Final published version
Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - Euclid preparation
T2 - I. The Euclid Wide Survey
AU - Euclid Collaboration
AU - Scaramella, R.
AU - Amiaux, J.
AU - Mellier, Y.
AU - Burigana, C.
AU - Carvalho, C. S.
AU - Cuillandre, J. -C.
AU - Silva, A. Da
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 - Venancio, L. M. Gaspar
AU - Gómez-Álvarez, P.
AU - Hoar, J.
AU - Alvarez, J. Lorenzo
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 - Meneghetti, M.
AU - Miller, L.
AU - Nakajima, R.
AU - Niemi, S. M.
AU - Pasian, F.
AU - Percival, W. J.
AU - Sauvage, M.
AU - Scodeggio, M.
AU - Wachter, S.
AU - Zacchei, A.
AU - Aghanim, N.
AU - Amara, A.
AU - Hook, I. M.
PY - 2022/6/30
Y1 - 2022/6/30
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 - space vehicles
KW - surveys
KW - methods: numerical
KW - dark energy
KW - dark matter
U2 - 10.1051/0004-6361/202141938
DO - 10.1051/0004-6361/202141938
M3 - Journal article
VL - 662
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 1432-0746
M1 - A112
ER -