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EUCLID NEAR IR SPECTROGRAPH FOCAL PLANE

EUCLID NEAR IR SPECTROGRAPH FOCAL PLANE. People:. EUCLID MISSION. Cosmology Medium-class mission in the ESA’s ‘Cosmic Vision’ program High-precision survey mission: centered on Weak Lensing and BAO L2 Orbit 4-5 year mission Passively cooled Telescope: 1.2 m Korsh • Instruments:

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EUCLID NEAR IR SPECTROGRAPH FOCAL PLANE

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  1. EUCLID NEAR IR SPECTROGRAPHFOCAL PLANE People: ENIS Focal Plane

  2. EUCLID MISSION • Cosmology Medium-class mission in the ESA’s ‘Cosmic Vision’ program • High-precision survey mission: centered on Weak Lensing and BAO • L2 Orbit • 4-5 year mission • Passively cooled • Telescope: 1.2 m Korsh • Instruments: • Visible imaging channel: 0.5 deg2, 0.10 ’’/pixel, 0.23’’ PSF FWHM, broad band R+I+Z (0.55-0.92µ), CCD detectors, galaxy shapes • NIR photometry channel: 0.5 deg2, 0.3 ’’/pixel, 3bands Y,J,H (1.0-1.7µ), HgCdTe detectors, photometric Z • NIR Spectroscopic channel: 0.5 deg2, R=200-600, baseline: slitless (0.8-2.0µ), option: multi-object (0.9-1.7µ) Digital-Micro-Devices (DMD) based, redshifts ENIS Focal Plane

  3. EUCLID MISSION Euclid will survey the entire extra galactic sky (20 000 deg2) to simultaneously measure its two principal dark energy probes: • Weak lensing: • Diffraction limited galaxy shape measurements in one broad visible band (R+I+Z) up to 24.5 ABmag • Photometric Z measurements in 3 NIR bands (Y,J,H) up to 24 ABmag (H) • Baryonic Acoustic Oscillations: • Spectroscopic Z survey for 33% of all galaxies brighter than 22 ABmag (H) ENIS Focal Plane

  4. ENIS: Slitless Spectrograph Option Input Tel. Beam To FP Telescope beam is collected at an intermediate instrument position, hits the pick-off mirror (in grey), passes through a couple of corrector lenses (blue), then is directed to the collimating parabola by a flat folder. The same folder, after collimation, projects the beam to the removable disperser. Light is then refocused onto the NIR focal plane array by a four lenses f# 6.8 camera. ENIS Focal Plane

  5. ENIS: DMD Spectrograph Option Digital Micromirror Device at the f#3 intermediate focal plane Input Tel. Beam ENIS Focal Plane

  6. ENIS: Slitless and DMD Focal Planes ‘DMD’ mode field is split at the pick-off optics in four independent channels ‘slitless’ mode FPA ENIS Focal Plane

  7. ENIS FOCAL PLANE Focal planes will be constructed making use of the forthcoming generation of 2048x2048 H2RG detectors with MBE processed MeCdTe sensitive layer (2.5 µ cut-off) and SiC mechanical substrate. Readout electronics is based on the forthcoming 32 ch. SIDECAR ASIC mounted in CGA technology. ENIS Focal Plane

  8. ENIS SLITLESS FOCAL PLANE ‘slitless’ mode FP mechanics: H2RG mosaic is mounted and aligned on a SiC thermally controlled frame 228x148x61 mm TOT. MASS + 20% Cont. : 5700 Gr Readout ASICs can stay @ higher temperature ENIS Focal Plane

  9. ENIS DMD FOCAL PLANE ‘DMD’ mode FP mechanics: 1 from 4 same concept as for ‘slitless’ mode. 140x95x70 mm Readout ASICs directly mounted in the housing back-cover to save space TOT. MASS + 20% Cont. : 3800 Gr ENIS Focal Plane

  10. ENIS FOCAL PLANE Extrapolated solar activity for the Euclid launch date. Preliminary Montecarlo simulations have been done considering the average fluence in L2 for 0-300 Mev Protons. Present mechanical design is compatible with shielding requirements. ENIS Focal Plane

  11. ENIS FOCAL PLANE THERMAL Temperature requirements derived from background radiometry: ‘slitless’ backgrounds ‘DMD’ backgrounds ENIS Focal Plane

  12. ENIS FOCAL PLANE THERMAL 150 K 80 K 77 K 75 K 80 K ENIS Focal Plane

  13. ENIS FOCAL PLANE READOUT Achievement of RON requirements and CRs deglitching possibility require a readout strategy based on multiple-readouts: Sampling in continuous non-destructive readout (NDRO) mode illustrated for a single H2RG cell and results for a 15 e- single CDS device. ENIS Focal Plane

  14. ENIS FOCAL PLANE READOUT Expected CR rates are 5÷30 events/Sec/Cm2 I.E. 4÷25% of FP pixels @ 500 Sec exposure and with 5 pixels/CR Simulation with 5÷30 events/Sec/Cm2 About 15÷20 UTR Groups needed to correct ENIS Focal Plane

  15. ENIS FOCAL PLANE CONTROL ENIS Focal Plane

  16. ENIS FOCAL PLANE CONTROL Space Wire (SPW) communication architecture makes the FP electronics exactly compatible between the two configurations: slitless and DMD: 150 ºK 150-75 ºK 80-100 ºK 150-75 ºK 150 ºK ENIS FP REQUIRED POWER + 20% CONTINGENCY: 5100 mW ENIS Focal Plane

  17. ENIS FOCAL PLANE CONTROL • Two redundant processing systems: • DAPU, data processing (averaging, deglitching) • ICU, Controls & Data Handling (compression) ENIS Focal Plane

  18. ENIS FOCAL PLANE CONCLUSIONS • ENIS yellowbook already presented • IDD document presented (end of September) • EUCLID ESA scientific presentation in november • Preselection results beginning next year ENIS Focal Plane

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