Satellite

Launcher: SpaceX Falcon 9 from Cape Canaveral

Orbit: Sun-Earth Lagrange point 2 (L2)

Telescope

Type: Korsch off-axis three mirror anastigmat; Silicon Carbide telescope

Aperture: 1.20m diameter primary mirror, 9926cm² effective collection area

Focus: 24.5m focal length; paraxial F-number F/20.42

Dichroic element: reflected beam to VIS, transmitted beam to NISP instrument

Prime reference for mission design parameters (will be updated for/after launch): Racca+ 2016

Visible instrument, VIS

• detector array: 36 4x4k pixel CCD273-84, produced by Teledyne E2V; detectors read from each corner, 144 read channels
• 16-bit digitisation, 3.4 e-/ADU; <4.4 electrons internal noise in VIS detection chain
• pixel scale: 0.1 arcsec (slightly undersampling diffraction limit)
• effective angular resolution: 0.18 arcsec (through multiple exposures)
• field of view: 0.57 deg²
• single passband: I_E=530-920nm, defined by dichroic reflection and combined effect of mirror coatings
• shutter unit
• calibration source (VIS-CU), for flat-fields and other calibration purposes: using LEDs at 6 wavelenghts

Near Infrared Spectrometer and Photometer, NISP

• detector array: 16 2x2k H2RG detectors, produced by Teledyne
• pixel scale: 0.3 arcsec (undersampling the PSF)
• radius of 50%/80% encircled energy (note: these are requirements; actual value will differ and be known only after launch):
  • rEE50: <0.4 arcsec
  • rEE80: <0.7 arcsec
• spectral elements: in filter wheel (FWA) and grism wheel (GWA)
• photometry passbands (50% cut-on to 50% cut-off, from Euclid Consortium: Schirmer+ 2022, Tab. 3):
  • Y_E: 949.6nm-1212.3nm
  • J_E: 1167.6nm-1567.0nm
  • H_E: 1521.5nm-2021.4nm
• grism passbands (50% cut-on to 50% cut-off):
  • BG_E (from grism BGS000, orientation 0°): 926nm-1366nm, R~400
  • RG_E (from grisms RGS000/RGS180, orientations 0°, 180° [RGS270 is unused]): 1206nm-1892nm, R~480
• calibration unit (NI-CU), for flat-fields and other calibration purposes:
  • 5 LEDs from ~920 to ~2000 nm

Euclid will conduct two major surveys, the Euclid Wide Survey (EWS) and the Euclid Deep Survey (EDS), as well as repeatedly cover two fields to increase spectroscopic completeness and decrease confusion (CPC fields), and a number of legacy fields, the Euclid Auxilliary Fields (EAFs).

Prime reference for the EWS but also giving initial info on EDS, CPC, and EAFs: Euclid Consortium: Scaramella+ 2022.

Euclid Wide Survey

The EWS will cover 14,500 to 15,000 deg² over a background- and contaminant-optimised extra-galactic and extra-ecliptic part of the sky.

Median limiting sensitivities, AB zeropoint, for 5σ point-like source, over the EWS reference survey footprint (EC: Scaramella+ 2022, Tab. 7 and Figs. 19+21):

• VIS visible band: I_E=26.2
• NISP near infrared bands:
  • Y_E=24.3
  • J_E=24.5
  • H_E=24.4
• NISP slitless spectroscopy, Hα line flux limit: 2 × 10⁻¹⁶ erg⁻¹ cm⁻² s⁻¹ at 1600 nm
• Diffuse emission, surface brightness limits (1sigma over a 10×10 arcsec area):
  • I_E=29.8 mag arcsec⁻²
  • Y_E=28.2 mag arcsec⁻²
  • J_E=28.4 mag arcsec⁻²
  • H_E=28.4 mag arcsec⁻²

Euclid Deep Survey

The EDS will cover ~53 deg² split over three fields, with field-centers in Equatorial (celestial) coordinates (RA/Dec.):

• EDF-North (EDFN, 20 deg² x 40 visits): 17:58:55.9 +66:01:03.7
• EDF-South (EDFS, 23 deg² x 45 visits): 04:04:57.84 -48:25:22.8
• EDF-Fornax (EDFF, 10 deg² x 53+ visits): 03:31:43.6 -28:05:18.6

The reference for EDF locations, shapes, and details is the ESA Euclid Deep Field page.

Euclid CPC fields

The Euclid CPC fields will each subtend 20 deg² and will be repeatedly observed at different times to obtain grism spectroscopy at different orientation angles on the sky. Their field centers have been chosen to coincide with the EDF-North and EDF-South, so the CPC fields are not separate fields from the EDS fields.

Euclid Auxiliary Fields

The EAFs will be used to calibrate photometric redshifts and colour-gradients (EC: Scaramella+ 2022, Sec. 6.2). They are these six well-known fields, plus an extra field for photometric self-calibration of the survey. Depth refers to increase in SNR compared to the Wide Survey: