Euclid preparation: I. the Euclid Wide Survey

R. Scaramella; J. Amiaux; Y. Mellier; C. Burigana; C. S. Carvalho; 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; T. Maciaszek; M. Meneghetti; L. Miller; R. Nakajima; S. M. Niemi; F. Pasian; W. J. Percival; S. Pottinger; 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; O. Lahav; S. Ligori; P. B. Lilje; I. Lloro; O. Mansutti; O. Marggraf; K. Markovic; F. Marulli; R. Massey; S. Maurogordato; 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; D. Di Ferdinando; G. Fabbian; R. Farinelli; S. Galeotta; 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; H. Dole; M. Fabricius; M. Farina; P. G. Ferreira; F. Finelli; P. Flose-Reimberg; S. Fotopoulou; 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

doi:10.1051/0004-6361/202141938

Euclid preparation: I. the Euclid Wide Survey

R. Scaramella, J. Amiaux, Y. Mellier, C. Burigana, C. S. Carvalho, 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 AlvarezG. 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, T. Maciaszek, M. Meneghetti, L. Miller, R. Nakajima, S. M. Niemi, F. Pasian, W. J. Percival, S. Pottinger, 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, O. Lahav, S. Ligori, P. B. Lilje, I. Lloro, O. Mansutti, O. Marggraf, K. Markovic, F. Marulli, R. Massey, S. Maurogordato, 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, D. Di Ferdinando, G. Fabbian, R. Farinelli, S. Galeotta, 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, H. Dole, M. Fabricius, M. Farina, P. G. Ferreira, F. Finelli, P. Flose-Reimberg, S. Fotopoulou, 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

Research output: Contribution to journal › Article › peer-review

111 Scopus citations

Abstract

Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 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.

Original language	English (US)
Article number	A112
Journal	Astronomy and Astrophysics
Volume	662
DOIs	https://doi.org/10.1051/0004-6361/202141938
State	Published - Jun 1 2022
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Dark energy
Dark matter
Methods: numerical
Space vehicles
Surveys

Access to Document

10.1051/0004-6361/202141938

Cite this

Scaramella, R., Amiaux, J., Mellier, Y., Burigana, C., Carvalho, C. S., Cuillandre, J. C., Da Silva, A., Derosa, A., Dinis, J., Maiorano, E., Maris, M., Tereno, I., Laureijs, R., Boenke, T., Buenadicha, G., Dupac, X., Gaspar Venancio, L. M., Gómez-Álvarez, P., Hoar, J., ... Whittaker, L. (2022). Euclid preparation: I. the Euclid Wide Survey. Astronomy and Astrophysics, 662, Article A112. https://doi.org/10.1051/0004-6361/202141938

@article{97b404a54cbc425084f378a72bb241c5,

title = "Euclid preparation: I. the Euclid Wide Survey",

abstract = "Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 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.",

keywords = "Dark energy, Dark matter, Methods: numerical, Space vehicles, Surveys",

author = "R. Scaramella and J. Amiaux and Y. Mellier and C. Burigana and Carvalho, {C. S.} and Cuillandre, {J. C.} and {Da Silva}, A. and A. Derosa and J. Dinis and E. Maiorano and M. Maris and I. Tereno and R. Laureijs and T. Boenke and G. Buenadicha and X. Dupac and {Gaspar Venancio}, {L. M.} and P. G{\'o}mez-{\'A}lvarez and J. Hoar and {Lorenzo Alvarez}, J. and Racca, {G. D.} and G. Saavedra-Criado and J. Schwartz and R. Vavrek and M. Schirmer and H. Aussel and R. Azzollini and Cardone, {V. F.} and M. Cropper and A. Ealet and B. Garilli and W. Gillard and Granett, {B. R.} and L. Guzzo and H. Hoekstra and K. Jahnke and T. Kitching and T. Maciaszek and M. Meneghetti and L. Miller and R. Nakajima and Niemi, {S. M.} and F. Pasian and Percival, {W. J.} and S. Pottinger and M. Sauvage and M. Scodeggio and S. Wachter and A. Zacchei and N. Aghanim and A. Amara and T. Auphan and N. Auricchio and S. Awan and A. Balestra and R. Bender and C. Bodendorf and D. Bonino and E. Branchini and S. Brau-Nogue and M. Brescia and Candini, {G. P.} and V. Capobianco and C. Carbone and Carlberg, {R. G.} and J. Carretero and R. Casas and Castander, {F. J.} and M. Castellano and S. Cavuoti and A. Cimatti and R. Cledassou and G. Congedo and Conselice, {C. J.} and L. Conversi and Y. Copin and L. Corcione and A. Costille and F. Courbin and H. Degaudenzi and M. Douspis and F. Dubath and Duncan, {C. A.J.} and S. Dusini and S. Farrens and S. Ferriol and P. Fosalba and N. Fourmanoit and M. Frailis and E. Franceschi and P. Franzetti and M. Fumana and B. Gillis and C. Giocoli and A. Grazian and F. Grupp and Haugan, {S. V.H.} and W. Holmes and F. Hormuth and P. Hudelot and S. Kermiche and A. Kiessling and M. Kilbinger and R. Kohley and B. Kubik and M. K{\"u}mmel and M. Kunz and H. Kurki-Suonio and O. Lahav and S. Ligori and Lilje, {P. B.} and I. Lloro and O. Mansutti and O. Marggraf and K. Markovic and F. Marulli and R. Massey and S. Maurogordato and M. Melchior and E. Merlin and G. Meylan and Mohr, {J. J.} and M. Moresco and B. Morin and L. Moscardini and E. Munari and Nichol, {R. C.} and C. Padilla and S. Paltani and J. Peacock and K. Pedersen and V. Pettorino and S. Pires and M. Poncet and L. Popa and L. Pozzetti and F. Raison and R. Rebolo and J. Rhodes and Rix, {H. W.} and M. Roncarelli and E. Rossetti and R. Saglia and P. Schneider and T. Schrabback and A. Secroun and G. Seidel and S. Serrano and C. Sirignano and G. Sirri and J. Skottfelt and L. Stanco and Starck, {J. L.} and P. Tallada-Cresp{\'i} and D. Tavagnacco and Taylor, {A. N.} and Teplitz, {H. I.} and R. Toledo-Moreo and F. Torradeflot and M. Trifoglio and Valentijn, {E. A.} and L. Valenziano and {Verdoes Kleijn}, {G. A.} and Y. Wang and N. Welikala and J. Weller and M. Wetzstein and G. Zamorani and J. Zoubian and S. Andreon and M. Baldi and S. Bardelli and A. Boucaud and S. Camera and {Di Ferdinando}, D. and G. Fabbian and R. Farinelli and S. Galeotta and J. Graci{\'a}-Carpio and D. Maino and E. Medinaceli and S. Mei and C. Neissner and G. Polenta and A. Renzi and E. Romelli and C. Rosset and F. Sureau and M. Tenti and T. Vassallo and E. Zucca and C. Baccigalupi and A. Balaguera-Antol{\'i}nez and P. Battaglia and A. Biviano and S. Borgani and E. Bozzo and R. Cabanac and A. Cappi and S. Casas and G. Castignani and C. Colodro-Conde and J. Coupon and Courtois, {H. M.} and J. Cuby and {De La Torre}, S. and S. Desai and H. Dole and M. Fabricius and M. Farina and Ferreira, {P. G.} and F. Finelli and P. Flose-Reimberg and S. Fotopoulou and K. Ganga and G. Gozaliasl and Hook, {I. M.} and E. Keihanen and Kirkpatrick, {C. C.} and P. Liebing and V. Lindholm and G. Mainetti and M. Martinelli and N. Martinet and M. Maturi and McCracken, {H. J.} and Metcalf, {R. B.} and G. Morgante and J. Nightingale and A. Nucita and L. Patrizii and D. Potter and G. Riccio and S{\'a}nchez, {A. G.} and D. Sapone and Schewtschenko, {J. A.} and M. Schultheis and V. Scottez and R. Teyssier and I. Tutusaus and J. Valiviita and M. Viel and W. Vriend and L. Whittaker",

note = "Publisher Copyright: {\textcopyright} ESO 2022.",

year = "2022",

month = jun,

day = "1",

doi = "10.1051/0004-6361/202141938",

language = "English (US)",

volume = "662",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Scaramella, R, Amiaux, J, Mellier, Y, Burigana, C, Carvalho, CS, Cuillandre, JC, Da Silva, A, Derosa, A, Dinis, J, Maiorano, E, Maris, M, Tereno, I, Laureijs, R, Boenke, T, Buenadicha, G, Dupac, X, Gaspar Venancio, LM, Gómez-Álvarez, P, Hoar, J, Lorenzo Alvarez, J, Racca, GD, Saavedra-Criado, G, Schwartz, J, Vavrek, R, Schirmer, M, Aussel, H, Azzollini, R, Cardone, VF, Cropper, M, Ealet, A, Garilli, B, Gillard, W, Granett, BR, Guzzo, L, Hoekstra, H, Jahnke, K, Kitching, T, Maciaszek, T, Meneghetti, M, Miller, L, Nakajima, R, Niemi, SM, Pasian, F, Percival, WJ, Pottinger, S, Sauvage, M, Scodeggio, M, Wachter, S, Zacchei, A, Aghanim, N, Amara, A, Auphan, T, Auricchio, N, Awan, S, Balestra, A, Bender, R, Bodendorf, C, Bonino, D, Branchini, E, Brau-Nogue, S, Brescia, M, Candini, GP, Capobianco, V, Carbone, C, Carlberg, RG, Carretero, J, Casas, R, Castander, FJ, Castellano, M, Cavuoti, S, Cimatti, A, Cledassou, R, Congedo, G, Conselice, CJ, Conversi, L, Copin, Y, Corcione, L, Costille, A, Courbin, F, Degaudenzi, H, Douspis, M, Dubath, F, Duncan, CAJ, Dusini, S, Farrens, S, Ferriol, S, Fosalba, P, Fourmanoit, N, Frailis, M, Franceschi, E, Franzetti, P, Fumana, M, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Haugan, SVH, Holmes, W, Hormuth, F, Hudelot, P, Kermiche, S, Kiessling, A, Kilbinger, M, Kohley, R, Kubik, B, Kümmel, M, Kunz, M, Kurki-Suonio, H, Lahav, O, Ligori, S, Lilje, PB, Lloro, I, Mansutti, O, Marggraf, O, Markovic, K, Marulli, F, Massey, R, Maurogordato, S, Melchior, M, Merlin, E, Meylan, G, Mohr, JJ, Moresco, M, Morin, B, Moscardini, L, Munari, E, Nichol, RC, Padilla, C, Paltani, S, Peacock, J, Pedersen, K, Pettorino, V, Pires, S, Poncet, M, Popa, L, Pozzetti, L, Raison, F, Rebolo, R, Rhodes, J, Rix, HW, Roncarelli, M, Rossetti, E, Saglia, R, Schneider, P, Schrabback, T, Secroun, A, Seidel, G, Serrano, S, Sirignano, C, Sirri, G, Skottfelt, J, Stanco, L, Starck, JL, Tallada-Crespí, P, Tavagnacco, D, Taylor, AN, Teplitz, HI, Toledo-Moreo, R, Torradeflot, F, Trifoglio, M, Valentijn, EA, Valenziano, L, Verdoes Kleijn, GA, Wang, Y, Welikala, N, Weller, J, Wetzstein, M, Zamorani, G, Zoubian, J, Andreon, S, Baldi, M, Bardelli, S, Boucaud, A, Camera, S, Di Ferdinando, D, Fabbian, G, Farinelli, R, Galeotta, S, Graciá-Carpio, J, Maino, D, Medinaceli, E, Mei, S, Neissner, C, Polenta, G, Renzi, A, Romelli, E, Rosset, C, Sureau, F, Tenti, M, Vassallo, T, Zucca, E, Baccigalupi, C, Balaguera-Antolínez, A, Battaglia, P, Biviano, A, Borgani, S, Bozzo, E, Cabanac, R, Cappi, A, Casas, S, Castignani, G, Colodro-Conde, C, Coupon, J, Courtois, HM, Cuby, J, De La Torre, S, Desai, S, Dole, H, Fabricius, M, Farina, M, Ferreira, PG, Finelli, F, Flose-Reimberg, P, Fotopoulou, S, Ganga, K, Gozaliasl, G, Hook, IM, Keihanen, E, Kirkpatrick, CC, Liebing, P, Lindholm, V, Mainetti, G, Martinelli, M, Martinet, N, Maturi, M, McCracken, HJ, Metcalf, RB, Morgante, G, Nightingale, J, Nucita, A, Patrizii, L, Potter, D, Riccio, G, Sánchez, AG, Sapone, D, Schewtschenko, JA, Schultheis, M, Scottez, V, Teyssier, R, Tutusaus, I, Valiviita, J, Viel, M, Vriend, W & Whittaker, L 2022, 'Euclid preparation: I. the Euclid Wide Survey', Astronomy and Astrophysics, vol. 662, A112. https://doi.org/10.1051/0004-6361/202141938

TY - JOUR

T1 - Euclid preparation

T2 - I. the Euclid Wide Survey

AU - Scaramella, R.

AU - Amiaux, J.

AU - Mellier, Y.

AU - Burigana, C.

AU - Carvalho, C. S.

AU - Cuillandre, J. C.

AU - Da Silva, A.

AU - Derosa, A.

AU - Dinis, J.

AU - Maiorano, E.

AU - Maris, M.

AU - Tereno, I.

AU - Laureijs, R.

AU - Boenke, T.

AU - Buenadicha, G.

AU - Dupac, X.

AU - Gaspar Venancio, L. M.

AU - Gómez-Álvarez, P.

AU - Hoar, J.

AU - Lorenzo Alvarez, J.

AU - Racca, G. D.

AU - Saavedra-Criado, G.

AU - Schwartz, J.

AU - Vavrek, R.

AU - Schirmer, M.

AU - Aussel, H.

AU - Azzollini, R.

AU - Cardone, V. F.

AU - Cropper, M.

AU - Ealet, A.

AU - Garilli, B.

AU - Gillard, W.

AU - Granett, B. R.

AU - Guzzo, L.

AU - Hoekstra, H.

AU - Jahnke, K.

AU - Kitching, T.

AU - Maciaszek, T.

AU - Meneghetti, M.

AU - Miller, L.

AU - Nakajima, R.

AU - Niemi, S. M.

AU - Pasian, F.

AU - Percival, W. J.

AU - Pottinger, S.

AU - Sauvage, M.

AU - Scodeggio, M.

AU - Wachter, S.

AU - Zacchei, A.

AU - Aghanim, N.

AU - Amara, A.

AU - Auphan, T.

AU - Auricchio, N.

AU - Awan, S.

AU - Balestra, A.

AU - Bender, R.

AU - Bodendorf, C.

AU - Bonino, D.

AU - Branchini, E.

AU - Brau-Nogue, S.

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PY - 2022/6/1

Y1 - 2022/6/1

N2 - Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 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.

AB - Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 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.

KW - Dark energy

KW - Dark matter

KW - Methods: numerical

KW - Space vehicles

KW - Surveys

UR - http://www.scopus.com/inward/record.url?scp=85133460463&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85133460463&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202141938

DO - 10.1051/0004-6361/202141938

M3 - Article

AN - SCOPUS:85133460463

SN - 0004-6361

VL - 662

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A112

ER -

Euclid preparation: I. the Euclid Wide Survey

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