Euclid Technical Details
- Focal plane array: 6×6 CCDs (4k×4k pixels each) with 0.101 arcsec pixel platescale
- Field of view: 0.57 (deg)2
- Wavelength coverage: one wide visible band (550-900 nm)
- System point-spread function: 0.16 arcsec (FWHM) excluding pixelisation
- Focal plane array: 4×4 HgCdTe NIR detectors (2k×2k pixels each) with 0.3 arcsec per pixel and 2.3 µm cut-off wavelength.
- Imaging bands: Y (0.95 to 1.192 µm), J (1.192 to 1.544 µm), H (1.544 to 2 µm)
- Grisms: 1 blue grism (0.92 to 1.3 µm); 3 identical red grisms (1.25 to 1.85 µm) at position angles 0 deg, 90 deg, 180 deg.
- Spectral resolution: constant Δλ at λ/Δλ ˃ 380 for an object of 0.5 arcsec diameter
- FoV: 0.53 (deg)2
- 15000 (deg)2 of the extragalactic sky
- VIS imaging of galaxy shapes down to AB magnitude 24.5 (10 σ, extended source)
- NISP photometry in the Y, J and H near-infrared bands (0.92 – 2.0 µm) reaching AB magnitude 24 (5σ, point source) corresponding to a photometric redshift accuracy of σ(z)/(1+z)<0.05
- Parallel to the VIS exposures, NISP will measure redshifts with σ(z)/(1+z)<0.001 of at least 1700 galaxies/(deg)2 with a completeness higher than 45% at a detection limit of 2×10-16 erg/s/cm2 (3.5σ) for a typical source of 0.5 arcsec in the wavelength range 1.25-1.85 µm.
> 40 (deg)2 of deep fields and calibration observations regularly interleaved within the main survey schedule.
Mission Characteristics (table on Euclid Consortium website)
Mission-level performance verification approach for the Euclid space mission, Vavrek et al. (2016),Proc. of SPIE, Vol. 9911, 991105
VIS: the visible imager for Euclid, Cropper et al. (2016), Proc. of SPIE, Vol. 9904, 99040Q
Euclid Near Infrared Spectrometer and Photometer instrument concept and first test results obtained for different breadboards models at the end of phase C, Maciaszek et al. (2016), Proc. of SPIE Vol. 9904 99040T
The Euclid mission design, Racca et al. (2016), Proc. of SPIE, Vol. 9904, 99040O