Project acronym 1D-Engine
Project 1D-electrons coupled to dissipation: a novel approach for understanding and engineering superconducting materials and devices
Researcher (PI) Adrian KANTIAN
Host Institution (HI) UPPSALA UNIVERSITET
Call Details Starting Grant (StG), PE3, ERC-2017-STG
Summary Correlated electrons are at the forefront of condensed matter theory. Interacting quasi-1D electrons have seen vast progress in analytical and numerical theory, and thus in fundamental understanding and quantitative prediction. Yet, in the 1D limit fluctuations preclude important technological use, particularly of superconductors. In contrast, high-Tc superconductors in 2D/3D are not precluded by fluctuations, but lack a fundamental theory, making prediction and engineering of their properties, a major goal in physics, very difficult. This project aims to combine the advantages of both areas by making major progress in the theory of quasi-1D electrons coupled to an electron bath, in part building on recent breakthroughs (with the PIs extensive involvement) in simulating 1D and 2D electrons with parallelized density matrix renormalization group (pDMRG) numerics. Such theory will fundamentally advance the study of open electron systems, and show how to use 1D materials as elements of new superconducting (SC) devices and materials: 1) It will enable a new state of matter, 1D electrons with true SC order. Fluctuations from the electronic liquid, such as graphene, could also enable nanoscale wires to appear SC at high temperatures. 2) A new approach for the deliberate engineering of a high-Tc superconductor. In 1D, how electrons pair by repulsive interactions is understood and can be predicted. Stabilization by reservoir - formed by a parallel array of many such 1D systems - offers a superconductor for which all factors setting Tc are known and can be optimized. 3) Many existing superconductors with repulsive electron pairing, all presently not understood, can be cast as 1D electrons coupled to a bath. Developing chain-DMFT theory based on pDMRG will allow these materials SC properties to be simulated and understood for the first time. 4) The insights gained will be translated to 2D superconductors to study how they could be enhanced by contact with electronic liquids.
Summary
Correlated electrons are at the forefront of condensed matter theory. Interacting quasi-1D electrons have seen vast progress in analytical and numerical theory, and thus in fundamental understanding and quantitative prediction. Yet, in the 1D limit fluctuations preclude important technological use, particularly of superconductors. In contrast, high-Tc superconductors in 2D/3D are not precluded by fluctuations, but lack a fundamental theory, making prediction and engineering of their properties, a major goal in physics, very difficult. This project aims to combine the advantages of both areas by making major progress in the theory of quasi-1D electrons coupled to an electron bath, in part building on recent breakthroughs (with the PIs extensive involvement) in simulating 1D and 2D electrons with parallelized density matrix renormalization group (pDMRG) numerics. Such theory will fundamentally advance the study of open electron systems, and show how to use 1D materials as elements of new superconducting (SC) devices and materials: 1) It will enable a new state of matter, 1D electrons with true SC order. Fluctuations from the electronic liquid, such as graphene, could also enable nanoscale wires to appear SC at high temperatures. 2) A new approach for the deliberate engineering of a high-Tc superconductor. In 1D, how electrons pair by repulsive interactions is understood and can be predicted. Stabilization by reservoir - formed by a parallel array of many such 1D systems - offers a superconductor for which all factors setting Tc are known and can be optimized. 3) Many existing superconductors with repulsive electron pairing, all presently not understood, can be cast as 1D electrons coupled to a bath. Developing chain-DMFT theory based on pDMRG will allow these materials SC properties to be simulated and understood for the first time. 4) The insights gained will be translated to 2D superconductors to study how they could be enhanced by contact with electronic liquids.
Max ERC Funding
1 491 013 €
Duration
Start date: 2018-10-01, End date: 2023-09-30
Project acronym 2DNANOPTICA
Project Nano-optics on flatland: from quantum nanotechnology to nano-bio-photonics
Researcher (PI) Pablo Alonso-González
Host Institution (HI) UNIVERSIDAD DE OVIEDO
Call Details Starting Grant (StG), PE3, ERC-2016-STG
Summary Ubiquitous in nature, light-matter interactions are of fundamental importance in science and all optical technologies. Understanding and controlling them has been a long-pursued objective in modern physics. However, so far, related experiments have relied on traditional optical schemes where, owing to the classical diffraction limit, control of optical fields to length scales below the wavelength of light is prevented. Importantly, this limitation impedes to exploit the extraordinary fundamental and scaling potentials of nanoscience and nanotechnology. A solution to concentrate optical fields into sub-diffracting volumes is the excitation of surface polaritons –coupled excitations of photons and mobile/bound charges in metals/polar materials (plasmons/phonons)-. However, their initial promises have been hindered by either strong optical losses or lack of electrical control in metals, and difficulties to fabricate high optical quality nanostructures in polar materials.
With the advent of two-dimensional (2D) materials and their extraordinary optical properties, during the last 2-3 years the visualization of both low-loss and electrically tunable (active) plasmons in graphene and high optical quality phonons in monolayer and multilayer h-BN nanostructures have been demonstrated in the mid-infrared spectral range, thus introducing a very encouraging arena for scientifically ground-breaking discoveries in nano-optics. Inspired by these extraordinary prospects, this ERC project aims to make use of our knowledge and unique expertise in 2D nanoplasmonics, and the recent advances in nanophononics, to establish a technological platform that, including coherent sources, waveguides, routers, and efficient detectors, permits an unprecedented active control and manipulation (at room temperature) of light and light-matter interactions on the nanoscale, thus laying experimentally the foundations of a 2D nano-optics field.
Summary
Ubiquitous in nature, light-matter interactions are of fundamental importance in science and all optical technologies. Understanding and controlling them has been a long-pursued objective in modern physics. However, so far, related experiments have relied on traditional optical schemes where, owing to the classical diffraction limit, control of optical fields to length scales below the wavelength of light is prevented. Importantly, this limitation impedes to exploit the extraordinary fundamental and scaling potentials of nanoscience and nanotechnology. A solution to concentrate optical fields into sub-diffracting volumes is the excitation of surface polaritons –coupled excitations of photons and mobile/bound charges in metals/polar materials (plasmons/phonons)-. However, their initial promises have been hindered by either strong optical losses or lack of electrical control in metals, and difficulties to fabricate high optical quality nanostructures in polar materials.
With the advent of two-dimensional (2D) materials and their extraordinary optical properties, during the last 2-3 years the visualization of both low-loss and electrically tunable (active) plasmons in graphene and high optical quality phonons in monolayer and multilayer h-BN nanostructures have been demonstrated in the mid-infrared spectral range, thus introducing a very encouraging arena for scientifically ground-breaking discoveries in nano-optics. Inspired by these extraordinary prospects, this ERC project aims to make use of our knowledge and unique expertise in 2D nanoplasmonics, and the recent advances in nanophononics, to establish a technological platform that, including coherent sources, waveguides, routers, and efficient detectors, permits an unprecedented active control and manipulation (at room temperature) of light and light-matter interactions on the nanoscale, thus laying experimentally the foundations of a 2D nano-optics field.
Max ERC Funding
1 459 219 €
Duration
Start date: 2017-01-01, End date: 2021-12-31
Project acronym 2DTHERMS
Project Design of new thermoelectric devices based on layered and field modulated nanostructures of strongly correlated electron systems
Researcher (PI) Jose Francisco Rivadulla Fernandez
Host Institution (HI) UNIVERSIDAD DE SANTIAGO DE COMPOSTELA
Call Details Starting Grant (StG), PE3, ERC-2010-StG_20091028
Summary Design of new thermoelectric devices based on layered and field modulated nanostructures of strongly correlated electron systems
Summary
Design of new thermoelectric devices based on layered and field modulated nanostructures of strongly correlated electron systems
Max ERC Funding
1 427 190 €
Duration
Start date: 2010-11-01, End date: 2015-10-31
Project acronym A-BINGOS
Project Accreting binary populations in Nearby Galaxies: Observations and Simulations
Researcher (PI) Andreas Zezas
Host Institution (HI) IDRYMA TECHNOLOGIAS KAI EREVNAS
Call Details Consolidator Grant (CoG), PE9, ERC-2013-CoG
Summary "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."
Summary
"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."
Max ERC Funding
1 242 000 €
Duration
Start date: 2014-04-01, End date: 2019-03-31
Project acronym ASD
Project Atomistic Spin-Dynamics; Methodology and Applications
Researcher (PI) Olof Ragnar Eriksson
Host Institution (HI) Uppsala University
Call Details Advanced Grant (AdG), PE3, ERC-2009-AdG
Summary Our aim is to provide a theoretical framework for studies of dynamical aspects of magnetic materials and magnetisation reversal, which has potential for applications for magnetic data storage and magnetic memory devices. The project focuses on developing and using an atomistic spin dynamics simulation method. Our goal is to identify novel materials and device geometries with improved performance. The scientific questions which will be addressed concern the understanding of the fundamental temporal limit of magnetisation switching and reversal, and the mechanisms which govern this limit. The methodological developments concern the ability to, from first principles theory, calculate the interatomic exchange parameters of materials in general, in particular for correlated electron materials, via the use of dynamical mean-field theory. The theoretical development also involves an atomistic spin dynamics simulation method, which once it has been established, will be released as a public software package. The proposed theoretical research will be intimately connected to world-leading experimental efforts, especially in Europe where a leading activity in experimental studies of magnetisation dynamics has been established. The ambition with this project is to become world-leading in the theory of simulating spin-dynamics phenomena, and to promote education and training of young researchers. To achieve our goals we will build up an open and lively environment, where the advances in the theoretical knowledge of spin-dynamics phenomena will be used to address important questions in information technology. In this environment the next generation research leaders will be fostered and trained, thus ensuring that the society of tomorrow is equipped with the scientific competence to tackle the challenges of our future.
Summary
Our aim is to provide a theoretical framework for studies of dynamical aspects of magnetic materials and magnetisation reversal, which has potential for applications for magnetic data storage and magnetic memory devices. The project focuses on developing and using an atomistic spin dynamics simulation method. Our goal is to identify novel materials and device geometries with improved performance. The scientific questions which will be addressed concern the understanding of the fundamental temporal limit of magnetisation switching and reversal, and the mechanisms which govern this limit. The methodological developments concern the ability to, from first principles theory, calculate the interatomic exchange parameters of materials in general, in particular for correlated electron materials, via the use of dynamical mean-field theory. The theoretical development also involves an atomistic spin dynamics simulation method, which once it has been established, will be released as a public software package. The proposed theoretical research will be intimately connected to world-leading experimental efforts, especially in Europe where a leading activity in experimental studies of magnetisation dynamics has been established. The ambition with this project is to become world-leading in the theory of simulating spin-dynamics phenomena, and to promote education and training of young researchers. To achieve our goals we will build up an open and lively environment, where the advances in the theoretical knowledge of spin-dynamics phenomena will be used to address important questions in information technology. In this environment the next generation research leaders will be fostered and trained, thus ensuring that the society of tomorrow is equipped with the scientific competence to tackle the challenges of our future.
Max ERC Funding
2 130 000 €
Duration
Start date: 2010-01-01, End date: 2014-12-31
Project acronym ASSESS
Project Episodic Mass Loss in the Most Massive Stars: Key to Understanding the Explosive Early Universe
Researcher (PI) Alceste BONANOS
Host Institution (HI) NATIONAL OBSERVATORY OF ATHENS
Call Details Consolidator Grant (CoG), PE9, ERC-2017-COG
Summary Massive stars dominate their surroundings during their short lifetimes, while their explosive deaths impact the chemical evolution and spatial cohesion of their hosts. After birth, their evolution is largely dictated by their ability to remove layers of hydrogen from their envelopes. Multiple lines of evidence are pointing to violent, episodic mass-loss events being responsible for removing a large part of the massive stellar envelope, especially in low-metallicity galaxies. Episodic mass loss, however, is not understood theoretically, neither accounted for in state-of-the-art models of stellar evolution, which has far-reaching consequences for many areas of astronomy. We aim to determine whether episodic mass loss is a dominant process in the evolution of the most massive stars by conducting the first extensive, multi-wavelength survey of evolved massive stars in the nearby Universe. The project hinges on the fact that mass-losing stars form dust and are bright in the mid-infrared. We plan to (i) derive physical parameters of a large sample of dusty, evolved targets and estimate the amount of ejected mass, (ii) constrain evolutionary models, (iii) quantify the duration and frequency of episodic mass loss as a function of metallicity. The approach involves applying machine-learning algorithms to existing multi-band and time-series photometry of luminous sources in ~25 nearby galaxies. Dusty, luminous evolved massive stars will thus be automatically classified and follow-up spectroscopy will be obtained for selected targets. Atmospheric and SED modeling will yield parameters and estimates of time-dependent mass loss for ~1000 luminous stars. The emerging trend for the ubiquity of episodic mass loss, if confirmed, will be key to understanding the explosive early Universe and will have profound consequences for low-metallicity stars, reionization, and the chemical evolution of galaxies.
Summary
Massive stars dominate their surroundings during their short lifetimes, while their explosive deaths impact the chemical evolution and spatial cohesion of their hosts. After birth, their evolution is largely dictated by their ability to remove layers of hydrogen from their envelopes. Multiple lines of evidence are pointing to violent, episodic mass-loss events being responsible for removing a large part of the massive stellar envelope, especially in low-metallicity galaxies. Episodic mass loss, however, is not understood theoretically, neither accounted for in state-of-the-art models of stellar evolution, which has far-reaching consequences for many areas of astronomy. We aim to determine whether episodic mass loss is a dominant process in the evolution of the most massive stars by conducting the first extensive, multi-wavelength survey of evolved massive stars in the nearby Universe. The project hinges on the fact that mass-losing stars form dust and are bright in the mid-infrared. We plan to (i) derive physical parameters of a large sample of dusty, evolved targets and estimate the amount of ejected mass, (ii) constrain evolutionary models, (iii) quantify the duration and frequency of episodic mass loss as a function of metallicity. The approach involves applying machine-learning algorithms to existing multi-band and time-series photometry of luminous sources in ~25 nearby galaxies. Dusty, luminous evolved massive stars will thus be automatically classified and follow-up spectroscopy will be obtained for selected targets. Atmospheric and SED modeling will yield parameters and estimates of time-dependent mass loss for ~1000 luminous stars. The emerging trend for the ubiquity of episodic mass loss, if confirmed, will be key to understanding the explosive early Universe and will have profound consequences for low-metallicity stars, reionization, and the chemical evolution of galaxies.
Max ERC Funding
1 128 750 €
Duration
Start date: 2018-09-01, End date: 2023-08-31
Project acronym ASTRODYN
Project Astrophysical Dynamos
Researcher (PI) Axel Brandenburg
Host Institution (HI) KUNGLIGA TEKNISKA HOEGSKOLAN
Call Details Advanced Grant (AdG), PE9, ERC-2008-AdG
Summary Magnetic fields in stars, planets, accretion discs, and galaxies are believed to be the result of a dynamo process converting kinetic energy into magnetic energy. This work focuses on the solar dynamo, but dynamos in other astrophysical systems will also be addressed. In particular, direct high-resolution three-dimensional simulations are used to understand particular aspects of the solar dynamo and ultimately to simulate the solar dynamo as a whole. Phenomenological approaches will be avoided in favor of obtaining rigorous results. A major problem is catastrophic quenching, i.e. the decline of dynamo effects in inverse proportion to the magnetic Reynolds number, which is huge. Tremendous advances have been made in the last few years since the cause of catastrophic quenching in dynamos has been understood in terms of magnetic helicity evolution. The numerical tools are now in place to allow for magnetic helicity fluxes via coronal mass ejections, thus alleviating catastrophic quenching. This work employs simulations in spherical shells, augmented by Cartesian simulations in special cases. The roles of the near-surface shear layer, the tachocline, as well as pumping in the bulk of the convection zone are to be clarified. The Pencil Code will be used for most applications. The code is third order in time and sixth order in space and is used for solving the hydromagnetic equations. It is a public domain code developed by roughly 20 scientists world wide and maintained under an a central versioning system at Nordita. Automatic nightly tests of currently 30 applications ensure the integrity of the code. It is used for a wide range of applications and may include the effects of radiation, self-gravity, dust, chemistry, variable ionization, cosmic rays, in addition to those of magnetohydrodynamics. The code with its infrastructure offers a good opportunity for individuals within a broad group of people to develop new tools that may automatically be useful to others.
Summary
Magnetic fields in stars, planets, accretion discs, and galaxies are believed to be the result of a dynamo process converting kinetic energy into magnetic energy. This work focuses on the solar dynamo, but dynamos in other astrophysical systems will also be addressed. In particular, direct high-resolution three-dimensional simulations are used to understand particular aspects of the solar dynamo and ultimately to simulate the solar dynamo as a whole. Phenomenological approaches will be avoided in favor of obtaining rigorous results. A major problem is catastrophic quenching, i.e. the decline of dynamo effects in inverse proportion to the magnetic Reynolds number, which is huge. Tremendous advances have been made in the last few years since the cause of catastrophic quenching in dynamos has been understood in terms of magnetic helicity evolution. The numerical tools are now in place to allow for magnetic helicity fluxes via coronal mass ejections, thus alleviating catastrophic quenching. This work employs simulations in spherical shells, augmented by Cartesian simulations in special cases. The roles of the near-surface shear layer, the tachocline, as well as pumping in the bulk of the convection zone are to be clarified. The Pencil Code will be used for most applications. The code is third order in time and sixth order in space and is used for solving the hydromagnetic equations. It is a public domain code developed by roughly 20 scientists world wide and maintained under an a central versioning system at Nordita. Automatic nightly tests of currently 30 applications ensure the integrity of the code. It is used for a wide range of applications and may include the effects of radiation, self-gravity, dust, chemistry, variable ionization, cosmic rays, in addition to those of magnetohydrodynamics. The code with its infrastructure offers a good opportunity for individuals within a broad group of people to develop new tools that may automatically be useful to others.
Max ERC Funding
2 220 000 €
Duration
Start date: 2009-02-01, End date: 2014-01-31
Project acronym BACCO
Project Bias and Clustering Calculations Optimised: Maximising discovery with galaxy surveys
Researcher (PI) Raúl Esteban ANGULO de la Fuente
Host Institution (HI) FUNDACION CENTRO DE ESTUDIOS DE FISICA DEL COSMOS DE ARAGON
Call Details Starting Grant (StG), PE9, ERC-2016-STG
Summary 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.
Summary
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.
Max ERC Funding
1 484 240 €
Duration
Start date: 2017-09-01, End date: 2022-08-31
Project acronym BePreSysE
Project Beyond Precision Cosmology: dealing with Systematic Errors
Researcher (PI) Licia VERDE
Host Institution (HI) UNIVERSITAT DE BARCELONA
Call Details Consolidator Grant (CoG), PE9, ERC-2016-COG
Summary Over the past 20 years cosmology has made the transition to a precision science: the standard cosmological model has been established and its parameters are now measured with unprecedented precision. But precision is not enough: accuracy is also crucial. Accuracy accounts for systematic errors which can be both on the observational and on the theory/modelling side (and everywhere in between). While there is a well-defined and developed framework for treating statistical errors, there is no established approach for systematic errors. The next decade will see the era of large surveys; a large coordinated effort of the scientific community in the field is on-going to map the cosmos producing an exponentially growing amount of data. This will shrink the statistical errors, making mitigation and control of systematics of the utmost importance. While there are isolated and targeted efforts to quantify systematic errors and propagate them through all the way to the final results, there is no well-established, self-consistent methodology. To go beyond precision cosmology and reap the benefits of the forthcoming observational program, a systematic approach to systematics is needed. Systematics should be interpreted in the most general sense as shifts between the recovered measured values and true values of physical quantities. I propose to develop a comprehensive approach to tackle systematic errors with the goal to uncover and quantify otherwise unknown differences between the interpretation of a measurement and reality. This will require to fully develop, combine and systematize all approaches proposed so far (many pioneered by the PI), develop new ones to fill the gaps, study and explore their interplay and finally test and validate the procedure. Beyond Precision Cosmology: Dealing with Systematic Errors (BePreSysE) will develop a framework to deal with systematics in forthcoming Cosmological surveys which, could, in principle, be applied beyond Cosmology.
Summary
Over the past 20 years cosmology has made the transition to a precision science: the standard cosmological model has been established and its parameters are now measured with unprecedented precision. But precision is not enough: accuracy is also crucial. Accuracy accounts for systematic errors which can be both on the observational and on the theory/modelling side (and everywhere in between). While there is a well-defined and developed framework for treating statistical errors, there is no established approach for systematic errors. The next decade will see the era of large surveys; a large coordinated effort of the scientific community in the field is on-going to map the cosmos producing an exponentially growing amount of data. This will shrink the statistical errors, making mitigation and control of systematics of the utmost importance. While there are isolated and targeted efforts to quantify systematic errors and propagate them through all the way to the final results, there is no well-established, self-consistent methodology. To go beyond precision cosmology and reap the benefits of the forthcoming observational program, a systematic approach to systematics is needed. Systematics should be interpreted in the most general sense as shifts between the recovered measured values and true values of physical quantities. I propose to develop a comprehensive approach to tackle systematic errors with the goal to uncover and quantify otherwise unknown differences between the interpretation of a measurement and reality. This will require to fully develop, combine and systematize all approaches proposed so far (many pioneered by the PI), develop new ones to fill the gaps, study and explore their interplay and finally test and validate the procedure. Beyond Precision Cosmology: Dealing with Systematic Errors (BePreSysE) will develop a framework to deal with systematics in forthcoming Cosmological surveys which, could, in principle, be applied beyond Cosmology.
Max ERC Funding
1 835 220 €
Duration
Start date: 2017-06-01, End date: 2022-05-31
Project acronym BioInspired_SolarH2
Project Engineering Bio-Inspired Systems for the Conversion of Solar Energy to Hydrogen
Researcher (PI) Elisabet ROMERO MESA
Host Institution (HI) FUNDACIO PRIVADA INSTITUT CATALA D'INVESTIGACIO QUIMICA
Call Details Starting Grant (StG), PE3, ERC-2018-STG
Summary With this proposal, I aim to achieve the efficient conversion of solar energy to hydrogen. The overall objective is to engineer bio-inspired systems able to convert solar energy into a separation of charges and to construct devices by coupling these systems to catalysts in order to drive sustainable and effective water oxidation and hydrogen production.
The global energy crisis requires an urgent solution, we must replace fossil fuels for a renewable energy source: Solar energy. However, the efficient and inexpensive conversion and storage of solar energy into fuel remains a fundamental challenge. Currently, solar-energy conversion devices suffer from energy losses mainly caused by disorder in the materials used. The solution to this problem is to learn from nature. In photosynthesis, the photosystem II reaction centre (PSII RC) is a pigment-protein complex able to overcome disorder and convert solar photons into a separation of charges with near 100% efficiency. Crucially, the generated charges have enough potential to drive water oxidation and hydrogen production.
Previously, I have investigated the charge separation process in the PSII RC by a collection of spectroscopic techniques, which allowed me to formulate the design principles of photosynthetic charge separation, where coherence plays a crucial role. Here I will put these knowledge into action to design efficient and robust chromophore-protein assemblies for the collection and conversion of solar energy, employ organic chemistry and synthetic biology tools to construct these well defined and fully controllable assemblies, and apply a complete set of spectroscopic methods to investigate these engineered systems.
Following the approach Understand, Engineer, Implement, I will create a new generation of bio-inspired devices based on abundant and biodegradable materials that will drive the transformation of solar energy and water into hydrogen, an energy-rich molecule that can be stored and transported.
Summary
With this proposal, I aim to achieve the efficient conversion of solar energy to hydrogen. The overall objective is to engineer bio-inspired systems able to convert solar energy into a separation of charges and to construct devices by coupling these systems to catalysts in order to drive sustainable and effective water oxidation and hydrogen production.
The global energy crisis requires an urgent solution, we must replace fossil fuels for a renewable energy source: Solar energy. However, the efficient and inexpensive conversion and storage of solar energy into fuel remains a fundamental challenge. Currently, solar-energy conversion devices suffer from energy losses mainly caused by disorder in the materials used. The solution to this problem is to learn from nature. In photosynthesis, the photosystem II reaction centre (PSII RC) is a pigment-protein complex able to overcome disorder and convert solar photons into a separation of charges with near 100% efficiency. Crucially, the generated charges have enough potential to drive water oxidation and hydrogen production.
Previously, I have investigated the charge separation process in the PSII RC by a collection of spectroscopic techniques, which allowed me to formulate the design principles of photosynthetic charge separation, where coherence plays a crucial role. Here I will put these knowledge into action to design efficient and robust chromophore-protein assemblies for the collection and conversion of solar energy, employ organic chemistry and synthetic biology tools to construct these well defined and fully controllable assemblies, and apply a complete set of spectroscopic methods to investigate these engineered systems.
Following the approach Understand, Engineer, Implement, I will create a new generation of bio-inspired devices based on abundant and biodegradable materials that will drive the transformation of solar energy and water into hydrogen, an energy-rich molecule that can be stored and transported.
Max ERC Funding
1 500 000 €
Duration
Start date: 2019-04-01, End date: 2024-03-31
