for pioneering research in the dynamics of binary compact objects as gravitational wave sources in galactic nuclei and dense star clusters.
Prof. Manuel Arca Sedda obtained his PhD in 2014 at the University La Sapienza. He then became a postdoctoral fellow at the University of Tor Vergata and moved, two years later, to the Heidelberg University at the Astronomisches Rechen Institut, where he started pursuing research on the formation and evolution of black holes of all sizes. He was awarded in 2018 an Alexander von Humboldt Fellowship and has recently obtained a Marie Skłodowska-Curie Individual Fellowship at the University of Padova. In May 2023, he will join the Gran Sasso Science Institute as an assistant professor. He is a member of several international collaborations, such as the Laser Interferometer Space Antenna, the Einstein Telescope Consortium, and the Lunar Gravitational Wave Antenna. His main research focuses on the formation of stellar and intermediate-mass black holes in dense star clusters and close to supermassive black holes in galactic nuclei.
Since the first detection of gravitational waves emitted during the merger of two black holes, understanding the formation channels of such systems has become one of the most pressing questions in theoretical astrophysics. Prof. Arca Sedda has delivered key results to shed light on the formation of binary black holes. He demonstrated that the dynamical evolution of stellar-born black holes in dense star clusters and galactic nuclei can result in a great variety of black hole masses and spins. Studying the interactions that occur in star clusters with and without a central black hole sub-system, he developed one of the first systematic studies of black hole-neutron star mergers forming in young, globular, and nuclear clusters, and suggested that one of the mergers, GW190814, could have had originated in a massive star cluster. Moreover, Manuel Arca Sedda studied the possible seeding and growth of intermediate-mass black holes in massive star clusters, pinning down both the astrophysical properties of these objects and their possible observation as gravitational-wave sources. Using state-of-the-art numerical simulations at unprecedented resolution, he developed a systematic study of nuclear cluster formation via in-spiral and merger of star clusters formed close to the central regions of galaxies, leading a unique series of papers focused on the dynamics of stellar- and intermediate-mass black holes delivered close to a supermassive black hole by spiralling star clusters.
The work of Prof. Manuel Arca Sedda was conducted at the University La Sapienza, Heidelberg University, and the University of Padova.
for her pioneering work using state-of-the-art IFU instruments, in particular for her work demonstrating the impact of supermassive black holes on their host galaxies and the large-scale environment.
Dr Dominika Wylezalek studied physics at Heidelberg University, Germany (BSc, 2010), and the University of Cambridge, UK (MASt, Part III Physics, 2011). In 2014, she received her PhD from Munich University (LMU) with a fellowship from the International Max Planck Research School on Astrophysics which she had spent at the European Southern Observatory (ESO) in Garching/Munich. She then worked as a postdoctoral researcher at the Johns Hopkins University, Baltimore, USA, where she held an Akbari-Mack and Provost Postdoctoral Fellowship. She then moved to ESO in Munich as an ESO Fellow. Since 2020, she has been leading her Emmy Noether Group at the Center for Astronomy of Heidelberg University. Her research focuses on the exploration of the role of AGN and quasars in galaxy evolution, one of the most important and pressing questions in extragalactic astronomy today.
Dominika Wylezalek is a world expert on the evolution of galaxies with intense AGN-driven activity and their impact on the intergalactic, circumgalactic and even galaxy cluster-scale environment. She uses a multi-wavelength, multi-technique, multi-scale and multi-era approach. During her PhD, Dominika found that powerful radio-loud AGN appear to trace very dense and massive distant galaxy proto-clusters, in which galaxy evolution seems to occur at an accelerated pace. As a junior postdoc, Dominika Wylezalek focused on the relation between AGN and galaxy evolution. Using large galaxy and AGN samples at low redshift, and smaller unique AGN samples at high redshift, she has developed new ideas and approaches on how to investigate AGN feedback processes. She has developed new spatially resolved techniques for identifying signatures of AGN, uncovering a much more nuanced picture of AGN activity. She has been and is leading several cutting-edge research projects on AGN feedback using ESO, ALMA, and JWST. She is PI of a JWST Early Release Science project (Q3D) and has become one of the leading experts for AGN science with the JWST. The initial Q3D data already resulted in an impressive and unanticipated result, namely identifying one of the densest knots of galaxy formation around a high-redshift quasar. The work received worldwide recognition, including media attention through several press releases. Under Wylezalek's lead, the Q3D team is actively working on several upcoming publications with their unique JWST data.
The work was conducted at Johns Hopkins University, the European Southern Observatory, and at Heidelberg University.
for his leading role in computational astrophysics, in particular for the IllustrisTNG series of cosmological simulations and his work to enable their widespread use.
Dr Dylan Nelson triple-majored in physics, mathematics, and astrophysics at the University of California, Berkeley. He completed his PhD at Harvard University in 2015. Dylan became one of the earliest active developers of the AREPO moving-mesh code for galaxy formation simulations, making key contributions to the original Illustris cosmological simulation. He was the recipient of the National Science Foundation Graduate Research Fellowship, as well as the Institute for Applied Computational Science Fellowship. In addition to his PhD, he obtained a secondary degree in Computational Science and Engineering at Harvard. He then moved to the Max Planck Institute for Astrophysics as a postdoctoral fellow (2015-2020). He became a key figure and leader of the IllustrisTNG simulations. He is the Co-PI of the TNG50 simulation, completed in 2019, a cosmological galaxy formation simulation of unprecedented scope and resolution. In 2020 he was awarded an Emmy Noether Research Group Leader position at Heidelberg University. He received the Research Career Development Award of the Hector Fellow Academy in 2022.
Dylan Nelson develops, carries out, and studies large numerical calculations of structure formation across cosmic time. He has played a unique role in making publicly accessible some of the largest and most sophisticated cosmological simulations, namely, IllustrisTNG. The simulation has (i) re-shaped our theoretical understanding of galaxy feedback and the impact of AGN-driven outflows, (ii) predicted how galactic disks and morphological structure emerge at early epochs, as now being probed with JWST, and (iii) provided foundational theoretical predictions for space telescope mission proposals. Based in part on the IllustrisTNG simulations, Dylan Nelson has studied the dynamics of the diffuse gas outside of galaxies, in the intergalactic medium and circumgalactic medium (CGM). His results have changed our understanding of cold, filamentary accretion flows, and their ability to feed high-redshift galaxies. One of the most scientifically exciting and novel results is that the CGM encodes a non-trivial "historical record" of past galactic feedback activity. The release of the simulations to the community is a high-impact example of Open Science in astronomy. Dylan Nelson has designed and developed the entire infrastructure to enable researchers to remotely explore, search, analyse, and download these petabyte-scale datasets (www.tng-project.org/data). Since its launch, more than 5,200 registered users have downloaded tens of thousands of simulation snapshots and catalogues, and tens of millions of individual galaxy datasets.
The work was conducted at Max Planck Institute for Astrophysics and at the Institute of Theoretical Astrophysics, which is part of the Centre for Astronomy of Heidelberg University.
for his multi-faceted approach to the field of galactic archaeology that transformed our understanding of the history and dynamics of the Milky Way.
Dr Helmer Koppelman studied astrophysics at the University of Groningen, obtaining his MSc in 2016 “ cum laude ” with a thesis on the evolution of gaps in cold stellar streams. Dr. Koppelman defended his PhD thesis at the University of Groningen in 2020 with the judicium "cum laude". In his remarkably extensive and broad thesis, Dr Koppelman combined theory, simulations, and vast datasets to yield new light on the structure and dynamics of the Milky Way halo and revolutionary new insights on its formation history. He spent a postdoc at the Institute for Advanced Study in Princeton and moved back to the Netherlands to start a new career as data scientist in an international company.
Dr Koppelman has produced an outstanding thesis on the formation and dynamics of the Galactic halo. The thesis offers new insights on how the Milky Way formed based on the newest datasets available and presents new modelling efforts and provides also a new characterization on the properties of dark matter halo of the Milky Way. Using Gaia DR2 data he discovered of a blob of stars that make up the local Galactic halo, which has been interpreted in terms of a large merger event that took place about 10 Gyr ago.
He further pushed the boundaries by fully exploiting the whole Gaia DR2 dataset, using the 1.3 billion stars with proper motion information to construct the biggest sample of halo stars currently available. Using data-mining tools, Dr Koppelman obtained the most precise lower limit to the mass of the Milky Way. In his thesis he further investigated the use of orbital frequencies to understand the gaps in narrow stellar streams, with as goal to put limits on the presence and properties of (dark matter) clumps in the halo.
Dr Koppelman's thesis excelled in the rigor of the analysis and detailed attention to uncertainties while keeping the broad overview of the scientific results and implications. Whereas most of the techniques were known, they were applied in rigorous way to totally new data with careful inference supported in an innovative way by insights from numerical simulations.
The PhD thesis of Dr Helmer Koppelman was conducted at the Kapteyn Astronomical Institute (Univ. of Groningen), under the supervision of Profs. Amina Helmi and Eline Tolstoy.
for the discovery of many new free-floating planets, which illuminated the origin of these exotic nomad planets.
Dr Miret Roig received a BSc in Physics and a MSc in Astrophysics from the University of Barcelona and obtained her PhD in 2020 from the University of Bordeaux, France, who also rewarded it with the Science and Technology Thesis Prize. Dr. Miret Roig expertise includes acquiring and analyzing massive observational datasets of nearby, young stars to derive fundamental properties such as the initial mass function, the spatial distribution, and the kinematics and dynamics of these systems. She has been co-PI of several successful proposals at major telescopes such as the GTC, VLT and CTIO, and led several studies of different aspects of the star formation process. Dr Miret Roig moved recently to a postdoc position at the University of Vienna, where she investigates the formation and origin of young stars in the solar neighbourhood.
Dr Núria Miret Roig's thesis presents the discovery of about a hundred new free-floating planets (FFPs) in the region encompassed by the Upper Scorpius stellar OB association and the Ophiuchus star-forming region. This sample is the largest ever discovered and constitutes an important step in setting the FFPs class and uncovering the origins and characteristics of these mysterious galactic nomads. Dr. Miret Roig demonstrated, for the first time, that the gravitational collapse of small clouds alone cannot explain the large fraction of observed FFPs. Instead, Dr. Miret-Roig thesis showed that an important fraction formed like planets but were ejected due to dynamical interactions.
Dr Miret Roig led an international team to combine images in public astronomical archives with new deep wide-field observations obtained with the best infrared and optical telescopes in the world, to measure proper motions and photometry of tens of millions of sources in a large area of the sky (171 square degrees). Dr. Miret-Roig used modern statistical and data mining techniques to identify the few thousands of stars and planets belonging to the young stellar association against the millions of background stars and galaxies. She obtained the mass function across four orders of magnitude for two regions of different ages (<10 Myr and 30 Myr), which now serve as a benchmark for defining the FFPs class, comparing to other regions, and testing theoretical models. Additionally, she presented a new methodology to determine the ages of young stellar associations based on their kinematics, in particular stemming from Gaia data. Dr Miret Roig has finished her PhD in three years with five articles as first author in high impact reviews.
The PhD thesis of Núria Miret-Roig was conducted at the Laboratoire d'Astrophysique de Bordeaux, University of Bordeaux (France), under the supervision of Prof. Hervé Bouy and Dr Javier Olivares.
for the development of novel laser frequency combs for the accurate calibration and extreme radial velocity-precision of astronomical spectrographs.
Dr Ewelina Obrzud graduated from the University of Geneva, Switzerland with a Master degree in Physics (specialisation in Astrophysics), and obtained in 2019 an interdisciplinary doctoral thesis (extra-solar planets and instrumentation) from the same university in collaboration with the Centre Suisse d'Electronique et de Microtechnique (CSEM), focussing on building and demonstrating alternatives for the existing laser frequency comb systems for astronomy. The quality of her thesis led her to be granted the Edith Alice Müller Award in 2020 by the Swiss Society for Astrophysics and Astronomy. Dr Obrzud has recently been promoted research & development engineer at CSEM.
In her PhD, Dr Obrzud developed two novel laser frequency combs for a precise and accurate calibration of extreme-radial-velocity-precision astronomical spectrographs. Both solutions are based on technologies providing laser pulses at ultra-high repetition rate (>10 GHz), a major challenge from a laser physics perspective but essential for spectrograph calibration. The first system, the electro-optic frequency comb, is characterized by an all-optical fibre-based design and simple architecture. The second system is based on dissipative Kerr soliton generation in optical microresonators. Dr Obrzud tested both systems, the electro-optic and Kerr frequency combs on astronomical spectrographs, demonstrating “real-life” operability and performance. She extended the scope of her work to a technique for frequency comb generation in the visible wavelength range, with a novel technique relying on triple-sum frequency generation in a nonlinear optical waveguide.
Dr Obrzud's work resulted in several peer-reviewed publications, four of them as first author, two of which in a Nature sub-journal. She also participated to international topical conferences and presented her results through talks and posters in conferences and workshops related to precise radial-velocity measurements and high-fidelity spectroscopy. Dr Obrzud's thesis work offers interesting solutions and concrete perspectives for the improvement of existing and future extreme-precision spectrographs for astronomy. While guided by the astronomical application, Dr Obrzud's work also attracted the attention of a wider interdisciplinary community including in particular those concerned with optical precision spectroscopy and nonlinear microphotonics.
The PhD thesis of Ewelina Obrzud was conducted at the Centre Suisse d'Electronique et Microtechnique (CSEM) in Neuchâtel and at the Department of Astronomy of the University of Geneva, under the supervision of Prof. Francesco Pepe, Dr François Wildi, and Dr Tobias Herr. The doctor title of “ Dr es sciences ” was granted by the University of Geneva with the tag 'Interdisciplinaire'.
for ground-breaking contributions in stellar astrophysics, including dynamo theory, predictions of solar flares and pioneering work on star-exoplanet interactions.
After fundamental studies in ENSTA-ParisTech, Antoine Strugarek obtained an MSc in Physics and Applied Maths. He then obtained a PhD joint between CEA Astrophysics Dept. and Fusion Dept., working on turbulent plasma confinement in the Sun and in Tokamak device. The creativity and robustness of his broad work was recognized as the best PhD in 2013 by the French Astronomical Society. He then moved to Canada, where he was awarded a CITA fellowship and a fellowship from Québec. He then came back to France to prepare the exploitation of Solar Orbiter (2016-2018). In 2018, he moved as a tenured researcher to the Dept. of Astrophysics of CEA Paris-Saclay to work on the Sun, stars and their interactions with exo-planets. Dr. Strugarek, is a highly-recognized expert on several topics: turbulent plasma confinement and turbulent dynamos, evolution of magnetism in star-planet systems, solar flare prediction and evolution.
Dr Antoine Strugarek tackled the difficult problem of magnetic confinement of turbulent plasmas using ambitious giro-kinetic simulations. He performed, with Prof. Jean-Paul Zahn, the first 3D global MHD model of the Sun from deep inside the radiative zone all the way to the surface. His key results include the proof that turbulence can be controlled by acting on the temperature gradient, improving the stability of Tokamak plasmas, and the fact that magnetic fields cannot prevent the spread of the solar tachocline contrary to horizontal turbulence.
Dr Strugarek led an unprecedented study of stellar dynamos. He conducted a coherent suite of convective dynamo simulations, spanning several effective temperatures and Rossby numbers, to measure the influence of rotation and stellar mass on magnetic field generation, which allowed him to derive scaling laws for stellar magnetism, and reconciled theoretical understanding of solar and stellar magnetic cycles. He also worked on a forecasting model for solar flares, based on self-organized critical models. His research was furthermore at the heart of the preparation to exploit the ESA Solar Orbiter, focusing on the how the Sun controls heliosphere.
Dr Strugarek has developed leading simulations of stellar winds and star-planet magnetic interactions. His group performed among the first comparisons of models and data for star-planet interactions, thanks to major allocations to the largest supercomputers in Europe.
The work of Dr Antoine Strugarek has been conducted at CEA and CNES, France, and University of Montréal, Canada.
for the investigation of the extremes of stellar explosions, providing a pioneering contribution to their understanding and their role in astronomy and astrophysics.
Dr Inserra obtained his PhD in 2012 from the University of Catania. He moved as Postdoc to Queen's University Belfast, United Kingdom where he was awarded the Royal Astronomical Society Winton Capital Award 2017. He moved to the University of Southampton in 2017, and then in 2018 to Cardiff University as Lecturer. Since 2019, he has been the principal investigator and survey manager of the largest worldwide spectroscopic survey in time-domain astronomy (ePESSTO+). His research strengths and cross-disciplinary skills led him to hold the Deputy Director of Research position at the School of Physics and Astronomy at Cardiff University, and that of Ambassador at the Data Intensive Research Institute in Cardiff.
Dr Cosimo Inserra's work has had a significant impact on time-domain astrophysics, cosmology and machine learning applied to astronomy. His seminal paper, that is still shaping the transient astronomy field presented the first sample analysis of a newly-discovered class of supernovae that defied previous knowledge of supernova explosions. He showed that the characteristic observational evidence of a supernova explosion could be reproduced by the energy deposition of a newborn magnetar. This investigation has been pivotal in the understanding of this new class of supernovae, which usually explode in low-metallicity, star-forming galaxies and are among the brightest explosions.
Dr Inserra has obtained pioneering work in different fields. He discovered a twin class of superluminous supernovae. The findings leading to the geometrical shape and the cosmological usefulness of superluminous supernovae have been pivotal studies expanding the frontier of cosmic explosions and opening a plethora of synergies with stellar and universe evolution over cosmic time up to z~10.
Dr Inserra is now the lead scientist and survey director of the current extension of the largest, worldwide, spectroscopic survey in time-domain astronomy, ePESSTO+. His vision of time-domain astronomy priorities and a new observing strategy has allowed ePESSTO+ to further improve efficiency and timeliness with respect to its earlier two progenitor surveys. He is a member of the Euclid Consortium leading the science area of the extremes of the supernova population, as well as a UK Principal Investigator and UK point of contact for Transient and Variable Stars science of the LSST Consortium at the Vera Rubin Observatory.
The work of Dr Cosimo Inserra has been conducted at Queens University Belfast, the University of Southampton and Cardiff University, United Kingdom.
for her fundamental contribution to the study of circumplanetary disks in planet formation, and the origin of the moons of giant planets.
Prof. Judit Szulágyi obtained a Master in Astronomy from Eötvös Loránd University, Hungary and then her PhD from the University of Nice Sophia Antipolis at the Observatoire de la Côte d'Azur in 2015. Shen then moved to ETH Zürich as postdoctoral fellow. In 2017 she was awarded an Ambizione Fellowship at the University of Zürich, until she returned in 2021 to ETH Zürich with an ERC starting grant. Prof. Szulágyi was listed on Forbes Europe "30 under 30 in Science" and obtained several prizes in Hungary and the Pro Scientia Golden Medal from the Hungarian Academy of Sciences. Her main topic is the study of circumplanetary disks and exomoon formation.
Prof. Judit Szulágyi has become a leading export of the rapidly developing research field of circumplanetary disks and in-situ moon formation. She conjugates deep theoretical and computational insight with the pragmatic attitude of a phenomenologist who delivers testable predictions for circumplanetary disk observations, and to guide the new exciting endeavor of exomoon detection. The whole notion of circumplanetary disks of gas and dust being a natural outcome of the planet formation process, both in core accretion and in disk instability, is new in exoplanet theory. Its implications for understanding the growth of massive planets owes a lot to Prof. Szulágyi's work. This is one of the very few important conceptual additions to the conventional core accretion formation scenario.
Prof. Szulágyi has been among the first scientists to describe the meridional circulation in circumplanetary disks, which she discovered in her hydrodynamical simulations, and which receives now observational support. Since her PhD, she authored many first-author in which all aspects of circumplanetary disks physics and satellites/exomoons formation, from the impact of circumplanetary disks on accretion shocks and the growth of giant planets to the growth of planetesimals in dust traps in circumplanetary disks, to satellites of gas and ice giants as well as their implications for exomoon formation.
Prof. Szulágyi is also working actively with observers using mock observations of her simulations to guide observational strategies to detect such disks around young planets, and interpret information contained in the observations, e.g., with ALMA and SPHERE. Moreover, recently observations of a circumplanetary disk have matched predictions by Szulágyi, and in general her ALMA dust continuum mocks correctly guided observers to discover new circumplanetary disks.
The work of Prof. Szulágyi has been conducted at the Observatoire de la Côte d'Azur, France, ETH Zürich and University of Zürich, Switzerland.
for fundamental contributions to the physics of the interstellar medium and the process of star formation.
Dr Aris Tritsis has been a post-doctoral fellow at the Research School of Astronomy & Astrophysics of the Australian National University since 2017. He studied Physics at the University of Ioannina and in 2013 he graduated with a master's degree in Astrophysics from the University College of London. He obtained his PhD at the University of Crete (2014 - 2017) where he worked on the physics of star formation, astrochemistry, and molecular line radiative transfer. He is a member of the SPICA collaboration aiming to launch the cryogenic infrared satellite for the ESA M5 slot.
Dr Tritsis studied a wide range of physical processes, from interstellar chemistry to cloud dynamics and radiative transfer. He made fundamental contributions to the understanding of the physical origin of striations (quasi-periodic, ordered structures in the low-density parts of otherwise chaotic-looking interstellar clouds). He demonstrated that striations are the result of magnetosonic waves, and he confirmed the predictions of this model by discovering normal modes that have been set up in an isolated cloud, the Musca molecular cloud, by these waves. In a highly surprising and impactful discovery, he used these normal modes to reconstruct the 3-dimensional shape of Musca. Tritsis showed that Musca is pancake-like, a sheet seen edge-on. This work received world-wide attention, both by scientists and the general public.
Using hydrodynamical numerical simulations coupled with the largest chemical network to date (300 species, 14,000 reactions, gas and grain species), Tritsis identified the best molecules to probe the true 3D shape of cloud cores. Tritsis is also the developer of the line radiative transfer code PyRaTE. He used it to post process the results of his MHD simulations of star forming regions to compare with observations.
Since his graduation, based on his PhD thesis results, Tritsis has developed a novel analytical method for measuring the magnetic field strength, taking advantage of the fact that striations are the imprint of hydromagnetic waves. He is currently using this method to create a 3D atlas of the magnetic field strength in the Milky Way.
The PhD thesis of Aris Tritsis was conducted at the University of Crete under the supervision of Prof. Konstantinos Tassis. He was also member of the Astrophysics Group at the Institute of Electronic Structure and Laser of the Foundation for Research and Technology - Hellas.
for spectacular results that have transformed the way we see and understand distant galaxies across time.
Dr Jorryt Matthee obtained his BSc degree from Utrecht on the observability of multiple stellar generations in globular clusters. He continued his studies at Leiden, where he got his MSc Cum Laude in 2012. Jorryt was then awarded a prestigious Huygens PhD fellowship by Leiden University to work on his own research project at Sterrewacht Leiden, combining observational studies of distant galaxies and theoretical analysis. Dr Matthee's thesis in late 2018 received the prize for best PhD thesis in the Leiden Science Faculty, and was distinguished by the 2018 IAU PhD Prize for Division J: Galaxies and Cosmology. Jorryt Matthee currently holds a Zwicky fellowship on extragalactic astrophysics at ETH Zürich, using emission lines to study the early formation of distant galaxies with ground and space observatories. Dr Matthee, furthermore, make use of state-of-the-art cosmological hydrodynamical simulations to understand which physical mechanisms make galaxies different and cause the scatter in galaxy scaling relations.
Dr Jorryt Matthee's thesis presents spectacular results in 11 first-author papers that have transformed the way we see and understand distant galaxies across time. His own state-of-the-art observations with ALMA, Hubble and the VLT revealed that very distant galaxies are complex, actively assembling systems. Jorryt discovered some of the brightest distant galaxies and has also investigated the co-evolution of dark matter halos and galaxies in the state-of-the-art cosmological EAGLE simulation.
Dr Matthee discovered some of the brightest distant galaxies and showed that they are much more common than previously thought, with important consequences for future space missions like Euclid. Jorryt's PhD work also mapped, dissected and discussed how galaxies have evolved over the first few billion years of the Universe and how they have played a key role in dissipating the cosmic fog during the epoch of re-ionisation, including the first direct observation of a galaxy ionising the surrounding inter-galactic medium.
With numerical simulations, Dr Matthee found new interesting relations between the growth of galaxies and their alpha-enhancement, which future observations will test, and he was able to shed unique light in the so-called 'galaxy main-sequence'.
The PhD thesis of Jorryt Matthee was conducted at Leiden University, under the supervision of Profs. Huub Röttgering, Joop Schaye, and Dr David Sobral.
for her leadership and creative work in instrumentation, from the conceptual design and the feasibility study to the final integration and verification, both in the laboratory and at the telescope, related to the instrument PANIC.
Dr M. Concepción Cárdenas graduated in Physics at the University of Granada and began working in 1999 at the Institute of Astrophysics of Andalusia (IAA-CSIC, Spain) in the Instrumental and Technological Development Unit, as optical engineer until 2016. Always interested in getting a PhD, she conducted a master degree, simultaneously to her job between 2001 and 2003. As part of the IAA team for the development of new instrumentation for Calar Alto Observatory, she was appointed as the responsible of the optical package of PANIC in 2006 and of the infrared channel of the spectrograph CARMENES, in 2011. While developing PANIC, she restarted her PhD activities simultaneously to her job at IAA, and defended her thesis in December 2018. She was awarded the prize for the best Spanish PhD in Instrumentation, Computing and Technological Development in Astronomy and Astrophysics from the Spanish Astronomical Society. She moved in early 2016 to the Max-Plack Institut für Astronomie (Germany) as Senior Optical Engineer with responsibilities on several instruments for the European Extremely Large Telescope.
Dr Concepción Cárdenas described in her thesis the complete development of an astronomical instrument, PANIC (Panoramic Near-Infrared Camera), from the conceptual design and the feasibility study to the final integration and verification, either in the laboratory as well as at the telescopes, following all the standard processes and exhaustive design revisions. Her thesis can be considered as a very good text book for students in the instrumental fields due to the rigor in the methodology, the achievement of all specifications and goals, with a scrupulous verification.
Her thesis work on PANIC was carried out in parallel with all the activities required to the optical team at IAA, to the CARMENES project (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Echelle Spectrographs), and with fulfilling her daily charges for an Optical Laboratory and the Observatory of Sierra Nevada.
The PhD thesis of M. Concepción Cárdenas Vázquez was conducted at IAA-CSIC under the supervision of Dr Julio F. Rodríguez Gómez and presented at the Univ. of Granada.
for pioneering contributions to exoplanetary science, particularly in advancing the frontiers of atmospheric characterisation of exoplanets.
Nikku Madhusudhan is a Reader in Astrophysics and Exoplanetary Science at the Institute of Astronomy of the University of Cambridge. He pursued his undergraduate studies in Engineering at the Indian Institute of Technology, Banaras Hindu University, India. He moved to the Massachusetts Institute of Technology (MIT) where he obtained a master degree in engineering in 2004 and a PhD in Physics (astrophysics) in 2009. He then pursued postdoctoral research at MIT (2009-2010), Princeton University (2010-2011), and Yale University (2012-2013) where he was the Yale Center for Astronomy and Astrophysics Prize Postdoctoral Fellow. In October 2013, he joined the University of Cambridge as Lecturer, and was promoted in 2017 to Reader. He was awarded the prestigious Bappu Gold Medal in Astrophysics for 2014 by the Astronomical Society of India and the 2016 Young Scientist Medal of the International Union of Pure and Applied Physics Commission on Astrophysics. His research interests span a wide range of theoretical topics in exoplanetary science, including exoplanetary atmospheres, interiors, and planetary formation.
Nikku Madhusudhan has made pioneering contributions to exoplanetary science which include precise chemical characterization of exoplanetary atmospheres, detailed studies of atmospheric and interior processes, and using exoplanetary compositions as tracers of their formation mechanisms. His work has led to several new insights into exoplanetary atmospheres, including constraints on non-equilibrium chemistry, temperature inversions, molecular abundances, and C/O ratios. His recent studies have led to major advances in exoplanetary science in three frontier areas: (1) high-precision chemical characterisation of exoplanetary atmospheres using state-of-the-art observations, (2) detailed constraints on exoplanetary atmospheric processes, and (3) new approaches to constrain exoplanetary formation and migration pathways using their atmospheric abundances.
The pioneering work by Nikku Madhusudhan in the last five years (2014-2018) was conducted at the University of Cambridge, United Kingdom. Prior to 2014, his seminal research was carried out in the USA.
for investigations of the Transient Radio Sky and the discovery of the second Lorimer burst, now known as Fast Radio Bursts.
Evan Keane did his undergraduate studies at the National University of Ireland, Galway, before undertaking a Masters as a scholarship student at Trinity College at the University of Cambridge. He then did his PhD at the Jodrell Bank Centre for Astrophysics in the University of Manchester. His thesis won the Springer Thesis Prize. He then worked as a postdoctoral researcher at the Max Planck Institut für Radioastronomie in Bonn and later as Senior Postdoctoral Fellow and Dynamic Theme Scientist for CAASTRO (Australian Research Council?s Centre of Excellence for All-Sky Astrophysics) at the Swinburne University of Technology. Since 2015 he is Project Scientist for the SKA Organisation. His research focuses on searching for radio transients and using them to understand fundamental questions of physics. He has discovered numerous pulsars and rotating radio transients and in 2011 discovered the second "Lorimer burst", events now known as "fast radio bursts" (FRBs). His current role involves ensuring the SKA will achieve all its scientific objectives in transient, pulsar, VLBI, solar and cosmic ray science.
Evan Keane has made significant contributions to developing and improving techniques to discover new pulsars, and determined timing solutions for challenging pulsars. He was part of the team that discovered the first Galactic Centre radio pulsar. Evan did the first systematic analysis of all known fast radio bursts, precipitating the Fast Radio Burst Catalogue (FRBCAT). Evan leads the Survey for Pulsars and Extragalactic Radio Bursts (SUPERB) project, a large-scale real-time accelerated pulsar and fast transient search programme with the Parkes telescope in Australia.
Evan Keane led the main SKA science case chapter for pulsars, describing the pulsar search yield, optimal search strategies and the science questions that can be addressed by the SKA, such as tests of General Relativity and alternative theories of gravity, gravitational wave astronomy with pulsar timing arrays and physics at super-nuclear density within neutron star interiors using pulsar timing.
This work has been conducted at the Square Kilometer Array Organisation, United Kingdom, and at the Max Planck Institut für Radioastronomie, Germany and Swinburne University of Technology, Australia.
for pioneering contributions to understanding the role of neutrinos in astronomy and astrophysics.
Irene Tamborra completed her (under-) graduate studies in Physics, all Cum Laude, at the University of Bari in 2011. Her PhD thesis focused on neutrinos in astrophysics and cosmology. She then won a prestigious Alexander von Humboldt Fellowship at the Max Planck Institute for Physics. She continued to work on neutrino flavour conversions in dense media while expanding towards astrophysics. In 2013, Irene joined the GRavitational AstroParticle Physics Amsterdam (GRAPPA) Center of Excellence at the University of Amsterdam. Close interactions with the astronomers guided her on the modelling of the microphysics of cosmic accelerators through multi-wavelength data. In 2016, Irene joined the Niels Bohr Institute in Copenhagen as Knud Højgaard Assistant Professor and won a Villum Young Investigator Grant. In 2017, Irene was promoted Associate Professor and awarded a career-development grant from the University of Copenhagen. More recently, she has received a competitive Sapere Aude grant from the Danish Council for Independent Research and a Distinguished Associate Professor Fellowship from the Carlsberg Foundation. She is also Mercator Fellow for the Collaborative Research Centre 1258 at the Max Planck Institutes for Physics and Astrophysics.
Irene Tamborra has made pioneering work in advancing our understanding of the role of neutrinos in extreme astrophysical sources. Among many examples, she has discovered the LESA instability, the first hydrodynamical instability occurring in core-collapse supernovae completely driven by neutrinos. She has proposed innovative ideas concerning the exploration of astrophysical transients by using neutrinos as probes, and has demonstrated a highly original research approach connecting the theoretical modelling of the microphysics of astrophysical transients to observations. This led to unravel fundamental properties of neutrinos in dense matter, to unveil the impact of neutrinos on the production of the heavy elements and the dynamics of transient astrophysical sources, as well as to highlight the promising approach of using neutrinos as probes of the inner working of extreme astrophysical sources.
The work of Irene Tamborra has been conducted at the Niels Bohr Institute, University of Copenhagen, Denmark, at Max Planck Institutes for Physics and Astrophysics, Germany, at GRAPPA, Center of Excellence of the University of Amsterdam, The Netherlands, and at the Department of Physics, University of Bari, Italy.
for the study of the imprint of the large-scale structure of the Universe on galaxy formation and cosmology.
Sandrine Codis graduated from the Ecole Normale Supérieure (Paris) in Mathematics and Theoretical Physics. She obtained her PhD at the Institut d'Astrophysique de Paris (IAP) from September 2011 to September 2015. She then became a CITA post-doctoral fellow in Toronto. She is now a CNRS permanent researcher at IAP, France. Sandrine Codis works on the theoretical modelling of the large-scale structure of the Universe and is particularly interested in cosmology, weak lensing, cosmic web and galaxy formation. She is also a member of the Euclid consortium, an ESA's space mission dedicated to mapping Dark Matter in the Universe and characterising the equation of state of the Dark Energy, potentially responsible for the acceleration of the expansion of the Universe.
Sandrine Codis' PhD thesis focused on the theoretical understanding and modelling of the large-cale structure of the Universe. She was particularly interested in addressing some of the challenges that the field of large-scale structure studies needs to overcome to extract the marrow of the gigantic precision datasets that will be produced by future galaxy surveys like ESA's cornerstone Euclid mission and LSST. She successfully developed innovative tools to probe (from first principles) the non-linear regime of structure formation and tackle systematic effects such as redshift space distortion and intrinsic alignment of galaxies which compromise high precision large-scale structure measurements. For that purpose, she developed new mathematical models and was involved in the post-processing and scientific analysis of massive N-body and hydrodynamical simulations. Her publications are already references in the field and span a wide range of topics from cosmology to galaxy formation. The quality of her thesis was recently honoured as the best PhD in astronomy by the Société Française d'Astronomie et d'Astrophysique.
The PhD thesis of Sandrine Codis was conducted at the Institut d'Astrophysique de Paris (IAP), with a degree delivered by the Université Pierre et Marie Curie - Paris VI, under the supervision of Christophe Pichon (IAP) and Dmitri Pogosyan (University of Alberta).
for the observational characterisation of the physical properties of the galaxies that formed in the first billion years of cosmic time.
Renske Smit earned her undergraduate and PhD degrees at Leiden University in the Netherlands. During her master thesis she secured a scholarship to pursue part of her degree at the University of California, Berkeley. For her PhD she conducted research into the formation and evolution of the first galaxies using cutting-edge observational facilities. She then began her postdoctoral career at the Centre for Extragalactic Astronomy at Durham University. In 2016 she was awarded a Rubicon grant by the Netherlands Organisation for Scientific Research (NWO) based on her thesis work. She is currently working as an independent research fellow at the Kavli Institute for Cosmology at the University of Cambridge, UK.
Renske Smit's doctoral research focused on the study of very distant galaxies, seen in the first few billion years of cosmic history, using the Hubble and Spitzer Space Telescopes. Her studies were among the first to obtain genuine insight into the physical conditions of these galaxies, paving the way for detailed follow-up studies with ground-based instrumentation. Her research established that emission lines associated with the formation of massive, young stars often dominate the broadband flux of distant galaxies. This work resolved a major discord between observations and theoretical models of the evolution of galaxies in the early Universe. Renske Smit's innovative work also enabled her to identify new galaxies in the Epoch of Reionisation; spectroscopic follow-up of these sources with the Atacama Large Millimeter Array allowed her to obtain the first measurement of velocity structure in galaxies at this early epoch. She participated in efforts to detect even more distant (z≈8-9) galaxies, spectroscopic follow-up of which yielded spectacular confirmation of their redshifts via the Lyman- alpha emission line, breaking two consecutive records for the most-distant galaxy known to science. As a member of the NIRSpec Guaranteed Time Observations (GTO) Galaxy Assembly team, Renske Smit is now preparing for the forthcoming revolution promised by the launch of the James Webb Space Telescope.
The PhD thesis of Renske Smit was conducted at the University of Leiden, under the supervision of Dr. Rychard Bouwens.
for a PhD thesis on cutting-edge concepts of compact polychromatic spectropolarimeters adapted to astrophysical space mission requirements in the UV domain.
Martin Pertenais has obtained an optical engineer degree from the prestigious Engineer School Institut d'Optique Graduate School (IOGS) in Paris and a Master in photonics from the University of Jena. He then undertook a PhD thesis in instrumentation for astrophysics at the Institut de Recherche en Astrophysique et Planétologie in Toulouse and at the Paris Observatory on "Stellar UV and Visible spectropolarimetry from space". This allowed him in particular to successfully lead the Arago Payload consortium and to innovate in new technologies for spectropolarimetry. After his PhD thesis, he moved on a position at DLR as the Optical System Engineer for PLATO. In parallel, he keeps working on new spectropolarimeter designs and co-supervises a PhD student on this topic for the NASA mission LUVOIR.
The goal of Martin Pertenais' PhD thesis was to find innovative concepts of spectropolarimeters, to build the first ever space mission equipped with a high-resolution spectropolarimeter working on a wide wavelength range including the UV domain. In Toulouse, he performed theoretical calculations and simulations for two different original concepts of polarimeters that he formulated. The first one is an inventive static polarimeter using birefringent wedges as polarisation spatial modulator. The second concept used a classical rotating polarimeter, albeit optimised to get constant efficiencies for the extraction of the Stokes parameters from 123 to 888 nm. The result is an ingenious very compact polarimeter working with the same polarimetric efficiency over a very large spectral range, including the UV. While in Paris Martin Pertenais created prototypes of both concepts to demonstrate experimentally his very encouraging theoretical results. He built and tested both prototypes, which showed excellent experimental results, increasing the Technology Readiness Level for these innovative technologies. Martin Pertenais also tested one of the two prototypes on the sky on real stars. In October 2015 he received the "Young Researcher Award" granted by the French CNES agency. Martin Pertenais was an essential member of the core team of the Arago international space mission project, a M4 and M5 ESA candidate mission.
The PhD thesis of Martin Pertenais was conducted at the Institut de Recherche en Astrophysique et Planétologie in Toulouse and at the Paris Observatory in Meudon, with a degree delivered by the Université Toulouse 3 Paul Sabatier, under the supervision of Coralie Neiner and Pascal Petit.
Group picture taken at EWASS 2018 in Liverpool, United Kingdom. The laureates are surrounded by Georges Meylan (left) and George Lake (right). Credit: Marc Audard (EAS)
for her major contributions to our understanding of the role of binarity as one of the dominant physical parameters for massive stars.
Selma de Mink completed her graduate studies in physics and math all Cum Laude at Utrecht University in the Netherlands. She continued with a PhD in theoretical astrophysics completed in 2010. She was then awarded the prestigious NASA Hubble fellowship, which she used to start her independent line of research at the Space Telescope Science Institute and Johns Hopkins University in Baltimore, Maryland. In 2013 she was awarded numerous fellowships and she chose to combine NASA's Einstein fellowship with the Princeton Lyman Spitzer fellowship, allowing her to spend her time between Carnegie Observatories, the TAPIR institute for theoretical astrophysics and relativity at the California Institute of Technology and Princeton University. In 2014 she returned to Europe to start to build her own research group as a MacGillavry assistant professor at the University of Amsterdam. Since then she was awarded a Marie Curie Fellowship (2015) and an ERC starting grant (2016).
Selma de Mink made a very large impact across different sub-disciplines in astrophysics by pushing our understanding of the role that binarity and rotation play in the complicated lives of massive stars. Her work has been absolutely crucial in changing the long held "single star paradigm" for massive stars. Although it was known before that massive binaries are common and give rise to various exciting phenomena, she and her collaborators showed that this property is necessary for a complete explanation of the main-sequence properties of massive stars, their diverse explosion channels and their various compact object remnants. Her theoretical work had large impact on the debate about the origin of merging binary black holes, as recently detected by the LIGO gravitational wave detector. Her early detailed simulations allowed her to explore new theories for the evolution of very close compact binary systems where the stars experience internal mixing processes. Selma de Mink is also recognised for her refreshing ideas challenging long-held beliefs, in particular on the possible role of massive binaries in explaining multiple populations in globular clusters.
The work of Selma de Mink has been conducted at the Anton Pannekoek Institute for Astronomy at the University of Amsterdam, The Netherlands, at the Carnegie Observatories and California Institute of Technology, Pasadena, USA, at the Space Telescope Science Institute and Johns Hopkins University, Baltimore, USA, at the Argelander Institut in Bonn, Germany, and at the Utrecht University, The Netherlands.
for his groundbreaking work on the galaxy/black hole connection and innovative use of citizen science in astrophysics.
Kevin Schawinski was a graduate student at Oxford University from 2004-2008 during which time he co-founded the Galaxy Zoo citizen science project. For his thesis on the role of black holes in the quenching of star formation in early-type galaxies, Kevin received the Royal Astronomical Society's Michael Penston prize for the best thesis in astronomy in the UK. He remained in Oxford for several months as the Henry Skynner Junior Research Fellow at Balliol College, Oxford before moving to Prof. C. Megan Urry's group at Yale University. He was awarded a NASA Einstein Fellowship and remained at Yale until 2012, working with the latest deep field observations from the Hubble, XMM-Newton and Chandra space telescopes. He moved to ETH Zurich in Switzerland as an Assistant Professor with a Swiss National Fund professorship grant where he now leads the black hole astrophysics group. He is strongly engaged in citizen science, recruiting large numbers of people from the general public to engage with science.
Kevin Schawinski has made major advances in the observational understanding of the feedback exerted on a galaxy by outflows from an active, super-massive back hole at its centre. He also used stellar evolution to build phenomenological models of galaxy evolution. Using stars as "cosmic clocks", he constrained the phases in the evolution of galaxies during which their central black holes become active as quasars. He showed using observations that while many disk galaxies – like our Milky Way – cease their star formation activity very slowly over billions of years, some galaxies whose morphology was transformed by a major galaxy merger to an elliptical shape shut down their star formation very quickly. The most plausible cause for this sudden end of star formation is that a very brief active phase by the black hole destroys the gas reservoir used as fuel for star formation. As a co-founder of the Galaxy Zoo project he involved several hundred thousand citizen scientists to classify nearly a million galaxies from the Sloan Digital Sky Survey. The discovery of the famous "Hanny's Voorwerp" by a Dutch school teacher taking part in Galaxy Zoo became a prototypical system for quasar ionisation echoes tracing the past energetic output of central black holes. Kevin Schawinski showed that such echoes limit the duration of a typical quasar phase to only a few hundred thousand years.
The work of Kevin Schawinski has been conducted at Oxford University in the United Kingdom (2004-2008), Yale University (2008-2012) and ETH Zurich in Switzerland (2012-2016).
for his unique and pioneering work on innovative astronomical instrumentation, based on active systems, freeform optics and curved focal planes.
Emmanuel Hugot is a French astrophysicist, expert in innovative instrumentation and, since 2015, leader of the Research and Development Group at the Laboratoire d'Astrophysique de Marseille (LAM). In 2004, he completed his Master Thesis on "Optics, Image and Signal" at the Aix Marseille University (AMU) and started a PhD Thesis completed in 2007 at the LAM. He has been awarded the young researcher prize of the French Society of Astronomy and Astrophysics in 2014, and received in 2017 the CNRS bronze medal delivered to early career scientists. He defended his accreditation Thesis at AMU in 2016. Besides his management activities with the science team at LAM, he is now leading an ERC-funded programme to enable compact, high-quality and affordable instrumentation for the future giant observatories, based on the revolutionary combination of freeform optics and curved detectors.
Emmanuel Hugot's interests in instrumentation are broad, from the manufacturing of super-polished freeform optics for cutting-edge instrumentation, to the development of a new type of focal planes using variable curvature detectors, thus leading to compact and cost-effective instrumentation, crucial for the E-ELT or the post-JWST generation such as the LUVOIR observatory currently under study at NASA. Over the past ten years, he has been leading cutting-edge R&D projects for high angular resolution and high contrast imaging, based on the synergies between active and adaptive optics, materials science and innovative focal plane architectures. His work has also a multi-disciplinary impact, as it involves imaging science with applications in many fields, from bio-medical science to artistic projects. One of his main achievement is the concept and building of the first active mirror ever used in an extreme adaptive optics system. Installed in 2015 on the Spectro-Polarimetric High-Contrast Exoplanet REsearch (SPHERE) instrument of ESO's Very Large Telescope (VLT), this system demonstrates the gain of smart flexible optics for sharp and accurate astronomical observations and triggered worldwide interest on this technique.
The work of Emmanuel Hugot has been conducted entirely at the Laboratoire d'Astrophysique de Marseille, a world-leading lab in the field of astronomical instrumentation, but with international and industrial collaborations, clearly enhancing the impact of his activities.
Group picture taken at EWASS 2017 in Prague, Czech Republic marking the 5-year jubilee of the MERAC Prizes. The laureates are surrounded by George Lake (far left), Jean-Marie Louzier (left), and Carl Stadelhofer (right) all from the FONDATION MERAC, together with the EAS President, Thierry Courvoisier (far right).
for her thesis on radiative instabilities and particle acceleration in high-energy plasmas with applications to relativistic jets of active galactic nuclei and gamma-ray bursts.
Maria Petropoulou received her Bachelor Degree in Physics (2008), Master Diploma in Astrophysics (2010) as well as her PhD Degree in Physics (2013) from the National and Kapodistrian University of Athens, Greece. Her PhD project was funded by a co-financed European-Greek Grant (HERACLEITUS II). She has been awarded the "Best PhD Thesis Prize 2015" from the Hellenic Astronomical Society. Just before her PhD Thesis defence, she has been awarded the NASA Einstein Fellowship for Post Doctoral research (2013-2016) on the subject of "High energy radiation, neutrino and cosmic ray production from relativistic outflows". She has published 20 articles in refereed journals, which reflect her research interests in emission processes and neutrino production from active galactic nuclei and gamma-ray bursts. She is now a Post Doctoral Einstein Fellow at Purdue University, West Lafayette, USA.
Maria Petropoulou's PhD thesis has a main focus on the theoretical study of plasma properties in compact energetic sources such as Active Galactic Nuclei (AGNs) and Gamma Ray Bursts (GRBs). Such extremely luminous sources in remote galaxies emit gamma-rays originating in a relativistic jet powered by a black hole. While most studies consider only the electrons in the jet and neglect the influence of the protons, Maria Petropoulou developed equations for a full treatment of plasmas containing magnetic field, relativistic protons and electrons, and photons. She then solved these equations via both numerical and analytical methods to describe the radiative instabilities in the ejected plasmas, which exhibit a rich temporal behaviour of prey-predator type. As a final step, she confronted her model to observations of the archetypical gamma-ray emitting blazar 3C 279. A theoretical study of the spectral and timing emission of GRB afterglows complements her PhD work.
The PhD thesis of Maria Petropoulou was entirely conducted at the University of Athens, Greece, under the supervision of Prof. Apostolos Mastichiadis.
for his thesis on the simplicity of the evolving galaxy population and the origin of the Schechter form of the galaxy stellar mass function.
Yingjie Peng is born in the Sichuan province in the southwest of China, near Tibet. Being ranked first in his city in the national evaluation, he was admitted by Beijing Normal University to study astrophysics as an undergraduate student. During this study, he spent one year in Tokyo Gakugei University in Japan to study Japanese history and culture. From 2005 to 2007, he was awarded the prestigious Erasmus Mundus Fellowship from European Commission to join the double-master degree program, studying Space Technology at Julius Maximilian University of Würzburg in Germany, Luleå University of Technology in Sweden, and astrophysics at the university Paul Sabatier Toulouse III in France. Then he joined the PhD program in observational cosmology at ETH Zurich in 2007 under the supervision of Prof. Simon Lilly, and obtained his PhD in 2013. He was awarded the ETH Medal for his outstanding PhD Thesis. He then moved to the UK as a research associate at Cavendish Laboratory, University of Cambridge and was awarded the prestigious Royal Astronomical Society Research Fellowship in 2015 for his high-impact research in observational cosmology. In October 2015, he moved from Cambridge to Beijing, China, joining the Kavli Institute for Astronomy and Astrophysics at Peking University, as a tenure-track Assistant Professor.
Yingjie Peng's PhD thesis focused on the analysis of high quality data from large sky surveys both locally and at high redshift, and introduced a novel phenomenological, observationally-based approach to study the formation and evolution of the galaxy population. The goal was to use the observational material as directly as possible in order to identify the simplest empirical "laws" for the evolution of the population. This approach has successfully explained the origin of the Schechter form of the stellar mass function and reproduced many observed essential features of the evolving galaxy population over cosmic time. The associated papers (Peng et al. 2010 & 2012) describing this simple and innovative approach have become some of the most highly cited papers in galaxy formation and evolution.
The PhD thesis of Yingjie Peng was carried out at the Institute for Astronomy at ETH Zurich, Switzerland between October 2007 and September 2012, under the supervision of Prof. Simon Lilly.
for his thesis on an innovative design of two subsystems for the VLTI instrument GRAVITY: the fibre coupler and the guiding system.
Oliver Pfuhl studied at the Technical University Munich and joined the Max- Planck-Institute for extraterrestrial physics (MPE) for his Diploma Thesis. He worked on optimizing the performance of the Very Large Telescope Interferometer (VLTI) instrument PRIMA. He then completed his PhD at MPE and the Ludwig Maximillian University under the supervision of Prof. Reinhard Genzel and Dr. Frank Eisenhauer. For his dissertation, "The GRAVITY Interferometer and the Milky Way's Nuclear Star Cluster", Oliver designed and built two key subsystems, the fiber coupler and the guiding system, for the second generation VLTI instrument GRAVITY. He also constrained the star formation history of the stellar cluster around the massive black hole in the Milky Way using an integral field spectroscopic sample of stars. He was awarded the Universe PhD Award for the best experimental dissertation by the Excellence Cluster for Astronomy in the Munich area. After his PhD in July 2012, Oliver Pfuhl took a postdoctoral position at MPE. He is currently seconded to ESO Chile for one year to ensure that GRAVITY is successfully commissioned at the VLTI.
Oliver Pfuhl started his PhD in 2008 on the GRAVITY project and contributed to the overall design of this new VLTI instrument. He developed two key-components, the fibre coupler and the guiding system, which are key for enabling waveguide based stellar interferometry and for achieving the required astrometric accuracy and stability. The fibre coupler he designed is unique for its compactness, elegance, and innovative use of modern technology. The unit offers all the functions necessary for precision control of the optical path, including tip/tilt-, pupil-, and piston control, field de-rotation, and polarisation control. He also made an innovative design for the guiding system, which actively corrects for tilt- and pupil errors resulting from numerous reflections over 100m of optical path between the telescopes and the instrument. The astrophysical part of Oliver Pfuhl's thesis is a spectroscopic study of more than 500 stars in the nuclear star cluster at the Galactic centre, which shows that this cluster formed most of its stars more than 5 billion years ago.
The PhD thesis of Oliver Pfuhl was carried out under the Supervision of Prof. Reinhard Genzel and Dr. Frank Eisenhauer at the Max-Planck-Institute for extraterrestrial Physics, Garching, Germany, and the Ludwig-Maximilian University, Munich, Germany.
Group picture taken at EWASS 2016 in Athens, Greece. The MERAC prize laureates are surrounded by Georges Meylan, chair of the prize committee (left) and George Lake representing the FONDATION MERAC (right).
for her theoretical and computational contributions to the dynamics of star clusters and galaxies, the reionization epoch, the Galactic centre, and the formation of massive stellar black holes.
Michela Mapelli studied Physics at the University of Milano Bicocca (1998-2002), where she received her Master degree in February 2003, with a Thesis on 'Four-body interactions in globular clusters'. In October 2006, she received her PhD at SISSA, with a Thesis on 'Relic signatures of reionization sources', for which she was awarded both the Gratton Prize 2007 and the Tacchini prize 2007. In 2007, she became postdoctoral fellow at the Institute for Theoretical Physics of the University of Zurich, Switzerland, where she studied the formation of giant low-surface brightness galaxies. She was awarded there the prestigious 'Forschungskredit' fellowship in 2008 before receiving an independent postdoctoral fellowship at the University of Milano Bicocca in 2009. In August 2011, she started a permanent research position at INAF - Padova Astronomical Observatory, where she created her independent research team.
Michela Mapelli's main scientific achievements of the last five years are her studies on the formation of massive stellar black holes from the collapse of metal-poor stars and her contribution to understanding star formation in the Galactic centre. In 2009, she proposed that black holes of more than 20 and up to 80 solar masses can form in the local universe from the direct collapse of metal-poor stars. This can explain why ultra-luminous X-ray sources (ULXs) occur more frequently in galaxies of low-metallicity, with considerable implications for high-energy astrophysics and the search of gravitational waves. In 2012, she simulated the disruption of a molecular cloud by the tidal shear of the super-massive black hole in the Galactic centre and showed that a gaseous disc forms and then fragments into proto-stellar clumps, thus explaining the presence of young, massive stars at the centre of our Galaxy.
The work of Michela Mapelli has been conducted entirely in Europe. After graduating in 2006 at SISSA (Trieste), she developed the model of massive stellar black holes during the post-doctoral fellowship at the University of Zurich, Switzerland, and then at the University of Milano Bicocca, Milan, Italy (2009-2011). Since 2011 she is Researcher at INAF - Padova Astronomical Observatory, Italy, where she has continued investigating massive stellar black holes, and started working on the Galactic centre.
for her ground-breaking contributions to the understanding of the internal structure of red-giant stars based on stellar oscillations measured by the CoRoT and Kepler satellites.
After receiving her PhD from the University of Leiden in the Netherlands in Sept. 2007, Saskia Hekker worked at the Royal Observatory of Belgium and the University of Birmingham. In 2011 she was awarded a personal 3-year Veni Fellowship from the Netherlands Organization for Scientific Research to conduct research at the Astronomical Institute 'Anton Pannekoek', University of Amsterdam. Since September 2013, she works in Göttingen at the Max Planck Institute for Solar System Research (MPS). In 2013 she obtained a European Research Council (ERC) Starting Grant to determine Stellar Ages through asteroseismology. In 2014, she was awarded a Max Planck Independent Research Group focusing on 'Asteroseismology and Galactic Evolution', which is an international node of the 'Stellar Astrophysics Centre', a Centre of excellence in research of the Sun, Stars and Extra-solar planets. Her career path and mobility is outstanding, particularly since Saskia is also a mother.
Saskia Hekker announced, already during her PhD, non-expected, non-radial oscillations in red-giant stars which she then confirmed using data of the CoRoT satellite. She was also heavily involved in the discovery, identification, and analysis of mixed oscillation modes, which allow to probe the core region of the stars, in particular to disentangle hydrogen-shell- from helium-core- burning red giants. She discovered the first red giant in an eclipsing binary and developed methods to determine global asteroseismic parameters, which she then applied to Kepler data of planet-hosting stars.
Saskia Hekker performed her work at the School of Physics and Astronomy, University of Birmingham, United Kingdom (2009-2011); Astronomical Institute 'Anton Pannekoek', University of Amsterdam, the Netherlands (2011-2013) and the Max Planck Institute for Solar System Research, Göttingen, Germany (2013-present).
for his development of pupil masking and pupil remapping observing techniques, which provide a unique combination of high contrast and high angular resolution to study the immediate environment of stars.
After his graduation from Ecole Normale Supérieure in electrical engineering, Sylvestre Lacour worked at The Johns Hopkins University from 2000 to 2002 as software engineer for the FUSE satellite. He pursued with a PhD in astrophysics on a project combining pupil remapping and long- baseline optical interferometry. It consisted partly in building a single- mode pupil remapping prototype instrument (FIRST), and partly in acquiring and interpreting observations from the IOTA interferometric array (Mount Hopkins, Arizona). After the successful defence of his PhD in 2007, he obtained a Lavoisier fellowship to pursue his research in high angular resolution instrumentation at the University of Sydney. He developed there a strong expertise in the emerging technique of pupil masking. Over the last years, he benefits from a CNRS tenured position at the Observatory of Paris, allowing him to work on the application of the pupil masking technique to the study of young stellar objects. As an expert in high precision astrometry, he is also deeply involved in the GRAVITY instrument for the VLT Interferometer.
Sylvestre Lacour is the leading European specialist in the pupil masking and pupil remapping observing techniques. These two techniques provide a unique combination of high contrast and high angular resolution that is key to studying the immediate environment of stars in all evolutionary stages. He also developed a complete pipeline to reduce this kind of observations, which are now performed by major astronomical facilities. This effort lead to an important result on scattering dust around evolved stars and opened a new observational window on the inner structure of transition disks, where extrasolar planets are expected to form.
Sylvestre Lacour started working in the field of interferometry since his PhD at the Observatoire de Paris. He then fully developed the field aperture masking during the Lavoisier Fellowship at Sydney University and a second post-doctoral position at the Observatoire de Grenoble. Since 2009 he is affiliated with the Observatoire de Paris, France.
Group picture of the three MERAC Prize laureates taken at EWASS 2015 in Tenerife, Spain.
for her thesis on the treatment of star formation and feedback in simulations of galaxy formation.
Claudia Lagos is a Chilean who gained an undergraduate degree in 2007, followed by a Master's in 2009, both at Universidad Católica de Chile. With three publications at the end of her master's, Lagos was awarded a prestigious studentship jointly funded by the Science and Technology Facilities Council and the Gemini Observatory to carry out a PhD at Durham University. Lagos completed her PhD at the Institute for Computational Cosmology in November 2012. She was awarded the Department of Physics Keith Nicholas Prize for Outstanding Academic Achievement and a Springer Thesis Prize, awarded to the three best thesis in all physics each year. She recently took up a highly competitive fellowship at the European Southern Observatory in Germany. She continues to play a leading role in the development of state-of-the-art models of galaxy formation.
Claudia Lagos' PhD thesis focused on the galaxy formation model, GALFORM, which can implement essentially all existing theoretical models of star formation. Her work overhauls the two key processes at the centre of how galaxies are made: the formation of stars and the regulation of star formation following the injection of energy into the interstellar medium. These calculations represent the first real advances in these areas in over a decade. Lagos' work allows the physical predictions of the galaxy formation model, such as the content of the interstellar medium, to be confronted directly by observations from new major telescopes, such as the Atacama Large Millimetre Array (ALMA).
The PhD thesis of Claudia Lagos was carried out at the Institute for Computational Cosmology at Durham University (UK) between October 2009 and September 2012, under the supervision of Prof. Carlton Baugh and Dr. Cedric Lacey.
for his thesis on the discovery and characterisation of many new exoplanetary systems.
Amaury Triaud is currently doing a postdoctoral fellowship supported by the Swiss National Science Foundation, at the Massachusetts Institute of Technology, in the USA. His path is an example of contemporary youth in Europe: born and schooled in France, he then decided to pursue his undergraduate studies at the University of St Andrews in Scotland graduating in 2007 with a Masters of Physics. His summers were spent in France (2003 & 2004), Germany (2005) and Switzerland (2006) doing research internships that nurtured his scientific career and produced his first papers. He moved to Geneva in 2007 for a four-year PhD program that was completed in August 2011. The number, variety and citation rate of his publications are a testimony of his achievements during and since his thesis. He also applied his skills to the service of multiple outreach activities to bring science to the wide public.
Amaury Triaud conducted the radial velocity confirmation of transiting exoplanet candidates produced by the Wide Angle Search for Planets (WASP). This led to the confirmation of 48 new nearby exoplanetary systems, which are prime targets for characterisation. Triaud chose to focus on measuring the angle between the star's rotation axis and the planet's orbit. Multiple observations using ESO's HARPS spectrograph unveiled the earliest evidence for planets on retrograde orbits and found that a large fraction of hot Jupiters do not occupy orbits coplanar with their star. Those results shacked widely held believes about planet formation and migration scenarios and triggered a flurry of theoretical papers and additional observations.
The PhD thesis of Amaury Triaud was carried out at the Observatory of the University of Geneva (Switzerland) between August 2007 and August 2011, under the supervision of Prof. Didier Queloz.
for his thesis on detector technologies for sub-millimetre wave astronomy.
Boon Kok Tan was born in a small town (Taiping) in Malaysia. At the age of 17, he was selected to become already an undergraduate student at the University of Technology Malaysia, due to his exceptional school performance. After completing the Bachelor degree in Electrical and Electronic Engineering in 2001, he was offered a postgraduate position in Solar Engineering, and was awarded the Master degree in 2002. Following a lecturing career at Tunku Abdul Rahman University in Kuala Lumpur, he was offered a D. Phil position – funded by the prestigious King of Malaysia awards – at Oxford Astrophysics to work on the development of quantum limited coherent detectors for submillimetre astronomy. B. K. Tan obtained the D. Phil degree at Oxford in 2012. He is currently a member the Millimetre Detectors group of Oxford Astrophysics, leading the development of coherent THz detectors for the Atacama Large Millimetre Array (ALMA) and collaborates also with the Wawasan Open University, Malaysia.
Boon Kok Tan's thesis describes the development of receiver technologies for sub-millimetre astronomy instruments, focusing on high performance coherent cryogenic detectors operating close to the superconductor gap frequency. The mixer receiver developed in his thesis work contributed novel ideas in all three major parts of Superconductor-Insulator-Superconductor (SIS) mixers. These novel detector systems pave the way into high performance THz mixers, which will have a strong impact on sub-millimetre wave astronomy.
The PhD thesis of Boon Kok Tan was carried out at the Department of Physics and Astrophysics of the University of Oxford between October 2007 and June 2012, under the supervision of Dr. Ghassan Yassin.
Group picture taken at EWASS 2014 in Geneva, Switzerland. The MERAC prize laureates are surrounded by Francesco Palla, chair of the prize committee (left), Thierry Courvoisier (EAS President) and George Lake representing the FONDATION MERAC (right).
for her work on the theoretical modeling of galaxy formation and evolution.
Gabriella De Lucia obtained a PhD in theoretical astrophysics at the Max-Planck Institute for Astrophysics (MPA, Garching, Germany) in 2004. In the same year, she was offered a 3-year (later extended to 5 years) postdoctoral position at MPA. In 2008, she was awarded a Starting Independent Researcher Grant from the European Research Council to set up a small research group at the Astronomical Observatory of Trieste, where she moved as a Senior Researcher in 2009. She is currently Astronomer of the Italian National Institute for Astrophysics at the Astronomical Observatory of Trieste.
Gabriella De Lucia has made key contributions to the connection between theoretical models of structure formation and the observed properties of galaxies at different cosmic epochs. She has explored this connection using several innovative techniques, which have brought important revisions to conventional interpretations of the observed properties of galaxies. The models she has developed have reshaped our understanding of the physical processes that drive galaxy evolution, and in particular, of how these depend on the environment in which galaxies reside.
for the discovery of a very primitive low-mass star in our Galaxy.
After several years of work as professor in secondary schools in Italy, Elisabetta Caffau obtained a PhD in observational astronomy from Paris Observatory in 2009. After a one year post-doctoral position in Paris Observatory, E. Caffau obtained a three year "Gliese fellow grant" at the Zentrum für Astronomie of the University of Heidelberg. E. Caffau has developed a method to obtain high precision abundances of the elements from 3D hydrodynamical computations. With the infrared spectrograph CRIRES at ESO/VLT, she measured the phosphorus abundance of twenty cool stars in the Galactic disk for the first time.
Elisabetta Caffau applied her method to recognize the extremely metal poor stars in the crowd of low-resolution spectra provided by large spectroscopic surveys like the Sloan Digital Sky Survey. Thanks to this very efficient tool, she discovered in 2011 the most primitive star currently known (SDSS J1029+1729) and she defined its chemical composition. The discovery of a star with an extremely low abundance of all the elements from C to Zn, is considered as a key for our understanding of the formation of stars and chemical elements in the early history of the Milky Way.
for his high-impact research in computational astrophysics and cosmology.
Justin Read obtained his PhD in theoretical astrophysics from Cambridge University, UK, in 2003. After a two-year postdoctoral research position, also in Cambridge, he moved to the University of Zürich to join the Institute for Theoretical Physics. In 2009, he joined the University of Leicester as a lecturer in theoretical astrophysics, and in October 2010 he was awarded an assistant professorship at ETH Zürich. Starting 2013 he took up a full Chair at the University of Surrey, Guildford, UK.
The MERAC Prize is awarded for his major achievements in the area of computational astrophysics. He has been able to improve substantially one of the two major computational methods adopted to model hydrodynamics in astrophysics, namely smoothed particle hydrodynamics (SPH). Since numerical simulations have become an essential part of astrophysics and cosmology over the past decade, often driving the interpretation of astronomical data, the impact of his work in the field is of primary importance, and will be even more so in the future. The method developed by Justin Read, called SPH-S, overcomes two related long-standing problems of standard SPH, namely its inability to resolve mixing in fluids and capture instabilities at fluid interfaces.
Group picture taken at EWASS 2013 in Turku, Finland. The MERAC prize laureates are surrounded by Francesco Palla, chair of the prize committee (left), and George Lake representing the FONDATION MERAC (right).
(Mobilising European Research in Astrophysics and Cosmology)
is a non-profit foundation started in 2012 with headquarters in Switzerland
to recognize and support young European astronomers. It is supervised by the Federal Department of Home Affairs FDHA.
There are yearly three MERAC Prizes awarded by the EAS.
The prizes of 25'000 € are for each of the three categories:
New Technologies (Instrumental/Computational/Multi-Messenger).
The prizes alternate by year for:
Best Early Career Researcher Prizes (on odd years),
Best Doctoral Thesis Prizes (on even years).
In addition, the awardees are eligible for further substantial support from the FONDATION MERAC. The FONDATION MERAC will inform the awardees after their selection on their eligibility and procedure to follow to receive the MERAC prize and to apply for further funds.
Nominations should arrive at the EAS Office by the end of October of the year preceding the awards. Nominations can only be made by EAS members and need to be endorsed by 2 additional persons, at least one of them being an EAS member.
The EAS Council invites EAS members to nominate suitable candidates for the
MERAC Prizes of 2024.
This being an even year, the three prizes will be
Best Doctoral Thesis Prizes.
The Prizes will be awarded for the best PhD Theses in Astrophysics
for degrees awarded in the previous 2 years before the call (i.e., from January 2021 onward).
The strict deadline for nomination is:
Tuesday, 31 October 2023 at 23:59:59 CET.
Important information: a proponent cannot self-nominate for a MERAC prize. An EAS member must propose
Nominations are only accepted through a web form accessible on this page for
EAS members upon logging in.
If you are not yet an EAS member, please consider to become a member.