ERC FUNDED PROJECTS

Most celestial bodies, from planets, to stars, to black holes; gain mass during their lives by means of an accretion disc. Understanding the physical processes that determine the rate at which matter accretes and energy is radiated in these discs is vital for unraveling the formation, evolution, and fate of almost every type of object in the Universe. Despite the fact that magnetic fields have been known to be crucial in accretion discs since the early 90’s, the majority of astrophysical questions that depend on the details of how disc accretion proceeds are still being addressed using the “standard” accretion disc model (developed in the early 70’s), where magnetic fields do not play an explicit role. This has prevented us from fully exploring the astrophysical consequences and observational signatures of realistic accretion disc models, leading to a profound disconnect between observations (usually interpreted with the standard paradigm) and modern accretion disc theory and numerical simulations (where magnetic turbulence is crucial). The goal of this proposal is to use several complementary approaches in order to finally move beyond the standard paradigm. This program has two main objectives: 1) Develop the theoretical framework to incorporate magnetic fields, and the ensuing turbulence, into self-consistent accretion disc models, and investigate their observational implications. 2) Investigate transport and radiative processes in collision-less disc regions, where non-thermal radiation originates, by employing a kinetic particle description of the plasma. In order to achieve these goals, we will use, and build upon, state-of-the-art magnetohydrodynamic and particle-in-cell codes in conjunction with theoretical modeling. This framework will make it possible to address fundamental questions on stellar and planet formation, binary systems with a compact object, and supermassive black hole feedback in a way that has no counterpart within the standard paradigm.

1 793 697 €

Start date: 2013-02-01, End date: 2018-01-31

Faithful repair of double stranded DNA breaks (DSBs) is essential, as they are at the origin of genome instability, chromosomal translocations and cancer. Cells repair DSBs through different pathways, which can be faithful or mutagenic, and the balance between them at a given locus must be tightly regulated to preserve genome integrity. Although, much is known about DSB repair factors, how the choice between pathways is controlled within the nuclear environment is not understood. We have shown that nuclear architecture and non-random genome organization determine the frequency of chromosomal translocations and that pathway choice is dictated by the spatial organization of DNA in the nucleus. Nevertheless, what determines which pathway is activated in response to DSBs at specific genomic locations is not understood. Furthermore, the impact of 3D-genome folding on the kinetics and efficiency of DSB repair is completely unknown. Here we aim to understand how nuclear compartmentalization, chromatin structure and genome organization impact on the efficiency of detection, signaling and repair of DSBs. We will unravel what determines the DNA repair specificity within distinct nuclear compartments using protein tethering, promiscuous biotinylation and quantitative proteomics. We will determine how DNA repair is orchestrated at different heterochromatin structures using a CRISPR/Cas9-based system that allows, for the first time robust induction of DSBs at specific heterochromatin compartments. Finally, we will investigate the role of 3D-genome folding in the kinetics of DNA repair and pathway choice using single nucleotide resolution DSB-mapping coupled to 3D-topological maps. This proposal has significant implications for understanding the mechanisms controlling DNA repair within the nuclear environment and will reveal the regions of the genome that are susceptible to genomic instability and help us understand why certain mutations and translocations are recurrent in cancer

1 999 750 €

Start date: 2017-03-01, End date: 2022-02-28

At the end of their life, stars spread their inner material into the diffuse interstellar medium. This diffuse medium gets locally denser and form dark clouds (also called dense or molecular clouds) whose innermost part is shielded from the external UV field by the dust, allowing for molecules to grow and get more complex. Gravitational collapse occurs inside these dense clouds, forming protostars and their surrounding disks, and eventually planetary systems like (or unlike) our solar system. The formation and evolution of molecules, minerals, ices and organics from the diffuse medium to planetary bodies, their alteration or preservation throughout this cosmic chemical history set the initial conditions for building planets, atmospheres and possibly the first bricks of life. The current view of interstellar chemistry is based on fragmental works on key steps of the sequence that are observed. The objective of this proposal is to follow the fractionation of the elements between the gas-phase and the interstellar grains, from the most diffuse medium to protoplanetary disks, in order to constrain the chemical composition of the material in which planets are formed. The potential outcome of this project is to get a consistent and more accurate description of the chemical evolution of interstellar matter. To achieve this objective, I will improve our chemical model by adding new processes on grain surfaces relevant under the diffuse medium conditions. This upgraded gas-grain model will be coupled to 3D dynamical models of the formation of dense clouds from diffuse medium and of protoplanetary disks from dense clouds. The computed chemical composition will also be used with 3D radiative transfer codes to study the chemical tracers of the physics of protoplanetary disk formation. The robustness of the model predictions will be studied with sensitivity analyses. Finally, model results will be confronted to observations to address some of the current challenges.

1 166 231 €

Start date: 2013-09-01, End date: 2018-08-31

This project investigates the two-way relationship between spatio-temporal genome organization and coordinated gene regulation, through an approach at the interface between physics, computer science and biology. In the nucleus, preferred positions are observed from chromosomes to single genes, in relation to normal and pathological cellular states. Evidence indicates a complex spatio-temporal coupling between co-regulated genes: e.g. certain genes cluster spatially when responding to similar factors and transcriptional noise patterns suggest domain-wide mechanisms. Yet, no individual experiment allows probing transcriptional coordination in 4 dimensions (FISH, live locus tracking, Hi-C...). Interpreting such data also critically requires theory (stochastic processes, statistical physics…). A lack of appropriate experimental/analytical approaches is impairing our understanding of the 4D genome. Our proposal combines cutting-edge single-molecule imaging, signal-theory data analysis and physical modeling to study how genes coordinate in space and time in a single nucleus. Our objectives are to understand (a) competition/recycling of shared resources between genes within subnuclear compartments, (b) how enhancers communicate with genes domain-wide, and (c) the role of local conformational dynamics and supercoiling in gene co-regulation. Our organizing hypothesis is that, by acting on their microenvironment, genes shape their co-expression with other genes. Building upon my expertise, we will use dual-color MS2/PP7 RNA labeling to visualize for the first time transcription and motion of pairs of hormone-responsive genes in real time. With our innovative signal analysis tools, we will extract spatio-temporal signatures of underlying processes, which we will investigate with stochastic modeling and validate through experimental perturbations. We expect to uncover how the functional organization of the linear genome relates to its physical properties and dynamics in 4D.

1 499 750 €

Start date: 2018-04-01, End date: 2023-03-31

"High-energy observations of our Galaxy offer a good, albeit not complete, picture of the X-ray source populations, in particular the accreting binary sources. Recent ability to study accreting binaries in nearby galaxies has shown that we would be short-sighted if we restricted ourselves to our Galaxy or to a few nearby ones. I propose an ambitious project that involves a comprehensive study of all the galaxies within 10 Mpc for which we can study in detail their X-ray sources and stellar populations. The study will combine data from a unique suite of observatories (Chandra, XMM-Newton, HST, Spitzer) with state-of-the-art theoretical modelling of binary systems. I propose a novel approach that links the accreting binary populations to their parent stellar populations and surpasses any current studies of X-ray binary populations, both in scale and in scope, by: (a) combining methods and results from several different areas of astrophysics (compact objects, binary systems, stellar populations, galaxy evolution); (b) using data from almost the whole electromagnetic spectrum (infrared to X-ray bands); (c) identifying and studying the different sub-populations of accreting binaries; and (d) performing direct comparison between observations and theoretical predictions, over a broad parameter space. The project: (a) will answer the long-standing question of the formation efficiency of accreting binaries in different environments; and (b) will constrain their evolutionary paths. As by-products the project will provide eagerly awaited input to the fields of gravitational-wave sources, γ-ray bursts, and X-ray emitting galaxies at cosmological distances and it will produce a heritage multi-wavelength dataset and library of models for future studies of galaxies and accreting binaries."

1 242 000 €

Start date: 2014-04-01, End date: 2019-03-31

"Eukaryotic nuclei are organised into functional compartments, – local microenvironments that are enriched in certain molecules or biochemical activities and therefore specify localised functional outputs. Our study seeks to unveil fundamental principles of co-regulation of genes in a chromo¬somal compartment and the preconditions for homeostasis of such a compartment in the dynamic nuclear environment. The dosage-compensated X chromosome of male Drosophila flies satisfies the criteria for a functional com¬partment. It is rendered structurally distinct from all other chromosomes by association of a regulatory ribonucleoprotein ‘Dosage Compensation Complex’ (DCC), enrichment of histone modifications and global decondensation. As a result, most genes on the X chromosome are co-ordinately activated. Autosomal genes inserted into the X acquire X-chromosomal features and are subject to the X-specific regulation. We seek to uncover the molecular principles that initiate, establish and maintain the dosage-compensated chromosome. We will follow the kinetics of DCC assembly and the timing of association with different types of chromosomal targets in nuclei with high spatial resolution afforded by sub-wavelength microscopy and deep sequencing of DNA binding sites. We will characterise DCC sub-complexes with respect to their roles as kinetic assembly intermediates or as representations of local, functional heterogeneity. We will evaluate the roles of a DCC- novel ubiquitin ligase activity for homeostasis. Crucial to the recruitment of the DCC and its distribution to target genes are non-coding roX RNAs that are transcribed from the X. We will determine the secondary structure ‘signatures’ of roX RNAs in vitro and determine the binding sites of the protein subunits in vivo. By biochemical and cellular reconstitution will test the hypothesis that roX-encoded RNA aptamers orchestrate the assembly of the DCC and contribute to the exquisite targeting of the complex."

2 482 770 €

Start date: 2012-02-01, End date: 2017-01-31

The discoveries that the expansion of the universe is accelerating due to an unknown “dark energy” and that most of the matter is invisible, highlight our lack of understanding of the major constituents of the universe. These surprising findings set the stage for research in cosmology at the start of the 21st century. The objective of this proposal is to advance observational constraints to a level where we can distinguish between physical mechanisms that aim to explain the properties of dark energy and the observed distribution of dark matter throughout the universe. We use a relatively new technique called weak gravitational lensing: the accurate measurement of correlations in the orientations of distant galaxies enables us to map the dark matter distribution directly and to extract the cosmological information that is encoded by the large-scale structure. To study the dark universe we will analyse data from a new state-of-the-art imaging survey: the Kilo- Degree Survey (KiDS) will cover 1500 square degrees in 9 filters. The combination of its large survey area and the availability of exquisite photometric redshifts for the sources makes KiDS the first project that can place interesting constraints on the dark energy equation-of-state using lensing data alone. Combined with complementary results from Planck, our measurements will provide one of the best views of the dark side of the universe before much larger space-based projects commence. To reach the desired accuracy we need to carefully measure the shapes of distant background galaxies. We also need to account for any intrinsic alignments that arise due to tidal interactions, rather than through lensing. Reducing these observational and physical biases to negligible levels is a necessarystep to ensure the success of KiDS and an important part of our preparation for more challenging projects such as the European-led space mission Euclid.

1 316 880 €

Start date: 2012-01-01, End date: 2016-12-31

"Ageing is the gradual and irreversible breakdown of living systems associated with the advancement of time, which leads to an increase in vulnerability and eventual mortality. Despite recent advances in ageing research, the intrinsic complexity of the ageing process has prevented a full understanding of this process, therefore, ageing remains a grand challenge in contemporary biology. In AGELESS, we will tackle this challenge by uncovering the molecular mechanisms of halted ageing in a unique model system, the bats. Bats are the longest-lived mammals relative to their body size, and defy the ‘rate-of-living’ theories as they use twice as much the energy as other species of considerable size, but live far longer. This suggests that bats have some underlying mechanisms that may explain their exceptional longevity. In AGELESS, we will identify the molecular mechanisms that enable mammals to achieve extraordinary longevity, using state-of-the-art comparative genomic methodologies focused on bats. We will identify, using population transcriptomics and telomere/mtDNA genomics, the molecular changes that occur in an ageing wild population of bats to uncover how bats ‘age’ so slowly compared with other mammals. In silico whole genome analyses, field based ageing transcriptomic data, mtDNA and telomeric studies will be integrated and analysed using a networks approach, to ascertain how these systems interact to halt ageing. For the first time, we will be able to utilize the diversity seen within nature to identify key molecular targets and regions that regulate and control ageing in mammals. AGELESS will provide a deeper understanding of the causal mechanisms of ageing, potentially uncovering the crucial molecular pathways that can be modified to halt, alleviate and perhaps even reverse this process in man."

1 499 768 €

Start date: 2013-01-01, End date: 2017-12-31

The goals are 1. To develop a scale assessing the diversity of active ageing with four dimensions that are ability (what people can do), activity (what people do do), ambition (what are the valued activities that people want to do), and autonomy (how satisfied people are with the opportunity to do valued activities); 2. To examine health and physical and psychological functioning as the determinants and social and build environment, resilience and personal skills as modifiers of active ageing; 3. To develop a multicomponent sustainable intervention aiming to promote active ageing (methods: counselling, information technology, help from volunteers); 4. To test the feasibility and effectiveness on the intervention; and 5. To study cohort effects on the phenotypes on the pathway to active ageing. “If You Can Measure It, You Can Change It.” Active ageing assessment needs conceptual progress, which I propose to do. A quantifiable scale will be developed that captures the diversity of active ageing stemming from the WHO definition of active ageing as the process of optimizing opportunities for health and participation in the society for all people in line with their needs, goals and capacities as they age. I will collect cross-sectional data (N=1000, ages 75, 80 and 85 years) and model the pathway to active ageing with state-of-the art statistical methods. By doing this I will create novel knowledge on preconditions for active ageing. The collected cohort data will be compared to a pre-existing cohort data that was collected 25 years ago to obtain knowledge about changes over time in functioning of older people. A randomized controlled trial (N=200) will be conducted to assess the effectiveness of the envisioned intervention promoting active ageing through participation. The project will regenerate ageing research by launching a novel scale, by training young scientists, by creating new concepts and theory development and by producing evidence for active ageing promotion

2 044 364 €

Start date: 2016-09-01, End date: 2021-08-31

"In our largely unchanging radio Universe, a highly dynamic component was recently discovered: flashes of bright radio emission that last only milliseconds but appear all over the sky. Some of these radio bursts can be traced to intermittently pulsating neutron stars. Other bursts however, apparently originate far outside our Galaxy. Due to great observational challenges, the evolution of the neutron stars is not understood, while more importantly, the nature of the extragalactic bursts remains an outright mystery. My overall aim is to understand the physics that drives both kinds of brief and luminous bursts. My primary goal is to identify the highly compact astrophysical explosions powering the extragalactic bursts. My previous surveys are the state of the art in fast-transient detection; I will now increase by a factor of 10 this exploration volume. In real-time I will provide arcsec positions, 10,000-fold more accurate than currently possible, to localize such extragalactic bursts for the first time and understand their origin. My secondary goal is to unravel the unexplained evolution of intermittently pulsating neutron stars (building on e.g., my recent papers in Science, 2013), by doubling their number and modeling their population. To achieve these goals, I will carry out a highly innovative survey: the Apertif-LOFAR Exploration of the Radio Transient Sky. ALERT is over an order of magnitude more sensitive than all current state-of-the art fast-transient surveys. Through its novel, extremely wide field-of-view, Westerbork/Apertif will detect many tens of extragalactic bursts. Through real-time triggers to LOFAR I will next provide the precise localisation that is essential for radio, optical and high-energy follow-up to, for the first time, shed light on the physics and objects driving these bursts – evaporating primordial black holes; explosions in host galaxies; or, the unknown?"

1 999 823 €

Start date: 2014-12-01, End date: 2019-11-30

A major challenge in contemporary traffic and transportation theory is having a comprehensive understanding of pedestrians and cyclists behaviour. This is notoriously hard to observe, since sensors providing abundant and detailed information about key variables characterising this behaviour have not been available until very recently. The behaviour is also far more complex than that of the much better understood fast mode. This is due to the many degrees of freedom in decision-making, the interactions among slow traffic participants that are more involved and far less guided by traffic rules and regulations than those between car-drivers, and the many fascinating but complex phenomena in slow traffic flows (self-organised patterns, turbulence, spontaneous phase transitions, herding, etc.) that are very hard to predict accurately. With slow traffic modes gaining ground in terms of mode share in many cities, lack of empirical insights, behavioural theories, predictively valid analytical and simulation models, and tools to support planning, design, management and control is posing a major societal problem as well: examples of major accidents due to bad planning, organisation and management of events are manifold, as are locations where safety of slow modes is a serious issue due to interactions with fast modes. This programme is geared towards establishing a comprehensive theory of slow mode traffic behaviour, considering the different behavioural levels relevant for understanding, reproducing and predicting slow mode traffic flows in cities. The levels deal with walking and cycling operations, activity scheduling and travel behaviour, and knowledge representation and learning. Major scientific breakthroughs are expected at each of these levels, in terms of theory and modelling, by using innovative (big) data collection and experimentation, analysis and fusion techniques, including social media data analytics, using augmented reality, and remote and crowd sensing.

2 458 700 €

Start date: 2015-11-01, End date: 2020-10-31

"During the last decade, a strikingly successful cosmological concordance model has been established. With only six free parameters, nearly all observables, comprising millions of data points, may be fitted with outstanding precision. However, in this beautiful picture a few ""blemishes"" have turned up, apparently not consistent with the standard model: While the model predicts that the universe is isotropic (i.e., looks the same in all directions) and homogeneous (i.e., the statistical properties are the same everywhere), subtle hints of the contrary are now seen. For instance, peculiar preferred directions and correlations are observed in the cosmic microwave background; some studies considering nearby galaxies suggest the existence of anomalous large-scale cosmic flows; a study of distant quasars hints towards unexpected large-scale correlations. All of these reports are individually highly intriguing, and together they hint toward a more complicated and interesting universe than previously imagined -- but none of the reports can be considered decisive. One major obstacle in many cases has been the relatively poor data quality. This is currently about to change, as the next generation of new and far more powerful experiments are coming online. Of special interest to me are Planck, an ESA-funded CMB satellite currently taking data; QUIET, a ground-based CMB polarization experiment located in Chile; and various large-scale structure (LSS) data sets, such as the SDSS and 2dF surveys, and in the future Euclid, a proposed galaxy survey satellite also funded by ESA. By combining the world s best data from both CMB and LSS measurements, I will in the proposed project attempt to settle this question: Is our universe really anisotropic? Or are these recent claims only the results of systematic errors or statistical flukes? If the claims turn out to hold against this tide of new and high-quality data, then cosmology as a whole may need to be re-written."

1 500 000 €

Start date: 2011-01-01, End date: 2015-12-31

Anopheles gambiae mosquitoes are the major vectors of malaria, a disease with devastating consequences for human health. Novel methods for controlling the natural vector populations are urgently needed, given the evolution of insecticide resistance in mosquitoes and the lack of novel insecticidals. Understanding the processes at the bases of mosquito biology may help to roll back malaria. In this proposal, we will target mosquito reproduction, a major determinant of the An. gambiae vectorial capacity. This will be achieved at two levels: (i) fundamental research, to provide a deeper knowledge of the processes regulating reproduction in this species, and (ii) applied research, to identify novel targets and to develop innovative approaches for the control of natural populations. We will focus our analysis on three major players of mosquito reproduction: male accessory glands (MAGs), sperm, and spermatheca, in both laboratory and field settings. We will then translate this information into the identification of inhibitors of mosquito fertility. The experimental activities will be divided across three objectives. In Objective 1, we will unravel the role of the MAGs in shaping mosquito fertility and behaviour, by performing a combination of transcriptional and functional studies that will reveal the multifaceted activities of these tissues. In Objective 2 we will instead focus on the identification of the male and female factors responsible for sperm viability and function. Results obtained in both objectives will be validated in field mosquitoes. In Objective 3, we will perform screens aimed at the identification of inhibitors of mosquito reproductive success. This study will reveal as yet unknown molecular mechanisms underlying reproductive success in mosquitoes, considerably increasing our knowledge beyond the state-of-the-art and critically contributing with innovative tools and ideas to the fight against malaria.

1 500 000 €

Start date: 2011-01-01, End date: 2015-12-31

Anxiety, a state of apprehension or fear, may provoke cognitive or behavioural disorders and eventually lead to serious medical illnesses. The high prevalence of anxiety disorders in our society sharply contrasts with the lack of clear factual knowledge about the corresponding brain mechanisms at the origin of this profound change in the appraisal of the environment. Little is known about how the psychopathological state of anxiety ultimately turns to a medical condition. The core of this proposal is to gain insight in the neural underpinnings of anxiety and disorders related to anxiety using modern human brain-imaging such as scalp EEG and fMRI. I propose to enlighten how anxiety transforms and shapes human cognition and what the neural correlates and time-course of this modulatory effect are. The primary innovation of this project is the systematic use scalp EEG and fMRI in human participants to better understand the neural mechanisms by which anxiety profoundly influences specific cognitive functions, in particular selective attention and decision-making. The goal of this proposal is to precisely determine the exact timing (using scalp EEG), location, size and extent (using fMRI) of anxiety-related modulations on selective attention and decision-making in the human brain. Here I propose to focus on these two specific processes, because they are likely to reveal selective effects of anxiety on human cognition and can thus serve as powerful models to better figure out how anxiety operates in the human brain. Another important aspect of this project is the fact I envision to help bridge the gap in Health Psychology between fundamental research and clinical practice by proposing alternative revalidation strategies for human adult subjects affected by anxiety-related disorders, which could directly exploit the neuro-scientific discoveries generated in this scientific project.

812 986 €

Start date: 2008-11-01, End date: 2013-10-31

Globular clusters (GCs) are enigmatic objects that hide a wealth of information. They are the living fossils of the history of their native galaxies and the record keepers of the violent events that made them change their domicile. This proposal aims to mine GCs as living fossils of galaxy evolution to address fundamental questions in astrophysics: (1) Do satellite galaxies merge as predicted by the hierarchical build-up of galaxies? (2) Which are the seeds of supermassive black holes in the centres of galaxies? (3) How did star formation originate in the earliest phases of galaxy formation? To answer these questions, novel population-dependent dynamical modelling techniques are required, whose development the PI has led over the past years. This uniquely positions him to take full advantage of the emerging wealth of chemical and kinematical data on GCs. Following the tidal disruption of satellite galaxies, their dense GCs, and maybe even their nuclei, are left as the most visible remnants in the main galaxy. The hierarchical build-up of their new host galaxy can thus be unearthed by recovering the GCs’ orbits. However, currently it is unclear which of the GCs are accretion survivors. Actually, the existence of a central intermediate mass black hole (IMBH) or of multiple stellar populations in GCs might tell which ones are accreted. At the same time, detection of IMBHs is important as they are predicted seeds for supermassive black holes in galaxies; while the multiple stellar populations in GCs are vital witnesses to the extreme modes of star formation in the early Universe. However, for every putative dynamical IMBH detection so far there is a corresponding non-detection; also the origin of multiple stellar populations in GCs still lacks any uncontrived explanation. The synergy of novel techniques and exquisite data proposed here promises a breakthrough in this emerging field of dynamical archeology with GCs as living fossils of the past of galaxies.

1 999 250 €

Start date: 2017-09-01, End date: 2022-08-31

The project ARTHUS aims at determining the physical origin of Dark Energy: in addition to the energy sources of the standard model of cosmology, effective terms arise through spatially averaging inhomogeneous cosmological models in General Relativity. It has been demonstrated that these additional terms can play the role of Dark Energy on large scales (but they can also mimic Dark Matter on scales of mass accumulations). The underlying rationale is that fluctuations in the Universe generically couple to spatially averaged intrinsic properties of space, such as its averaged scalar curvature, thus changing the global evolution of the effective (spatially averaged) cosmological model. At present, we understand these so- called backreaction effects only qualitatively. The project ARTHUS is directed towards a conclusive quantitative evaluation of these effects by developing generic and non-perturbative relativistic models of structure formation, by statistically measuring the key-variables of the models in observations and in simulation data, and by reinterpreting observational results in light of the new models. It is to be emphasized that there is no doubt about the existence of backreaction effects; the question is whether they are even capable of getting rid of the dark sources (as some models discussed in the literature suggest), or whether their impact is substantially smaller. The project thus addresses an essential issue of current cosmological research: to find pertinent answers concerning the quantitative impact of inhomogeneity effects, a necessary, worldwide recognized step toward high-precision cosmology. If the project objectives are attained, the results will have a far-reaching impact on theoretical and observational cosmology, on the interpretation of astronomical experiments such as Planck and Euclid, as well as on a wide spectrum of particle physics theories and experiments.

2 091 000 €

Start date: 2017-09-01, End date: 2022-08-31

Since 2012, over 4 million people have fled Syria in ‘the most dramatic humanitarian crisis that we have ever faced’ (UNHCR). By November 2015 there were 1,078,338 refugees from Syria in Lebanon, 630,776 in Jordan and 2,181,293 in Turkey. Humanitarian agencies and donor states from both the global North and the global South have funded and implemented aid programmes, and yet commentators have argued that civil society groups from the global South are the most significant actors supporting refugees in Lebanon, Jordan and Turkey. Whilst they are highly significant responses, however, major gaps in knowledge remain regarding the motivations, nature and implications of Southern-led responses to conflict-induced displacement. This project draws on multi-sited ethnographic and participatory research with refugees from Syria and their aid providers in Lebanon, Jordan and Turkey to critically examine why, how and with what effect actors from the South have responded to the displacement of refugees from Syria. The main research aims are: 1. identifying diverse models of Southern-led responses to conflict-induced displacement, 2. examining the (un)official motivations, nature and implications of Southern-led responses, 3. examining refugees’ experiences and perceptions of Southern-led responses, 4. exploring diverse Southern and Northern actors’ perceptions of Southern-led responses, 5. tracing the implications of Southern-led initiatives for humanitarian theory and practice. Based on a critical theoretical framework inspired by post-colonial and feminist approaches, the project contributes to theories of humanitarianism and debates regarding donor-recipient relations and refugees’ agency in displacement situations. It will also inform the development of policies to most appropriately address refugees’ needs and rights. This highly topical and innovative project thus has far-reaching implications for refugees and local communities, academics, policy-makers and practitioners.

1 498 069 €

Start date: 2017-07-01, End date: 2022-06-30

The Milky Way is a complex system, with dynamical and chemical substructures, where several competing processes such as mergers, internal secular evolution, gas accretion and gas flows take place. To study in detail how such a giant spiral galaxy was formed and evolved, we need to reconstruct the sequence of its main formation events with high (~10%) temporal resolution. Asterochronometry will determine accurate, precise ages for tens of thousands of stars in the Galaxy. We will take an approach distinguished by a number of key aspects including, developing novel star-dating methods that fully utilise the potential of individual pulsation modes, coupled with a careful appraisal of systematic uncertainties on age deriving from our limited understanding of stellar physics. We will then capitalise on opportunities provided by the timely availability of astrometric, spectroscopic, and asteroseismic data to build and data-mine chrono-chemo-dynamical maps of regions of the Milky Way probed by the space missions CoRoT, Kepler, K2, and TESS. We will quantify, by comparison with predictions of chemodynamical models, the relative importance of various processes which play a role in shaping the Galaxy, for example mergers and dynamical processes. We will use chrono-chemical tagging to look for evidence of aggregates, and precise and accurate ages to reconstruct the early star formation history of the Milky Way’s main constituents. The Asterochronometry project will also provide stringent observational tests of stellar structure and answer some of the long-standing open questions in stellar modelling (e.g. efficiency of transport processes, mass loss on the giant branch, the occurrence of products of coalescence / mass exchange). These tests will improve our ability to determine stellar ages and chemical yields, with wide impact e.g. on the characterisation and ensemble studies of exoplanets, on evolutionary population synthesis, integrated colours and thus ages of galaxies.

1 958 863 €

Start date: 2018-04-01, End date: 2023-03-31

ASTROFLOW aims to make ground-breaking progress in our physical understanding of exoplanetary mass loss, by quantifying the influence of stellar outflows on atmospheric escape of close-in exoplanets. Escape plays a key role in planetary evolution, population, and potential to develop life. Stellar irradiation and outflows affect planetary mass loss: irradiation heats planetary atmospheres, which inflate and more likely escape; outflows cause pressure confinement around otherwise freely escaping atmospheres. This external pressure can increase, reduce or even suppress escape rates; its effects on exoplanetary mass loss remain largely unexplored due to the complexity of such interactions. I will fill this knowledge gap by developing a novel modelling framework of atmospheric escape that will, for the first time, consider the effects of realistic stellar outflows on exoplanetary mass loss. My expertise in stellar wind theory and 3D magnetohydrodynamic simulations is crucial for producing the next-generation models of planetary escape. My framework will consist of state-of-the-art, time-dependent, 3D simulations of stellar outflows (Method 1), which will be coupled to novel 3D simulations of atmospheric escape (Method 2). My models will account for the major underlying physical processes of mass loss. With this, I will determine the response of planetary mass loss to realistic stellar particle, magnetic and radiation environments and will characterise the physical conditions of the escaping material. I will compute how its extinction varies during transit and compare synthetic line profiles to atmospheric escape observations from, eg, Hubble and our NASA cubesat CUTE. Strong synergy with upcoming observations (JWST, TESS, SPIRou, CARMENES) also exists. Determining the lifetime of planetary atmospheres is essential to understanding populations of exoplanets. ASTROFLOW’s work will be the foundation for future research of how exoplanets evolve under mass-loss processes.

1 999 956 €

Start date: 2019-09-01, End date: 2024-08-31

‘Consistency’ is regularly cited as a desirable attribute of border control, but it has received little critical social scientific attention. This inter-disciplinary project, at the inter-face between critical human geography, border studies and law, will scrutinise the consistency of European asylum adjudication in order to develop richer theoretical understanding of this lynchpin concept. It will move beyond the administrative legal concepts of substantive and procedural consistency by advancing a three-fold conceptualisation of consistency – as everyday practice, discursive deployment of facts and disciplinary technique. In order to generate productive intellectual tension it will also employ an explicitly antagonistic conceptualisation of the relationship between geography and law that views law as seeking to constrain and systematise lived space. The project will employ an innovative combination of methodologies that will produce unique and rich data sets including quantitative analysis, multi-sited legal ethnography, discourse analysis and interviews, and the findings are likely to be of interest both to academic communities like geographers, legal and border scholars and to policy makers and activists working in border control settings. In 2013 the Common European Asylum System (CEAS) was launched to standardise the procedures of asylum determination. But as yet no sustained multi-methodological assessment of the claims of consistency inherent to the CEAS has been carried out. This project offers not only the opportunity to assess progress towards harmonisation of asylum determination processes in Europe, but will also provide a new conceptual framework with which to approach the dilemmas and risks of inconsistency in an area of law fraught with political controversy and uncertainty around the world. Most fundamentally, the project promises to debunk the myths surrounding the possibility of fair and consistent border controls in Europe and elsewhere.

1 252 067 €

Start date: 2016-09-01, End date: 2021-08-31

Throughout history, what has been causing tremendous suffering is groups of people fighting each other. While behavioral science research has advanced our understanding of such intergroup conflict, it has exclusively focused on micro-level processes within and between groups at conflict. Disciplines that employ a more historical perspective like climate studies or political geography report that macro-level pressures due to changes in climate or economic scarcity can go along with social unrest and wars. How do these macro-level pressures relate to micro-level processes? Do they both occur independently, or do macro-level pressures trigger micro-level processes that cause intergroup conflict? And if so, which micro-level processes are triggered, and how? With unavoidable signs of climate change and increasing resource scarcities, answers to these questions are urgently needed. Here I propose carrying-capacity stress (CCS) as the missing link between macro-level pressures and micro-level processes. A group experiences CCS when its resources do not suffice to maintain its functionality. CCS is a function of macro-level pressures and creates intergroup conflict because it impacts micro-level motivation to contribute to one’s group’s fighting capacity and shapes the coordination of individual contributions to out-group aggression through emergent norms, communication and leadership. To test these propositions I develop a parametric model of CCS that is amenable to measurement and experimentation, and use techniques used in my work on conflict and cooperation: Meta-analyses and time-series analysis of macro-level historical data; experiments on intergroup conflict; and measurement of neuro-hormonal correlates of cooperation and conflict. In combination, this project provides novel multi-level conflict theory that integrates macro-level discoveries in climate research and political geography with micro-level processes uncovered in the biobehavioral sciences

2 490 383 €

Start date: 2018-08-01, End date: 2023-07-31

This project focuses on Sun-like stars, which possess convective envelopes and universally exhibit magnetic activity (in the mass range 0.1 to 1.3 MSun). The rotation of these stars influences their internal structure, energy and chemical transport, and magnetic field generation, as well as their external magnetic activity and environmental interactions. Due to the huge range of timescales, spatial scales, and physics involved, understanding how each of these processes relate to each other and to the long-term evolution remains an enormous challenge in astrophysics. To face this challenge, the AWESoMeStars project will develop a comprehensive, physical picture of the evolution of stellar rotation, magnetic activity, mass loss, and accretion. In doing so, we will (1) Discover how stars lose the vast majority of their angular momentum, which happens in the accretion phase (2) Explain the observed rotation-activity relationship and saturation in terms of the evolution of magnetic properties & coronal physics (3) Characterize coronal heating and mass loss across the full range of mass & age (4) Explain the Skumanich (1972) relationship and distributions of spin rates observed in young clusters & old field stars (5) Develop physics-based gyrochronology as a tool for using rotation rates to constrain stellar ages. We will accomplish these goals using a fundamentally new and multi-faceted approach, which combines the power of multi-dimensional MHD simulations with long-timescale rotational-evolution models. Specifically, we will develop a next generation of MHD simulations of both star-disk interactions and stellar winds, to model stars over the full range of mass & age, and to characterize how magnetically active stars impact their environments. Simultaneously, we will create a new class of rotational-evolution models that include external torques derived from our simulations, compute the evolution of spin rates of entire star clusters, & compare with observations.

2 206 205 €

Start date: 2016-07-01, End date: 2021-06-30

A new generation of galaxy surveys will soon start measuring the spatial distribution of millions of galaxies over a broad range of redshifts, offering an imminent opportunity to discover new physics. A detailed comparison of these measurements with theoretical models of galaxy clustering may reveal a new fundamental particle, a breakdown of General Relativity, or a hint on the nature of cosmic acceleration. Despite a large progress in the analytic treatment of structure formation in recent years, traditional clustering models still suffer from large uncertainties. This limits cosmological analyses to a very restricted range of scales and statistics, which will be one of the main obstacles to reach a comprehensive exploitation of future surveys. Here I propose to develop a novel simulation--based approach to predict galaxy clustering. Combining recent advances in computational cosmology, from cosmological N--body calculations to physically-motivated galaxy formation models, I will develop a unified framework to directly predict the position and velocity of individual dark matter structures and galaxies as function of cosmological and astrophysical parameters. In this formulation, galaxy clustering will be a prediction of a set of physical assumptions in a given cosmological setting. The new theoretical framework will be flexible, accurate and fast: it will provide predictions for any clustering statistic, down to scales 100 times smaller than in state-of-the-art perturbation--theory--based models, and in less than 1 minute of CPU time. These advances will enable major improvements in future cosmological constraints, which will significantly increase the overall power of future surveys maximising our potential to discover new physics.

1 484 240 €

Start date: 2017-09-01, End date: 2022-08-31

The standard model of cosmology, the ɅCDM model, is remarkably successful at explaining a wide range of observations of our Universe. However, it is now being subjected to much more stringent tests than ever before, and recent large-scale structure (LSS) measurements appear to be in tension with its predictions. Is this tension signalling that new physics is required? For example, time-varying dark energy, or perhaps a modified theory of gravity? A contribution from massive neutrinos? Before coming to such bold conclusions we must be certain that all of the important systematic errors in the LSS tests have been accounted for. Presently, the largest source of systematic uncertainty is from the modelling of complicated astrophysical phenomena associated with galaxy formation. In particular, energetic feedback processes associated with star formation and black hole growth can heat and expel gas from collapsed structures and modify the large-scale distribution of matter. Furthermore, the LSS field is presently separated into many sub-fields (each using different models, that usually neglect feedback), preventing a coherent analysis. Cosmological hydrodynamical simulations (are the only method which) can follow all the relevant matter components and self-consistently capture the effects of feedback. I have been leading the development of large-scale simulations with physically-motivated prescriptions for feedback that are unrivalled in their ability to reproduce the observed properties of massive systems. With ERC support, I will build a team to exploit these developments, to produce a suite of simulations designed specifically for LSS cosmology applications with the effects of feedback realistically accounted for and which will allow us to unite the different LSS tests. My team and I will make the first self-consistent comparisons with the full range of LSS cosmology tests, and critically assess the evidence for physics beyond the standard model.

1 725 982 €

Start date: 2018-06-01, End date: 2023-05-31