With its 39m primary mirror, the ESO Extremely Large Telescope (E-ELT) will be the largest optical/near-infrared telescope ever built. MOSAIC (Multi-Object Spectrograph for Astrophysics, Inter-galactic medium studies and Cosmology) is expected to become the E-ELTs workhorse instrument for astrophysics, intergalactic medium studies and cosmology in the coming decades. MOSAIC will fully explore the large aperture and superb spatial resolution of the biggest eye on the sky. Key science cases involve searching for extra-galactic planets, resolving stellar populations in thousands of nearby galaxies, and studying high-redshift galaxies at the edge of the visible universe. MOSAIC is a fiber-fed spectrograph, covering the telescopes full field of view with several hundred fibers and a dozen integral field units with adaptive optics capability delivering milli-arcsec spatial resolution, providing spectra ranging from the ultraviolet to the near infrared (380 - 2500 nm) at intermediate spectral resolution. The MOSAIC consortium includes scientists from Brazil, France, The Netherlands, and the United Kingdom, as main partners. Another 6 European countries are associated with the consortium at different levels. The Netherlands will be involved in designing and building the MOSAIC spectrographs; Brazil will contribute to its fiber system and spectrograph slit assembly. This proposal aims to study and develop the fibers to spectrograph interface by producing prototype slit assemblies for MOSAIC, exchanging expertise between Brazilian and Dutch technicians and industry, and to scientifically explore state-of-the-art MOS observations to optimize the scientific and technical requirements for MOSAIC. These activities are not covered by our currently assigned budgets.

The recent direct detections of gravitational waves and multi-messenger discovery of a binary neutron star merger opened new exciting opportunities for probing fundamental physics in unexplored regimes. Key scientific targets in this field are the rich phenomena of neutron star binary systems, whose unique science is imprinted in the gravitational waves generated during their inspiral and merger, as well as the accompanying electromagnetic counterparts. Each messenger conveys complementary information about these violent events, with a joint analysis being essential for tests gravity and cosmology, for probing the microphysics of matter at supra-nuclear densities, and for gaining deeper insights into neutron star and black hole formation. The aim of this project is to jointly analyze information from gravitational waves and electromagnetic counterparts to probe the rich physics of neutron stars. Neutron stars contain matter compressed by gravity to up to several times the density of an atomic nucleus and represent exceptional environments where all four fundamental forces are simultaneously important. Despite a decades-long effort in theory, experiments, and astrophysical observations to probe neutron star physics, we still have only a diverse set of hypotheses about the composition and properties of matter in such extreme conditions. The proposal is organized around three interrelated projects. We will first develop a systematic analysis strategy for the joint interpretation of gravitational waves and electromagnetic counterparts to determine the nature of the compact objects in a merging binary system. We will then address several current challenges in extracting the fundamental science from gravitational-wave signals, which relies on robust theoretical models, by advancing models to include more realistic physics and developing efficient descriptions for practical use. Finally, we will assess the prospects for probing black hole formation and measuring new physics with gravitational wave experiments such as LIGO, Virgo and the Einstein telescope. This project will provide key inputs for using the new field of GWs to (i) probe the fundamental physics of matter in unexplored regimes, (ii) distinguish double neutron star binaries from those involving a black hole or exotic object, (iii) measure the microphysics and energetics driving the merger, tidal disruption, and black hole formation, and (iv) elucidate the full cosmological context of these cataclysmic events. The proposal’s timely and urgent approach leverages experimental opportunities opening up with new facilities (including NWO funded projects) that, in return, will rely on the deliverables of such research. Given that this is an emerging new field, the current proposal may also achieve unexpected discoveries.

We will use the dedicated high-throughput computing facilities at SURF to analyze some of the most accurate GRMHD simulations carried out to date. The simulations include the effects of general relativity, (two-temperature) plasma, magnetic fields and radiation. The simulations have been carried out on European Tier-0 facilities and with their detailed analysis we hope to get closer to answering long-standing questions of the field such as How does a two-temperature accretion disk corona form? What is the role of winds in luminous accretion disks? How do accretion disks produce the observed quasi-periodic variability?

Characterizing the diversity of extrasolar planets (exoplanets) and assessing their potential for harboring life is one of the ultimate goals of the branch of astronomy dedicated to exoplanet studies. Whether a planet has a stable atmosphere is a key question, the answer to which depends on an interplay between a number of complex physical and chemical processes, including atmospheric escape. Atmospheric escape or mass loss can have a profound influence on the extent, composition, and evolution of a planetary atmosphere. Many aspects of this process, however, are still poorly understood, mostly due to a small number of direct observations of atmospheric escape in exoplanets that have been available until recently. In 2018, the spectral line of neutral helium at the wavelength of 1083 nm was discovered to be an excellent new diagnostic of upper layers of exoplanet atmospheres, where signatures of atmospheric escape can be studied. My previous work on theoretical modeling of escaping exoplanet atmospheres and their signatures at 1083 nm significantly contributed to establishing this new frontier in exoplanet characterization. As a Veni fellow, I will develop new 3D magnetohydrodynamic simulations of atmospheric escape in exoplanets and use them to generate synthetic observations (absorption spectra and transit light curves) in the helium 1083 nm line. I will compare the results of my simulations with high-resolution spectroscopic observations of three exoplanets with the strongest helium absorption signals recorded to date. This will allow me to constrain the physical properties of these atmospheres and infer their escape rates. This work will pave the way toward the development of empirically-based models of atmospheric mass loss and evolution, which are necessary for improving our understanding of planet formation and long-term stability and potential habitability of their atmospheres.

The project will use the adaptive mesh radiative magnetohydrodynamic simulation code RAMSES to model the evolution of nebulae in the Large and Small Magellanic Clouds neighbouring our Milky Way galaxy. The project will use the results of the previous 500 khr Cartesius project AMUN, which focussed on Orion and other Milky Way clouds, to explore wider conditions in the universe. This is timely because our group in Amsterdam is heavily involved in the VFTS survey of the LMC which requires theoretical interpretation, while collaborating groups in Leiden and Heidelberg are active in the new and upcoming surveys SOFIA and SDSS-V targetting this galaxy. The project is split into three subprojects: a large pathfinder for a full simulation of the 30 Doradus region, a zoom-in project supporting the successful HPC Europa 3 grant by Raphael Mignon-Risse to visit UvA and SURF, and a project exploring the dynamics and environment of large cloud complexes using targetted simulations. The project is integral to my research at API and to the science questions of the group at API/UvA and wider NOVA-network institutions.