-SSP is a three tier 'wedding cake' survey composed of a 1400 deg 2 wide layer, a 26 deg 2 deep layer covering four fields, and a 3.5 deg 2 ultra-deep layer covering COSMOS and SXDS. The extended COSMOS field and XMMLSS, which encompasses SXDS and VVDS, were both observed as part of the deep survey. A single pointing centered on the AEGIS field was also observed to the depth of the wide survey for photoz calibration. The HSC-SSP observing strategy is discussed in Aihara et al. (2018a) and details of the data reduction are described in Bosch et al. (2018) and Aihara et al. (2018b, 2019, 2022).", '3.3.3. Archival HSC data': 'Additional HSC observations were extracted from the archive where available. The HEROES (Taylor et al. 2023a) and AKARI-NEP (Oi et al. 2021) programs both obtained grizy observations in EDF-N. Various PI-led programs at the University of Hawaii provide supplementary data for the COSMOS (see Hu et al. 2016; Tanaka et al. 2017, for details) and GOODS-N fields.', '3.4. MegaCam ultraviolet observations': "MegaCam (Boulade et al. 2003) is an optical wide-field imaging camera mounted at the prime focus of the 3.6 m Canada France Hawaii Telescope (CFHT) on Maunakea, Hawaii. MegaCam has a 1 · × 1 · FoV and a pixel scale of 0 . '' 187. Over its lifetime, MegaCam has had two di ff erent u band filters: an original u ∗ filter that was discontinued in 2015 due to a red leak around 5000 Å and a new bluer u filter that has been in use since then (Sawicki et al. 2019).  \nThe H20 team conducted a dedicated MegaCam u band imaging survey in EDF-N and EDF-F. Observations were obtained in a 4 × 4 grid with a total area coverage of 13.7 deg 2 in each field. In the EDF-N the ongoing 240-hour Deep Euclid U-band Survey (DEUS; PIs: Arnouts and Sawicki) will reach a depth of u = 27 AB over ∼ 10 deg 2 when completed; the DEUS data taken to date were shared by the DEUS team and used in making the u band mosaic for this field. The third Euclid Deep Field, EDF-S, has not been observed by MegaCam as it is not accessible from Maunakea. Planned observations of EDF-S by the Rubin observatory are discussed in Sect. 3.6.  \nAvariety of programs provide MegaCam observations of the EAFs. The CFHT Large Area U-band Deep Survey (CLAUDS; Sawicki et al. 2019) performed dedicated observations using the u band in the COSMOS EAF. CLAUDS and the MegaCam Ultra-deep Survey: u ∗ band Imaging (MUSUBI; Wang et al. 2022) survey provide u ∗ band in XMM-LSS and COSMOS. Observations of the AEGIS EAF were obtained through the CFHT Legacy Survey (CFHTLS) (Gwyn 2012) in the u ∗ band with deep imaging in the CFHTLS-D3 field covering 1 deg 2 and shallower data in the larger CFHTLS-W3 field covering 7 deg 2 . Archival u ∗ band observations of GOODS-N (PI: L. Cowie) were extracted from the Canadian Astronomy Data Centre 1 (CADC) and reduced in the same manner as the data obtained by the H20 team.", '3.5. K band observations': 'Ground-based observations in the K band provide supplementary data to fill in the wavelength gap between the Euclid NISP and Spitzer / IRAC data. Various programs have obtained K band data in the DAWN fields which we briefly summarise here and provide relevant citations where available. The UltraVISTA program (McCracken et al. 2012; Moneti et al. 2023) performed  \nK s band observations of the COSMOS field using VIRCAM on the 4 m VISTA telescope at Cerro Paranal Observatory in Chile. Deep observations of 20 deg 2 in EDF-S have been executed through the EDFS-Ks program (PI M. Nonino). The VIDEO (Jarvis et al. 2013) and VEILS (Hönig et al. 2017) surveys provide VIRCAM K s data in XMM-LSS and CDFS. Additional K band observations from the UKIRT WFCAM also exist in SXDS from UKIDSS UDS (Lawrence et al. 2007).', '3.6. Future Rubin observations': "The Vera Rubin Observatory will perform repeated observations over 18 000 deg 2 to identify optical transients, study dark energy and dark matter, map the Milky Way, and characterise the population of Solar System objects through the 10 year Legacy Survey of Space and Time (LSST) survey (Ivezi'c et al. 2019). In addition to the main LSST program, Rubin will also observe a set of deep drilling fields with more frequent visits that will ultimately have much deeper data in the ugrizy bands than the main survey. Although the specific fields for the deep drilling survey have not been finalised at this time, they will likely include EDF-S, CDFS, COSMOS, and XMM-LSS. When available, these data will also be incorporated into the DAWN survey data set.", '4. Spectroscopic follow-up': 'Spectroscopic follow-up is essential for precise redshift measurements, confirming objects of interest, and photoz calibration. Extensive spectroscopic surveys have already been conducted in the EAFs and will be summarised along with the DAWN catalogue release for those regions. This section provides a brief summary of ongoing spectroscopic follow-up in the EDFs.', '4.1. Keck DEIMOS': "The H20 team in Hawaii is conducting an ongoing spectroscopic survey of high-redshift galaxies in the EDF-N and EDF-F using the Deep Extragalactic Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) on the 10 m Keck II telescope. The survey, so far, has focused on Lyman break galaxies (Steidel et al. 1996), also known as 'dropout' galaxies, selected using observed optical colours. Specifically, the program has focused on targeting Lyα emission in overdensities of g band dropout galaxies at z ∼ 4. See Murphree et al. (in prep.) for a full description of the colour selection criteria, overdensity calculations, and results.  \nHighz galaxies in protoclusters are scientifically interesting and convenient observationally since a large number of galaxies can be observed in a single mask. These observations increase the number of high-redshift specz measurements which have immediate impact in achieving the science goals of the DAWN survey and help to improve redshift estimates derived from the photometry.", '4.2. Hobby-Eberly Telescope VIRUS IFU': 'The Texas-Euclid Survey for Lyman-Alpha (TESLA; Chávez Ortiz et al. 2023) is a spectroscopic survey targeting a 10 deg 2 region in the center of EDF-N to generate a large sample ( ∼ 50 000) of Lyα emitting galaxies (LAEs) at redshifts z = 2-3.5 to explore how the physical properties of LAEs correlate with emerg-  \nLyα emission. The combination of these spectra with the deep H20 imaging allows redshift identification of TESLAidentified emission lines via spectral-energy distribution (SED) fitting, and subsequent analyses including the study of the physical properties of identified LAEs. TESLA spectroscopic data is acquired by the Visible Integral-field Replicable Unit Spectrograph (VIRUS; Hill et al. 2018) instrument atop the HobbyEberly Telescope. The VIRUS instrument has a wavelength coverage of 3500-5500 Å with a resolving power of R ∼ 800 making the VIRUS instrument optimal for detecting Lyα emission from galaxies at redshifts z = 1.9-3.5, as well as O ii -emitting galaxies at z < 0.5.', '5. Science goals': "The DAWN survey's deep NIR imaging from Euclid , complemented by matched-depth UV to IR data, facilitates a wide array of scientific analyses. Sharing similarities in wavelength coverage and depth with prior surveys like CANDELS (Grogin et al. 2011) and COSMOS (Scoville 2007), DAWN stands out due to its significantly larger area coverage-thirty times that of the COSMOS field. This expanded scope opens up numerous new analytical possibilities. The primary scientific goals of the DAWN survey revolve around understanding galaxy formation and evolution, particularly in the high-redshift Universe. This section outlines the core objectives for the survey team, although the dataset will support a multitude of other research endeavors as well.", '5.1. UV luminosity functions and mapping reionization': "The Epoch of Reionisation (EoR) marks the period of 'cosmic dawn' in which light from the first galaxies ionised the predominately neutral intergalactic medium (IGM) allowing this radiation to stream freely throughout the Universe. Although observations of the cosmic microwave background (CMB) (Planck Collaboration: Aghanim et al. 2020), highz quasars (Bouwens et al. 2015; Robertson et al. 2015), and Lyα emitting galaxies (Treu et al. 2012; Castellano et al. 2016; Kakiichi et al. 2016) constrain the end of the EoR to z ≳ 6, many important questions remain. When did the EoR begin? What is the relative contribution of rarer luminous galaxies versus more numerous faint galaxies to the budget of ionizing photons (e.g., Naidu et al. 2020; Hutter et al. 2021, 2023)? How does the reionization e ffi ciency and the Lyα escape fraction scale with the local density of galaxies?  \nOne of the primary means of addressing these questions is through measurements of the rest-frame UV luminosity function (UVLF), which describes the co-moving volume density of galaxies as a function of their UV luminosity. Integrating the UVLF not only yields an estimate of the ionizing photon budget at a given redshift but also provides constraints on the unobscured cosmic star-formation rate density (see Madau & Dickinson 2014, for a review). Although deep surveys from HST and JWST have been and will continue to be instrumental for measuring the faint end of the UVLF (e.g., Oesch et al. 2018; Bouwens et al. 2021; Casey et al. 2023), larger survey areas are needed to definitively constrain the abundance of rare luminous sources on the bright end (see Fig. 5). Thanks to the combination of depth and area, the DAWN survey will robustly constrain the bright end of the UVLF to absolute magnitudes of M UV ∼ -24 at z = 8-10, with su ffi cient depth to overlap at fainter magnitudes studied by HST (e.g., Bouwens et al. 2021) and JWST surveys (e.g., Casey et al. 2023; Donnan et al. 2023).  \nFig. 5. Measurements of the ultraviolet luminosity function ϕ at z = 8-10 from the literature (Oesch et al. 2018; Bowler et al. 2020; Bouwens et al. 2021; Finkelstein & Bagley 2022; Adams et al. 2024; Donnan et al. 2023). The red and blue lines show extrapolations to the volume of the DAWN survey based on the best fitting Schechter and double power-law (DPL) functions, with the shaded regions showing associated Poisson uncertainties for the DAWN survey volume. Upper limits based on survey volume are indicated with the horizontal lines. The DAWN volume in each panel assumes an area of 59 deg 2 , a redshift slice of ± 0 . 5 from the redshift bin center, and a Planck Collaboration: Aghanim et al. (2020) Λ CDMcosmology.  \n<!-- image -->  \nFig. 6. Large-scale spatial distribution of the neutral hydrogen fraction at z ≃ 7 (neutral = black, white / gray = ionised) of the MHDEC (i.e. f esc decreases with halo mass, M h) simulation presented in Hutter et al. (2023). The neutral hydrogen fraction shown here is averaged over 3 cells along the line of sight, where each cell has a comoving depth of 312 . 5 h -1 kpc and the dimensionless Hubble constant h = 0 . 6777. The width and height of the box are given in comoving units and correspond to 1 · at z = 7. Blue circles depict galaxies with UV luminosities of at least M UV ≥ -18 and red stars the brightest galaxies in the simulation box with M UV ≥ -21.  \n<!-- image -->  \nTheoretical models predict that the most massive galaxies trace the large-scale structure (LSS) at high redshifts, with lower mass galaxies clustered around them (e.g., Mo & White 1996; Vogelsberger et al. 2014). They also predict that reionization proceeds more e ffi ciently in these over-dense regions (e.g., Treu et al. 2012; Kakiichi et al. 2016; Castellano et al. 2016). However, the details are still poorly understood (Mason & Gronke 2020; Naidu et al. 2020; Larson et al. 2022; Finkelstein & Bagley 2022). For example, what is the observational evidence for the  \nassociation between massive galaxies and LSS at high-redshifts (Hatfield et al. 2018; Harikane et al. 2022)?  \nStructures extending over 0 . · 25-1 . · 0 at z > 3 are rare and the existing pre Euclid Deep Fields do not cover a su ffi cient contiguous area to capture them. Thus, a survey like DAWN is essential to probe the full range of reionization conditions in diverse environments, probing the same variety of structures in the real Universe as those found in cosmological simulations. According to the Millennium simulation (Springel et al. 2005), the DAWNsurvey will find ∼ 125-250 proto-structures, i.e., progenitors of modern day > 5 × 10 14 M ⊙ clusters, and ∼ 1250-2500 regions with densities more than three times the mean density of the Universe at 3 < z < 8. For example, the comoving volume of the DAWN survey at 6 . 5 < z < 7 . 5 will contain more than 100 DM halos with masses ( M 200) greater than 10 12 M ⊙ ; with only 5 ± 2 such massive halos expected in a survey like COSMOS (Despali et al. 2016). Figure 6 shows reionization bubbles around luminous galaxies at z ∼ 7 from the ASTREUS simulation framework (Hutter et al. 2023) in a similar area as the COSMOS field.", '5.2. Galaxy stellar mass function': 'Among the most outstanding problems in astronomy today is understanding the nature and formation mechanism of the most massive galaxies ( M ⋆ ≳ 3 × 10 10 M ⊙ ) in the early Universe ( z ≳ 2). These rare systems are the best candidate progenitors of local early-type galaxies with M ⋆ ∼ 10 12 M ⊙ . Some have been shown to be surprisingly mature, having no ongoing starformation and well-formed discs in contrast with the hierarchical formation scenario (e.g., Toft et al. 2017). In a hierarchical model, the mapping between the galaxies and host dark matter haloes is controlled by the stellar mass-halo mass relation (SMHM). Di ff erent mappings generate di ff erent merger histories as well as di ff erent star formation histories (e.g. Grylls et al. 2019; Fu et al. 2022). The shape of the highz galaxy stellar mass function (SMF) is particularly valuable in this respect as it provides a benchmark for the evolution of galaxies at lower redshifts. For example, it has been shown that an abundance of massive galaxies at high redshift is more consistent with the nearly  \nFig. 7. Stellar mass function, Φ , measurements (hatched regions) from HST (S + 21; Stefanon et al. 2021), the COSMOS field (W + 22; Weaver et al. 2023), and JWST (N-C + 23; Navarro-Carrera et al. 2024) in three redshift bins: z ∼ 6 (left), 7 (middle), and 8 (right). The dashed lines show extrapolations to higher masses for the DAWN survey volume (calculated in the same way as in Fig. 5) assuming the corresponding literature Schechter function fits, and the accompanying shaded regions show estimated uncertainties. Upper limits for empty bins for the respective survey are indicated with horizontal lines. Note that Due to the shallower IRAC data in EDF-S (see Table 2) the z ∼ 8 bin assumes a smaller e ff ective area of 39 deg 2 . The grey shaded regions indicate the theoretical upper limit of the SMF in each redshift bins based on the Despali et al. (2016) halo mass function assuming a fixed baryon fraction of 0.018 as in Weaver et al. (2023).  \n<!-- image -->  \n/circledot  \n/circledot  \n/circledot  \nflat SFHs retrieved from galaxies at lower redshifts, which suggest that galaxies have grown much of their stellar mass at early epochs (Fu et al. 2022).  \nTo understand the evolution of these systems one needs to address the following questions: How fast did massive galaxies build up their mass? Of those that have quenched, what mechanisms are responsible? What is the number density of di ff erent populations of galaxies at z = 3-8? How does environment determine their existing and future mass?  \nPursuing these questions with existing resources has already yielded surprises. While detailed follow-up of individual objects have clarified their unusual properties (e.g., Toft et al. 2017), statistical arguments as to their demographics - namely the galaxy stellar mass function (SMF) - have provided meaningful clues (Cole et al. 2001; Adams et al. 2021; McLeod et al. 2021; Stefanon et al. 2021; Weaver et al. 2022). Its shape and evolution with time is sensitive not only to star-formation histories and galaxy mergers, but also to the associated physical processes thought responsible for ceasing galaxy growth such as heating of gas by accreting central supermassive black holes or by supernovae explosions, gas removal by outflows, or by a host of other proposed scenarios (Dubois et al. 2013; Gabor & Davé 2015).  \nMassive galaxies are some of the best laboratories for testing galaxy formation theories. However, a comprehensive view of massive galaxy evolution cannot come from shallow large-area surveys like SDSS or GAMA, which are restricted to z < 0 . 5, nor from deep but narrow surveys like HUDF or CANDELS, which reach z ∼ 9-10 but only cover a total area of < 0.25 deg 2 (see Finkelstein 2016, for a review). Only a handful of highz detections have ∼ 5 × 10 10 M ⊙ in the small cosmic volume probed by HST, with no M ⋆ > 10 11 M ⊙ candidates found at z > 5. Even the largest contiguous HST galaxy survey, COSMOS, has not detected massive galaxy candidates beyond z ∼ 5 (Weaver et al. 2023).  \nThe DAWN survey will measure the shape and evolution of the SMF to z ∼ 8 with directly measured stellar masses from Spitzer / IRAC. Thanks to its large area coverage, the DAWN survey will reduce Poisson uncertainties by a factor of ∼ 6 compared to the Weaver et al. (2023) SMF from COSMOS and will pro-  \nthe first robust constraints on the number density of ultramassive galaxies ( M ⋆ > 10 11 M ⊙ ) at z = 6-8 (see Fig. 7).  \nThe large area of the DAWN survey will also improve measurements of the SMF for quiescent and star-forming galaxies as well as galaxies in di ff erent environments. Colour-colour selection criteria are often used to separate star-forming and quiescent galaxies (Williams et al. 2009; Arnouts et al. 2013; Ilbert et al. 2010; Davidzon et al. 2017; Gould et al. 2023). Weaver et al. (2023) only find 52 quiescent galaxies at z = 4.5-6.5 in 1.3 deg 2 of the COSMOS field which limited their analysis of the quiescent SMF to z < 4 . 5. Assuming a similar source density, the DAWN survey will detect ∼ 2000 quiescent galaxies at z = 4.5-6.5 providing new constraints on the quiescent SMF in the early Universe. So far, measurements of the SMF as a function of environment have been limited to redshifts z < 3 (Baldry et al. 2006; Peng et al. 2010; Papovich et al. 2018; Taylor et al. 2023b). The DAWN survey will not only expand this type of analysis to higher redshifts but will also be able to explore more extreme under- or over-dense environments thanks to the large contiguous areas of the EDFs.', '5.3. Origins of large-scale structure at high-redshift': "The current standard model for cosmology, Lambda Cold Dark Matter ( Λ CDM), describes the growth of structure from density fluctuations in the primordial plasma to the LSS that we observe today. The Λ CDM model has been successful in describing the power spectra of galaxies and the CMB, but recent work has found tensions (Abdalla et al. 2022) in two of its key parameters: H 0, the Hubble rate at present day (e.g., Planck Collaboration: Aghanim et al. 2020; Riess et al. 2022), and σ 8, the amplitude of matter density fluctuations at present day (e.g., Planck Collaboration: Aghanim et al. 2020; Asgari et al. 2021; Heymans et al. 2021; Abbott et al. 2022; Amon et al. 2022). Both tensions arise between early (CMB-based) and late (galaxy-based) methods. While H 0 has been measured across a wide range of redshifts, σ 8 remains unconstrained at z ∼ 3-7.  \nThe DAWN data set will allow us to measure galaxy clustering at these high redshifts. As galaxies are a biased tracer of the underlying matter distribution, we will assume a linear galaxy  \nFig. 8. The redshift evolution of linear galaxy bias. The early prediction from Tegmark & Peebles (1998) is shown in solid grey, and more recent models separated by stellar mass from Moster et al. (2010) are shown as dashed grey curves. Highz measurements for dropout-selected samples from Beck et al. (2020) and Harikane et al. (2022) are shown in red and green, respectively. Lowz measurements for two stellar masses from Ishikawa et al. (2020) are shown in blue and purple. The DAWN survey will allow us to constrain bias as a function of redshift and stellar mass in the shaded region.  \n<!-- image -->  \nbias b gal. This galaxy bias is similarly unconstrained at z ∼ 37 and is degenerate with σ 8 in two-point clustering measurements. At high redshift, we can break this degeneracy by crosscorrelating galaxy clustering measurements with CMB lensing, or by combining galaxy bias measurements with higher order statistics (e.g. Repp & Szapudi 2022). Using HSC data from SSP and the University of Hawaii (SSP + UH; Tanaka et al. 2017) in the ∼ 2 deg 2 COSMOS field, Beck et al. (2020) measured linear galaxy bias out to z ∼ 6 for g , r , and i band dropouts. We will extend this analysis to the full 59 deg 2 of the DAWN survey and use its robust photometric redshifts to select our galaxy samples, which should reduce the uncertainties by more than a factor of three. By cross-correlating our galaxy clustering measurements with CMB lensing (e.g. Planck Collaboration: Aghanim et al. 2020), we can constrain σ 8 at high-redshift and compare our result with constraints from previous work (Murphree et al. in prep).  \nThe total volume of the DAWN survey out to z ∼ 7 will be about 3.8 Gpc 3 . This volume is large enough to include several extreme density fluctuations. By applying advanced statistical techniques such as su ffi cient statistics and indicator functions, we can double this volume and make robust estimates of cosmological parameters (Wolk et al. 2015; Repp & Szapudi 2022). The DAWN data set will allow us to constrain parameters (see Fig. 8) well beyond the z ∼ 2 . 5 forecasted for the photometric Euclid data set (Euclid Collaboration: Ili'c et al. 2022).", '6. Summary': "The DAWN survey is a deep multiwavelength imaging survey that covers ∼ 59 deg 2 in the Euclid Deep and Auxiliary fields. Deep space-based NIR image data from Euclid NISP and Spitzer / IRAC form the core of the DAWN data set  \nalong with complementary ground-based UV-optical data from CFHT / MegaCam, Subaru / HSC, and future observations from the Vera Rubin Observatory. The DAWN survey aims to provide catalogues for the widest area collection of extragalactic deep fields with consistent data reduction. These data will be essential for photometric redshift calibration of the Euclid Wide Survey and will be the reference data set for extragalactic studies in the Euclid Deep and Auxiliary fields.  \nThe DAWN survey is designed to address a variety of science goals including measuring the galaxy stellar mass function to z = 8, mapping reionization, studying the formation of largescale structure, and characterising the first quenched galaxies. Data collection for the survey is ongoing with the ground-based component planned to be completed in the next few years and the Euclid observations scheduled to be completed by 2030. A companion paper, Euclid Collaboration: Zalesky et al. (2024), will provide the first DAWN data release of photometric catalogues and galaxy physical parameters in EDF-N and EDF-F. Future publications will present subsequent data releases of image data and catalogues that include all of the DAWN fields. The DAWN data have immediate value for studying galaxy formation and evolution in the high-redshift Universe and that legacy value will only increase as the survey is completed.  \nAcknowledgements. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant DNRF140. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid , in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum für Luft- und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d'Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space O ffi ce (SSO), and the United Kingdom Space Agency. 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Marconi, 00185 Roma, Italy\n- 32 Minnesota Institute for Astrophysics, University of Minnesota, 116 Church St SE, Minneapolis, MN 55455, USA\n- 33 Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan\n- 34 Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan\n- 35 Institut d\'Astrophysique de Paris, 98bis Boulevard Arago, 75014, Paris, France\n- 36 ESAC / ESA, Camino Bajo del Castillo, s / n., Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Spain\n- 37 School of Mathematics and Physics, University of Surrey, Guildford, Surrey, GU2 7XH, UK\n- 38 INAF-Osservatorio Astronomico di Brera, Via Brera 28, 20122 Milano, Italy\n- 39 INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93 / 3, 40129 Bologna, Italy\n- 40 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191, Gif-sur-Yvette, France\n- 41 SISSA, International School for Advanced Studies, Via Bonomea 265, 34136 Trieste TS, Italy\n- 42 INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy\n- 43 INFN, Sezione di Trieste, Via Valerio 2, 34127 Trieste TS, Italy\n- 44 IFPU, Institute for Fundamental Physics of the Universe, via Beirut 2, 34151 Trieste, Italy  \n- 45 Dipartimento di Fisica e Astronomia, Università di Bologna, Via Gobetti 93 / 2, 40129 Bologna, Italy\n- 46 INFN-Sezione di Bologna, Viale Berti Pichat 6 / 2, 40127 Bologna, Italy\n- 47 INAF-Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy\n- 48 Dipartimento di Fisica, Università di Genova, Via Dodecaneso 33, 16146, Genova, Italy\n- 49 INFN-Sezione di Genova, Via Dodecaneso 33, 16146, Genova, Italy\n- 50 Department of Physics "E. Pancini", University Federico II, Via Cinthia 6, 80126, Napoli, Italy\n- 51 INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy\n- 52 INFN section of Naples, Via Cinthia 6, 80126, Napoli, Italy\n- 53 Dipartimento di Fisica, Università degli Studi di Torino, Via P. Giuria 1, 10125 Torino, Italy\n- 54 INFN-Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy\n- 55 INAF-IASF Milano, Via Alfonso Corti 12, 20133 Milano, Italy\n- 56 Institut de Física d\'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain\n- 57 Port d\'Informació Científica, Campus UAB, C. Albareda s / n, 08193 Bellaterra (Barcelona), Spain\n- 58 Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, 52056 Aachen, Germany\n- 59 Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s / n, 08193 Barcelona, Spain\n- 60 Institut d\'Estudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC, 08860 Castelldefels, Barcelona, Spain\n- 61 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, via Piero Gobetti 93 / 2, 40129 Bologna, Italy\n- 62 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, Viale Berti Pichat 6 / 2, 40127 Bologna, Italy\n- 63 Instituto de Astrofísica de Canarias, Calle Vía Láctea s / n, 38204, San Cristóbal de La Laguna, Tenerife, Spain\n- 64 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK\n- 65 Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK\n- 66 European Space Agency / ESRIN, Largo Galileo Galilei 1, 00044 Frascati, Roma, Italy\n- 67 Université Claude Bernard Lyon 1, CNRS / IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, F-69100, France\n- 68 Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland\n- 69 UCB Lyon 1, CNRS / IN2P3, IUF, IP2I Lyon, 4 rue Enrico Fermi, 69622 Villeurbanne, France\n- 70 Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Edifício C8, Campo Grande, PT1749-016 Lisboa, Portugal\n- 71 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa, Campo Grande, 1749-016 Lisboa, Portugal\n- 72 INAF-Istituto di Astrofisica e Planetologia Spaziali, via del Fosso del Cavaliere, 100, 00100 Roma, Italy\n- 73 Université Paris-Saclay, CNRS, Institut d\'astrophysique spatiale, 91405, Orsay, France\n- 74 INFN-Padova, Via Marzolo 8, 35131 Padova, Italy\n- 75 School of Physics, HH Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol, BS8 1TL, UK\n- 76 Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Via Irnerio 46, 40126 Bologna, Italy\n- 77 INAF-Osservatorio Astronomico di Padova, Via dell\'Osservatorio 5, 35122 Padova, Italy\n- 78 Dipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, Via Celoria 16, 20133 Milano, Italy  \n- 79 Department of Physics, Lancaster University, Lancaster, LA1 4YB, UK\n- 80 von Hoerner & Sulger GmbH, Schlossplatz 8, 68723 Schwetzingen, Germany\n- 81 Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark\n- 82 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany\n- 83 Department of Physics and Helsinki Institute of Physics, Gustaf Hällströmin katu 2, 00014 University of Helsinki, Finland\n- 84 Aix-Marseille Université, CNRS / IN2P3, CPPM, Marseille, France\n- 85 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK\n- 86 Université de Genève, Département de Physique Théorique and Centre for Astroparticle Physics, 24 quai Ernest-Ansermet, CH1211 Genève 4, Switzerland\n- 87 Department of Physics, P.O. Box 64, 00014 University of Helsinki, Finland\n- 88 Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland\n- 89 Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, 0315 Oslo, Norway\n- 90 NOVA optical infrared instrumentation group at ASTRON, Oude Hoogeveensedijk 4, 7991PD, Dwingeloo, The Netherlands\n- 91 Centre de Calcul de l\'IN2P3 / CNRS, 21 avenue Pierre de Coubertin 69627 Villeurbanne Cedex, France\n- 92 Universität Bonn, Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany\n- 93 Department of Physics, Institute for Computational Cosmology, Durham University, South Road, DH1 3LE, UK\n- 94 Université Côte d\'Azur, Observatoire de la Côte d\'Azur, CNRS, Laboratoire Lagrange, Bd de l\'Observatoire, CS 34229, 06304 Nice cedex 4, France\n- 95 Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France\n- 96\n- University of Applied Sciences and Arts of Northwestern Switzerland, School of Engineering, 5210 Windisch, Switzerland\n- 97 European Space Agency / ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands\n- 98 School of Mathematics, Statistics and Physics, Newcastle University, Herschel Building, Newcastle-upon-Tyne, NE1 7RU, UK\n- 99 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade 120, DK-8000 Aarhus C, Denmark\n- 100 Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada\n- 101 Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada  \n102  \nPerimeter Institute for Theoretical Physics, Waterloo, Ontario N2L  \n2Y5, Canada  \n- 103 Space Science Data Center, Italian Space Agency, via del Politecnico snc, 00133 Roma, Italy\n- 104 Centre National d\'Etudes Spatiales - Centre spatial de Toulouse, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9, France\n- 105 Institute of Space Science, Str. Atomistilor, nr. 409 M˘agurele, Ilfov, 077125, Romania\n- 106 Departamento de Astrofísica, Universidad de La Laguna, 38206, La Laguna, Tenerife, Spain\n- 107 Dipartimento di Fisica e Astronomia "G. Galilei", Università di Padova, Via Marzolo 8, 35131 Padova, Italy\n- 108 Institut für Theoretische Physik, University of Heidelberg, Philosophenweg 16, 69120 Heidelberg, Germany\n- 109 Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, 31400 Toulouse, France\n- 110 Université St Joseph; Faculty of Sciences, Beirut, Lebanon\n- 111 Departamento de Física, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile\n- 112 Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstr. 25 / 8, 6020 Innsbruck, Austria\n- 113 Satlantis, University Science Park, Sede Bld 48940, Leioa-Bilbao, Spain\n- 114 Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Avenida Complutense 40, 28040 Madrid, Spain\n- 115 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal\n- 116 Universidad Politécnica de Cartagena, Departamento de Electrónica y Tecnología de Computadoras, Plaza del Hospital 1, 30202 Cartagena, Spain\n- 117 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands\n- 118 INFN-Bologna, Via Irnerio 46, 40126 Bologna, Italy\n- 119 INAF, Istituto di Radioastronomia, Via Piero Gobetti 101, 40129 Bologna, Italy\n- 120 Junia, EPA department, 41 Bd Vauban, 59800 Lille, France\n- 121 ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing, Via Magnanelli 2, Bologna, Italy\n- 122 Instituto de Física Teórica UAM-CSIC, Campus de Cantoblanco, 28049 Madrid, Spain\n- 123 CERCA / ISO, Department of Physics, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106, USA\n- 124 Laboratoire Univers et Théorie, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS, 92190 Meudon, France\n- 125 Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara, Via Giuseppe Saragat 1, 44122 Ferrara, Italy\n- 126 Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara, Via Giuseppe Saragat 1, 44122 Ferrara, Italy\n- 127 Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, 67000 Strasbourg, France\n- 128 Dipartimento di Fisica - Sezione di Astronomia, Università di Trieste, Via Tiepolo 11, 34131 Trieste, Italy\n- 129 NASA Ames Research Center, Mo ff ett Field, CA 94035, USA\n- 130 Bay Area Environmental Research Institute, Mo ff ett Field, California 94035, USA\n- 131 Institute Lorentz, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands\n- 132 Department of Physics & Astronomy, University of California Irvine, Irvine CA 92697, USA\n- 133 Departamento Física Aplicada, Universidad Politécnica de Cartagena, Campus Muralla del Mar, 30202 Cartagena, Murcia, Spain\n- 134 Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK\n- 135 CEA Saclay, DFR / IRFU, Service d\'Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France\n- 136 Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK\n- 137 Department of Computer Science, Aalto University, PO Box 15400, Espoo, FI-00 076, Finland\n- 138 Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB), German Centre for Cosmological Lensing (GCCL), 44780 Bochum, Germany\n- 139 DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 155, 2200 Copenhagen, Denmark\n- 140 Instituto de Astrofísica de Canarias (IAC); Departamento de Astrofísica, Universidad de La Laguna (ULL), 38200, La Laguna, Tenerife, Spain\n- 141 Université PSL, Observatoire de Paris, Sorbonne Université, CNRS, LERMA, 75014, Paris, France\n- 142 Université Paris-Cité, 5 Rue Thomas Mann, 75013, Paris, France\n- 143 Department of Physics and Astronomy, Vesilinnantie 5, 20014 University of Turku, Finland\n- 144 Serco for European Space Agency (ESA), Camino bajo del Castillo, s / n, Urbanizacion Villafranca del Castillo, Villanueva de la Cañada, 28692 Madrid, Spain\n- 145 ARC Centre of Excellence for Dark Matter Particle Physics, Melbourne, Australia  \n- 146 Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia\n- 147 School of Physics and Astronomy, Queen Mary University of London, Mile End Road, London E1 4NS, UK\n- 148 Department of Physics and Astronomy, University of the Western Cape, Bellville, Cape Town, 7535, South Africa\n- 149 ICTP South American Institute for Fundamental Research, Instituto de Física Teórica, Universidade Estadual Paulista, São Paulo, Brazil\n- 150 Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, Stockholm, SE-106 91, Sweden\n- 151 Astrophysics Group, Blackett Laboratory, Imperial College London, London SW7 2AZ, UK\n- 152 Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 53, Avenue des Martyrs, 38000, Grenoble, France\n- 153 INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy\n- 154 Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy\n- 155 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal\n- 156 Zentrum für Astronomie, Universität Heidelberg, Philosophenweg 12, 69120 Heidelberg, Germany\n- 157 Thales Alenia Space - Euclid satellite Prime contractor, Strada Antica di Collegno 253, 10146 Torino, Italy\n- 158 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK\n- 159 Department of Astrophysics, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland\n- 160 Dipartimento di Fisica, Università degli studi di Genova, and INFN-Sezione di Genova, via Dodecaneso 33, 16146, Genova, Italy\n- 161 Theoretical astrophysics, Department of Physics and Astronomy, Uppsala University, Box 515, 751 20 Uppsala, Sweden\n- 162 Department of Physics and Astronomy, University of California, Davis, CA 95616, USA\n- 163 Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544, USA\n- 164 Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA\n- 165 Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, 10010, New York, NY, USA\n- 166 School of Physics & Astronomy, University of Southampton, Highfield Campus, Southampton SO17 1BJ, UK', 'Appendix A: Image data footprints': "Figures A.1 and A.2 show footprints of the image data compiled by the DAWN survey in the Euclid Deep and Auxiliary fields.  \nFig. A.1. Footprints of the DAWN survey image data in the Euclid Deep Fields. Note that the Rubin / LSST footprint in EDF-S shows the expected pointing pattern for the EDF-S Deep Drilling Field and may change once the survey begins (Ivezi'c et al. 2019).  \n<!-- image -->  \n64  \n·  \nFig. A.2. Footprints of the DAWN survey image data in the EAFs. The coloured lines show the extent of the image data indicated in the legend. Note that the EAF footprints are approximations based on the Euclid survey plan. Updated footprints that to reflect the actual Euclid coverage in the EAFs will be provided along with subsequent DAWN data releases.  \n<!-- image -->"}