Our understanding of cosmology and fundamental physics continues to be challenged by ever more precise experiments. The resulting “standard” model of cosmology describes the data well, but is unable to explain the origin of the main constituents of our Universe, namely dark matter and dark energy. More than an order of magnitude improvement in the quality and quantity of observational data is needed. This has motivated ESA to select Euclid as the second mission of its cosmic vision program, with a scheduled launch in 2020. It is designed to accurately measure the alignments of distant galaxies due to the differential deflection of light-rays by intervening structures, a phenomenon called gravitational lensing. Euclid will measure this signal by imaging 1.5 billion galaxies with a resolution similar to that of the Hubble Space Telescope. Although Euclid is designed to minimize observational systematics the observations are still compromised by two factors. Various instrumental effects need to be corrected for, and the tremendous improvement in precision has to be matched with comparable advances in the modelling of astrophysical effects that affect the signal. The objective of this proposal is to make significant progress on both fronts. To do so, we will (i) quantify the morphology of galaxies using archival HST observations; (ii) carry out a unique narrow-band photometric redshift survey to obtain state-of-the-art constraints on the intrinsic alignments of galaxies that arise due to tidal interactions, and would otherwise contaminate the cosmological signal; (iii) integrate these results into the end-to-end simulation pipeline; (iv) perform a spectroscopic redshift survey to calibrate the photometric redshift technique. The Euclid Consortium has identified these as critical issues, which need to be addressed before launch, in order to maximise the science return of this exciting mission, and enable the dark energy science objectives of Europe.

The goal of the RADIOBLOCKS project is to achieve a maximal boost for the European major world-leading research infrastructures in radio astronomy, which over the years have invested heavily in maintaining existing facilities as well as in substantial upgrade programmes, after identifying common challenges towards their mid- and long-term scientific visions. In this project, the institutes responsible of these facilities join forces, together with partners from industry and academia, in order to develop “common building blocks” for technological solutions beyond state-of-the-art, that will enable a broad range of new science and enhance European scientific competitiveness. They share the need to continuously improve their capabilities in order to enable new science: sensitivity, field of view, bandwidth, angular, time and frequency resolution, commensality and on-sky time, reaction time and RFI mitigation. Engagement with industry to co-develop advanced technologies will increase the partners’ technological levels and strengthen their market positions, creating a true European innovation system. This project carries out carefully targeted development work and addresses common aspects in the complete data chain, categorizing this in four phases: Novel detectors and components, digital receivers, transport and correlator, and data (post)processing. We will design and demonstrate common building blocks based on cutting-edge technologies, that will be enablers and extenders in the areas most critical to the RIs, and can and will be used for upgrades of several RIs. The building blocks will be new instrument components and advanced digital solutions based on newly available (HPC/AI optimized) hardware. This approach will enable a tremendous increase of the science delivery potential of Europe’s major radio astronomical observatories, for science cases that are high on their long-term agendas, aimed at the widest possible science community in Europe and beyond.

We propose a conceptual design study for a 12-metre wide-field spectroscopic survey telescope (WST) with simultaneous operation of a large field-of-view (3 sq. degree), high-multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 arcmin integral field spectrograph (IFS). In scientific capability these specifications place WST far ahead of existing and planned facilities. In only 5 years of operation, the MOS would target 250 million galaxies and 25 million stars at low spectral resolution plus 2 million stars at high resolution. Without need for pre-imaged targets, the IFS would deliver 4 billion spectra offering many serendipitous discoveries. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work in synergy with future ground and space-based facilities. We show how it can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; the origin of stars and planets; and time domain and multi-messenger astrophysics. WST’s uniquely rich dataset may yield unforeseen discoveries in many of these areas. The study will deliver telescope and instrument designs, cost estimates, an updated science white paper and survey plan, concept studies for data management, and a facility operation concept. The telescope and instruments will be designed as an integrated system and will mostly use existing technology, with the aim to minimise the carbon footprint and environmental impact. We will propose WST as the next ESO project after completion of the 39-metre ELT. Our consortium includes institutes from Australia, which has a strategic partnership with ESO and aims to apply shortly for full membership. Together with ESO and institutes in 9 European countries, our team has the necessary technical and scientific expertise, and brings 70 years of in-kind effort to the proposed study.