VIS: the visible imager for Euclid

Abstract

Euclid-VIS is the large format visible imager for the ESA Euclid space mission in their Cosmic Vision program, scheduled for launch in 2020. Together with the near infrared imaging within the NISP instrument, it forms the basis of the weak lensing measurements of Euclid. VIS will image in a single r+i+z band from 550-900 nm over a field of view of ~0.5 deg2. By combining 4 exposures with a total of 2260 sec, VIS will reach to deeper than mAB=24.5 (10sigma) for sources with extent ~0.3 arcsec. The image sampling is 0.1 arcsec. VIS will provide deep imaging with a tightly controlled and stable point spread function (PSF) over a wide survey area of 15000 deg2 to measure the cosmic shear from nearly 1.5 billion galaxies to high levels of accuracy, from which the cosmological parameters will be measured. In addition, VIS will also provide a legacy dataset with an unprecedented combination of spatial resolution, depth and area covering most of the extra-Galactic sky. Here we will present the results of the study carried out by the Euclid Consortium during the period up to the Critical Design Review.

arXiv comment16 pages, 15 figures, 1 table

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• On the shear estimation bias induced by the spatial variation of colour across galaxy profiles
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Cited by in corpus (14)

• The Euclid mission design
• Reconstructing the Lensing Mass in the Universe from Photometric Catalogue Data
• Scientific Synergy Between LSST and Euclid
• VIS: the visible imager for Euclid
• Euclid Mission: building of a Reference Survey
• Detecting solar system objects with convolutional neural networks
• The high energy universe at ultra-high resolution: the power and promise of X-ray interferometry
• Auto-identification of unphysical source reconstructions in strong gravitational lens modelling
• Rethinking data-driven point spread function modeling with a differentiable optical model
• Precision cosmology with time delay lenses: high resolution imaging requirements
• Galaxy shape measurement synergies between LSST and Euclid
• Using Strong Lensing to Detect Subhalos with Steep Inner Density Profiles
• Impact of PSF misestimation and galaxy population bias on precision shear measurement using a CNN
• The Read-Out Shutter Unit of the Euclid VIS Instrument