We propose to model black holes in the framework of General Relativity in four and higher dimensions as well in alternative theories of gravity using numerical relativity and approximation theories. For convenience, our proposed research can be classified into two main areas: (i) The modeling of astrophysical compact binaries as sources of gravitational waves and (ii) the study of black-hole (BH) collisions in four and higher dimensional spacetimes as well as alternative theories of gravity. The first part of this proposal is motivated by the ongoing effort to detect gravitational waves (GW) from astrophysical sources with ground based laser interferometer detectors, LIGO, VIRGO and GEO600, as well as the planned space mission LISA. Among the most promising sources for these detectors are binary systems of stellar-mass and massive BHs. In order to maximize the physical output from the observations it is necessary to have available accurate theoretical predictions of the expected GW signal which will then be used in the analysis of the GW data stream using the so-called matched filtering technique. The major target of our study is to improve such theoretical predictions by combining numerical relativity results with approximate studies, including post-Newtonian and perturbation theory, over a wider range of mass ratios and including spin configurations with spin precession. We will use these simulations to generate template banks of waveforms and assess how the inclusion of the merger and ringdown part of the waveforms will improve parameter estimation in GW observations. We further plan to compare the numerical results with perturbative calculations for extreme-mass-ratio inspirals. The second part of this proposal is motivated by TeV particle collisions performed at the LHC and the possibility of generating BHs in such collisions. BH formation in these experiments may occur if the fundamental Planck scale is lowered due to the presence of large extra dimensions or extra dimensions with a warp factor. In these scenarios gravity becomes the dominant force at energies as low as the TeV range reachable by the LHC. BH formation and subsequent evaporation via Hawking radiation can be detected via its special signature in the experimental data, such as the jet multiplicity and transverse energy. The event generators to be used for the data analysis require as key input parameters the scattering threshold for BH formation and losses of energy and angular momentum in the form of GWs during the collision. We propose to perform numerical simulations of high-energy collisions of BHs in four as well as higher dimensional spacetimes in order to accurately determine these parameters. We also plan to explore the dynamics of BHs in non-asymptotically flat spacetimes as a preliminary investigation to use numerical relativity in the context of the AdS/CFT correspondence. Finally, we plan to develop tools in gravitational physics to perform tests of the space-time geometry of BHs and the validity of General Relativity and alternative theories of gravity by means of gravitational-wave observations. This involves the generation of waveform templates that include parameters that describe deviations from the Kerr geometry and from General Relativity.

The OAdM is the Montsec Astronomical Observatory (Observatori Astronòmic del Montsec in Catalan). It is located south of the Pyrenees on the Montsec mountain range at 1570 m a.s.l. and houses an 80 cm telescope that will be controlled either remotely or robotically. Its prime objectives are both scientific and technological. The commissioning work is being carried out in collaboration with the Universitat de Barcelona and Universitat Politècnica de Catalunya. This work consists in preparing the telescope to operate in the two modes and developing the necessary software to carry out such operations.

SQT is a 1-m robotic telescope enclosed in a clam shell-type dome of 6 m in diameter and mounted on a platform located next to the SuperWASP complex. The design of the telescope is such that it permits fully unattended operation thanks to its robotic mode. SQT is installed at the Observatorio del Roque de los Muchachos at La Palma, Canary Islands, one of the best astronomical sites in the world. The main goal of the SQT telescope is the exploration of exoplanetary systems. The Institute for Space Sciences has committed itself to carrying out a number of different aspects of the project, involving both hardware and software.

We perform numerical simulations of black holes in the framework of general relativity for the purpose of using them in the analysis of gravitational wave data from gravitational wave detectors, LIGO, VIRGO and LISA, and for the analysis of experimental data from parton-parton collisions at the LHC.

Numerical relativity, the gauge/gravity duality and trans-Planckian scattering have been tremendously active and successful areas in gravitational/high energy physics in recent years. They are strongly motivated by direct experimental connections: gravitational wave detection, probing strong interactions at the Large Hadron Collider (LHC) and at the Relativistic Heavy Ion Collider (RHIC) and even black hole production at the LHC. Numerical relativity methods, applied to black holes, will be essential (and powerful) in studying these high energy physics topics. Such merging is a new born field, pioneered by the proponents. It involves a strong numerical effort, requiring access to supercomputing facilities, expertise in theoretical and phenomenological modelling in high energy physics and contact with research teams working on dedicated experiments in particle accelerators. The necessary numerical relativity techniques have only very recently reached a state of sufficient maturity, which, together with the ongoing scientific runs at LHC and the beginning of science runs for advanced LIGO in the near future make this research programme extremely timely.

Medi Interestel·lar amb alta resolució angular: iniciant l'era d'ALMA

Estudi de viabilitat de LOFT, candidata a missió M3 d'ESA

Several planned space missions with the main goal to explore solar system small bodies will need to identify the best regions for sampling materials back to terrestrial laboratories. In this context, we need to increase our knowledge on the processes occurred in asteroids and comets, particularly the effect of metamorphism by collisional compaction, brecciation, and aqueous alteration. It is unclear that materials located at the surface or close to the surface of these bodies are really representative of pristine materials to gain insight on the first stages of solar system formation. Most chondrites have suffered alteration of their mineral components due to different processes. Thermal metamorphism and aqueous alteration are the most important ones. In any case, we still don’t know the extent of these processes in most of the chondrite groups. For example, some carbonaceous chondrite groups suffered extensive aqueous alteration, but for the most part escaped thermal metamorphism (e.g. only a few CMs evidence heating over several hundred Kelvin). Some chondrites escaped to the main early processes that altered the initial mineralogy and the abundances of presolar grains. Consequently, the materials forming these pristine chondrites, can be considered representative of the initial chemical and isotopic abundances present into the protoplanetary disk at the time and location where the parent bodies accreted. This research project works on these important issues for future missions of solar system minor bodies exploration, like e.g. the Marco Polo-R proposed mission to ESA and the ongoing Osiris-Rex (NASA) missions.

Gamma-ray astrophysics in the MeV energy range plays an important role for the understanding of many exciting stellar phenomena such as stellar explosions. However, a big step forward is still needed to detect the lines of radioactive nuclei directly in their sources, and in particular to detect the main isotopes produced in supernovae (e.g., 56Ni and 56Co, responsible for the optical light curve of type Ia supernovae) or in novae (7Be and 22Na), as well as the short duration 511 keV line in all of them. Only a strong effort in the field of simulations of gamma-ray detectors and the build-up of prototypes will allow for the necessary step forward in sensitivity required to reach such a goal. In parallel with the instrumental advances, it is necessary –of course- to pursue the theoretical models and the observations at other wavelengths (with the X-rays being also very crucial), to better understand the explosive phenomena in the Universe.

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