With more than 5300 exoplanets detected so far, it is clear that planet formation is a robust and efficient process. The current population of known exoplanets exhibits a wide diversity, both in nature (mass, radius) and in architecture: while giant planets can be found at large separations, the most common type of exoplanetary systems revealed by Kepler transits consist of chains of low-mass planets, super-Earths and mini-Neptunes, located close to their host stars. To understand the origin of this diversity, we need to explore the birth environment of the planets, namely the planet-forming protoplanetary disks, and to investigate their structure and evolution on both local and global scales. While considerable progress has recently been made in probing the disks on large scales (a few tens of astronomical units, au), little is known about the innermost regions (less than a few au). The IRYSS (Innermost Regions of Young Stellar Systems) project aims at deciphering the processes at play in the innermost regions of protoplanetary disks (PPDs). For the first time, we will provide a statistical view of the inner parts of a large sample of PPDs, thus bringing to light the main missing piece in our understanding of planet formation. The project builds on the unique synergy between the observational approaches developed by the partners, IPAG and IRAP, on national Research Infrastructures such as ESO/VLTI (with the PIONIER and GRAVITY interferometric instruments, largely developed at IPAG) and CFHT (with the ESPaDOnS and SPIRou spectropolarimeters, both developed at IRAP), in combination with the development of advanced physical models of the inner disk edge and of the accretion flows onto the central star. Benefiting from these world-class facilities, which are at the heart of the orientations of the call, we will conduct a multi-wavelength, multi-technique, and multi-scale investigation of the inner disk regions in a few tens of young stellar systems. We will explore the initial and environmental conditions that prevail at the time of planet formation by addressing three intrinsically interconnected pillars: 1) the morphological (asymmetry, vortex, dead zone) and physical (temperature, density) properties of the innermost scales of the protoplanetary disk, by spatially resolving at the sub-au level the near- and mid-infrared continuum emission with interferometry; 2) the magnetic star-disk interaction region, extending over a few stellar radii, and whose outer edge is thought to be the place where inwards migrating planets pile up, with spectropolarimetric observations and Zeeman-Doppler Imaging to derive the magnetic field topology and strength; 3) the dynamical timescales of the physical processes from a few days to months, by monitoring the variability of both the magnetic topology and the small-scale disk features. The combined analysis of these data sets arising from these two state-of-the-art observational techniques will put the world-leading French experts in a unique position to provide the stellar and exoplanet communities with legacy databases of magnetic maps, line profiles, inner rim positions and disk substructures. These are the key ingredients to relate the magnetic properties of young stars to the structure of their inner disk, and to investigate their evolution over periods as long as 10 years for some emblematic objects. As such, this legacy will provide access to a detailed overview of the innermost regions of nascent stellar systems and their disks where close-in planets form. Our team has access to all the ESO and CFHT Large Program and Guarantee Time observations to be exploited in the IRYSS project, and has developed during previous ERC-funded grants cutting-edge analysis and modeling tools required for their interpretation. We therefore gather the optimal expertise to yield major advances in this competitive field, supported by the appropriate workforce provided by this specific and quite timely ANR call.

One of the major questions in modern physics is how life emerged on Earth and whether it is a general characteristic of our Universe. In addition to its own interest, understanding molecular complexity in space helps to understand the link between the young Solar System and its small bodies, in which today we detect complex molecules and even amino acids (as in comets and meteorites). Where these molecules come from? How and where did they form? What do they tell us about stars and planets formation? And last, but not least, atoms and molecules are the remote thermometers and barometers, as their observed line spectra can and are used to extract a mine of precious and often unique information. Grain-surface astrochemistry is facing new fascinating and challenging questions. Among them, three are particularly relevant for this project: - Is it possible to build a grain-surface chemistry starting from radical blocks, and if so, what will be the chemical routes? - Is the diffusion of radicals fast enough to compete with atom addition (and destruction)? - How to measure radicals in experiments, in realistic conditions ? - Is grain-surface chemistry fully compatible with the astronomical observations and the current astrochemical models? Or in other words, what ISM molecules form prevalently on the grain surfaces and when? Here we propose to join the forces between two groups with complementary laboratory expertise (LERMA and PIIM) and one with astrophysical, observations and modeling, expertise (IPAG). The immediate project goal is to understand how molecules diffuse, meet and mate on the grain surfaces in order to assess what COMs are formed on them and how. To reach it, we will compare dedicated laboratory experiments and include them in a new astrochemical code able, at the end of the project, to compare predictions with observations, and to better understand the role and limits of the solid-state chemistry in space. The work is organized in 3 connected tasks corresponding of our 3 expertises : 1) Diffusion of radicals and building-up molecules on surfaces. It includes i) the optimization of new source of radicals and the measurement of their diffusions ii) the systematic studies of the reactivity of specific chemical groups iii) in order to understand what is the limit of the complexity of COMs synthesized on surfaces 2) An innovative experimental set-up will be implemented at PIIM coupling low-temperature chemistry and electron spin resonance (ESR) to overcome our blindness to intermediate species. Once done, slow reactivity of radical with their molecular environment will be studied, simulating the early stage of ice mantle growth. The final goal is to study radical-radical chemistry that should occur during the formation of stars 3) We will build up a new code, from GRAINOBLE, that is able to simulate the experimental results. Only after this first step, it will be possible to extrapolate the experimental results to the ISM conditions, as well as having a better determination of physical parameters to be included in astrochemical codes. The natural end of this project will be to compare our understanding of the solid-state chemistry to observations, to evaluate its impact on the molecular growth and to diffuse our results.

The observation of the sky at millimetre and submillimetre wavelengths in the past years contributed to tremendous improvements in our understanding of a great variety of scientific topics ranging from the star formation in the Milky Way to the measurement of cosmological parameters. Following the recent results obtained by the Planck and Herschel satellites, the advent of a millimetre camera, capable of surveying large areas of the sky at a high-angular resolution, with a high sensitivity and a large field of view, will continue to reveal the details of the formation and evolution of structures throughout the Universe. The NIKA2 camera is a next-generation instrument for millimetre astronomy. It is operated at 100 mK and will be installed in June 2015 on the 30-m telescope of IRAM (Institut de RadioAstronomie Millimétrique). NIKA2 will observe the sky at 150 and 260 GHz with a wide field of view (6.5 arcmin) at high-angular resolution (nominally 18 and 12 arcsec, respectively), and state-of-art sensitivity (requirement 20 and 30 mJy.s1/2, respectively). It will also have polarization capabilities at 260 GHz. With its high mapping speed (5000 detectors in total) and dual band observation, NIKA2 will revolutionize our view of the cold Universe. No other instrument exists or is even planned for the coming years to compete with NIKA2 in terms of sensitivity, angular resolution, polarization capabilities and available time of observation in the world. The NIKA2 consortium is an international collaboration gathering 14 laboratories from France UK and Italy that has successfully answered in 2011 a call for tender issued by the IRAM concerning the next generation large field continuum instrumentation at the 30-m telescope. The first phase (2011-2015) of the project has been partially funded by the ANR. It addresses the design, building and testing of the NIKA2 camera. This phase is completed and the camera is taking the first laboratory images in the two bands, including the polarization channel. The NIKA2 schedule for the installation in June 2015 at the 30-m telescope has been approved by IRAM. During this first phase, a prototype camera (NIKA1, dual-band with a total of ~300 KIDs) has also been built and installed at the IRAM 30-m telescope. As a test bench for the final NIKA2 instrument, the NIKA1 camera has been optimized during the two observation campaigns on November 2012 and June 2013. Current NIKA1 performance fulfills already the NIKA2 requirements in terms of sensitivity. The second phase (2016-2020) regards the scientific exploitation of this future world-leading instrument. Indeed, 1300 hours have been allocated to the NIKA2 consortium, i.e. the largest amount of guaranteed time ever given by IRAM to a single collaboration. Our NIKA2Sky project is centered on the three large programs led by French institutes, that have each been granted 300 hours of observation (900 hr in total). The scientific program is dedicated to the study of the inner structure of galaxy clusters via Sunyaev Zel’dovich effect, and of star formation at low and high redshift, both by studying the role of magnetic fields on sub-parsec scales (down to a resolution of ~ 2000 AU) in our Galaxy, and mapping the dusty star forming galaxies up to redshifts 6. We request a financial support to hire 4 post-docs and organize collaboration meetings as well as a workshop to ensure a high visibility of the results obtained with NIKA2. This support would capitalize on our instrumental efforts, funded by the ANR, which led to the building of a unique and world-leading instrument in millimetre astronomy.

ABSTRACT. In regions of active star formation, the protoplanetary discs around young stars act as planetary factories. Recent observing campaigns have shown that the majority of protostars belong to multiple stellar systems: the younger the stars, the higher the degree of multiplicity. Young discs are then strongly affected by stellar multiplicity, unavoidably modifying the way in which planets form. The detailed evolution of multiple systems with discs and planets however remains to be explored. Since most current models have been designed for single stars, there is an urgent need to extend these models to multiple stars. This will pave the way for a better understanding of the process of planet formation within our galaxy. The Stellar-MADE project aims to provide a comprehensive view of disc dynamics and planet formation within multiple stellar systems. My team and I will thoroughly study multiples to: (1) Establish the formation channels of protoplanetary discs around young stellar objects; (2) Follow disc dynamics and grain growth in order to identify the regions of planetesimal formation; (3) Characterise planetary architectures and the resulting exoplanet population. To achieve our goals we will perform hydrodynamical and N-body simulations, developing and adapting state-of-the-art codes (Phantom, mcfost, Rebound). Our calculations will include a broad range of physical processes: disc thermodynamics, radiative transfer, gravitational perturbations, aerodynamic friction, dust growth, and Mean-Motion Resonances. This will allow us to identify and quantify stellar multiplicity effects across evolution. My previous work on binary stars constitutes proof-of-concept that it is possible to coherently connect protoplanetary disc evolution to planetary architectures. Unveiling the effects of stellar multiplicity on planet formation will be a major breakthrough. PROJECT OBJECTIVES. The aim of this project is to study the impact of stellar multiplicity on planet formation: from the onset of disc formation in gaseous clouds to the final stage where stars host stable planetary systems. Three scientific questions will drive the proposed investigation: i) What are the initial protoplanetary disc conditions around young stellar multiple objects? ii) Where do solid bodies and planetesimals grow within discs in multiple stellar systems? iii) What are the most stable planetary architectures in multiple stellar systems? SCIENTIFIC IMPACT. This project will unveil the effects of stellar multiplicity on planet formation, which will allow us to interpret the whole exoplanetary population under a new prism. Our expected results will become the stepping stone for future research on multiple stellar systems. As a matter of fact, stellar multiplicity is the norm – rather than the exception – in active star-forming regions. It is therefore key to understand the impact of stellar multiplicity on planet formation. The ground- breaking nature of this proposal will guarantee a high impact at the international level, placing the Stellar- MADE team at the forefront of the emerging field of research on disc and planet dynamics in multiples. Our results are expected to open new avenues for studying the disc chemical reservoir across stellar evolution, planetesimal formation, and its impact on exoplanet composition.

Cometary dust particles rain on Earth. However, they can only be found in collections performed in the cleanest regions of the Earth (the stratosphere and Antarctica). From Antarctic snow at the vicinity of the French-Italian Concordia Antarctic base, we recovered large (> 50-100 µm) particles of very probable cometary origin, the Ultracarbonaceous Antarctic Micrometeorites (UCAMMs). UCAMMs are constituted of a dominant fraction of a solid macromolecular organic matter intimately mixed with a minor mineral component. The organic matter is structurally disorganized, shows large deuterium enrichments and exhibit an unusually large bulk nitrogen concentrations (up to 20 at%). Preliminary studies have shown that several types of organic matter co-exist in UCAMMs, with different nitrogen contents and mixed with different amounts of minerals. The minerals embedded in the organic matter have typical sizes around 50-100 nm. Both crystalline and amorphous minerals are present and exhibit a wide range of compositions. Some precursors of UCAMM organic matter (the most N-rich) could have been formed by galactic cosmic rays’ irradiation of nitrogen-rich ices at the surface of icy bodies in the outer regions of the protoplanetary disk. UCAMMs are remarkable particles as their subcomponents preserved records of early solar system formation and evolution. The association in UCAMMs of minerals (formed at high temperatures) among large amounts of organic matter (necessarily formed at lower temperatures) opens a new window on the study of the origin and formation mechanisms of matter originating from the outer regions of the solar system. This proposal focuses on the formation mechanism and evolution of cometary dust organics and their relation with the mineral components embedded within, following 3 main questions: 1. What is the origin of the subcomponents of cometary matter? "Inner and outer solar system…" 2. What are the variations of the composition of organics and their embedded minerals with heliocentric distance? 3. How did the different environments encountered (radiative interplanetary medium, terrestrial atmosphere, Antarctica) modify the cometary particles collected on Earth? This project proposes innovative analysis protocols of UCAMMs using state-of the-art analysis techniques to characterize both the organic matter, the minerals and their association. Experimental simulations of their evolution from interplanetary space to their collection in Antarctica will be performed on cometary organic analogues and on synthetic UCAMMs produced in the laboratory. The originality of the COMETOR proposal resides in four points: i) the availability in the laboratory of well-preserved cometary samples; ii) the analysis of these complex particles with a combination of complementary and state-of-the-art techniques – including infrared spectroscopy coupled with atomic force microscopy (AFMIR) that allows infrared analysis at the ~ 50-100 nm scale; iii) the production of analogues of cometary solids and the real-time observation of their evolution under irradiation thanks to the unique JANNuS platform, coupling a transmission electron microscope with two ion accelerators; iv) the search for soluble organic compounds (including amino acids) in UCAMMs with the very high mass resolution Orbitrap technique to probe the input of prebiotic molecules on the early Earth by cometary dust. The expected results will have implications in the fields of astrophysics, planetology-cosmochemistry and astrobiology. They will bring an original contribution to the understanding of the formation and evolution of solid matter in the outer regions of the protoplanetary disk, as well as important inputs for the interpretation of data from Rosetta and Stardust samples, from samples returned by future space missions such as Hayabusa 2, OSIRIS-Rex, and for the observations of protoplanetary disks by the future James Webb Space Telescope (JWST).