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.

Time-of-flight positron emission tomography (TOF-PET) is the standard-of-care in cancer detection. TOF-PET scanners’ performance is dependent on the radiation detectors they use. Improving time and spatial detection features in such detectors will dramatically impact the diagnostic capacity of TOF-PET systems. The goal of this project is to build a gamma detector concept for TOF-PET able to improve the time resolution and spatial segmentation of state-of-the-art detectors by a factor of up to 7 and 10, respectively, without additional production costs. CHLOE-PET is a forward-looking gamma detector design for TOF-PET able to exploit the new photodetector technologies that are currently under development and will become available within the next 5-to-10 years. The novelty of the proposed design lies in using Cherenkov light as a prompt time source, using an innovative geometry optimized to maximize light collection, and employing photodetectors with small pixel pitch. This project is the first attempt to build a detector module scalable to a full-size system that can be used in a hospital setting. The CHLOE-PET detector will consist of bismuth germanate (BGO) crystals with 12 mm thickness and will combine the readout of scintillation and Cherenkov light. CHLOE-PET will provide an effective 3D segmentation of 2x2x2 mm3, an intrinsic photon time spread of 20 ps, and no intrinsic radiation background (unlike state-of-the-art TOF-PET detectors). Such improvements will allow increasing the signal-to-noise ratio of images by >2-fold, to be able to detect lesions of 2 mm size (>3 times the current performance), to build portable high-performance organ-dedicated TOF-PET systems, and to universalize the use of dynamic TOF-PET studies. The combination of these outcomes will provide significantly better diagnostic capabilities in a range of fields such as oncology, neurology, or cardiology, among others, and ultimately boost treatment efficacy and patient comfort.

Astrophysical and cosmological observations imply that only 5% of the energy of the Universe is made of conventional matter. The rest is composed by a new type of matter, the so-called dark matter, which has no (or extremely weak) interactions with the known particles, and a yet more puzzling repulsive form of energy accelerating the universe's expansion (dark energy). Advancing our knowledge on the nature of this dark universe is the focus of a global multidisciplinary effort in astroparticle physics. Indeed, solving these puzzles have been identified as a priority for the future of particle physics and cosmology by several scientific agencies worldwide. In this context, UNDARK’s main objective is to transform the Instituto de Astrofísica de Canarias (IAC) into a world-class institution in astroparticle physics. This will be accomplished by leveraging IAC's expertise in astronomy and astrophysics with the excellence and theoretical expertise provided by the world’s leading particle physics laboratory (CERN), and three renowned EU institutions in astroparticle physics. UNDARK's work plan includes an ambitious program of networking, scientific events, staff exchanges and scientific collaborations that will significantly enhance the IAC's research capacity and creativity, and will increase its reputation within the EU and global R&I systems. This will be complemented by an extensive outreach program developed in parallel which aims to boost the recognition of the IAC within the general public and public funding bodies. Finally, UNDARK also incorporates training activities focused on research management to increase the management capacity of the IAC and its involvement in HE funding programs. In summary, UNDARK has been designed with the goal of achieving excellence at the Widening coordinator in a priority area of fundamental physics research, thereby addressing one of the most significant challenges in contemporary physics.