Pubblica selezione per titoli e colloquio per il conferimento di una borsa di studio dal titolo: “Studio di nuove tecnologie per lo sviluppo di software di Monitoring Logging a Alarm […]
Pubblica selezione per titoli ed eventuale colloquio per il conferimento di un assegno di ricerca post dottorato dal titolo “Tecniche diagnostiche e modellistiche per lo studio della corona solare estesa”, […]
Pubblica selezione per titoli ed eventuale colloquio per il conferimento di un assegno di ricerca di professionalizzazione, della durata di 12 mesi, eventualmente prorogabili, dal titolo “Attività di divulgazione per […]
One of the major challenges in the context of the Cosmic Microwave Background (CMB) radiation is to detect a polarization pattern, the so called B-modes of CMB polarization, that are thought to be directly linked to the space-time fluctuations present in the Universe at the very first instants of life. To date, several challenges have prevented to detect the B-modes partly because of the lower sensitivity of the detectors. Our own Galaxy is observed in this context as a foreground contamination. However the awareness of improving the modeling of its polarized emission has been constantly increase not only to assess the cosmological signals but also to provide new insights onto the Galactic magnetic field probed with the Galactic polarized emissions, e.g. synchrotron and thermal dust. This is particularly relevant in order to better characterize the foreground contamination for future CMB experiments (e.g. SO, LiteBIRD, CMB-S4 ), where unprecedented polarization sensitivities are expected to be achieved in the coming decades.
Pubblica selezione per titoli ed eventuale colloquio per il conferimento di un assegno di ricerca di professionalizzazione, per la durata di 12 mesi, eventualmente prorogabili, dal titolo “Sviluppo software per […]
The atmospheric parameters have a strong impact on the image formation through the atmosphere. Indeed, the effect of atmospheric turbulence on wavefronts reduces severely the resolution of ground-based astronomical observations. Thus, in the context of astronomical observations, the site-selection has now become essential with the advent of the next generation of Extremely Large Telescopes (ELT). Indeed, it is important to choose sites with reduced cloud coverage, weak turbulence and low aerosol distribution in order to enhance observations time and to improve their scientific performance. It is also important to remember that the choice of sites hosting astronomical projects must meet very strict criteria in terms of optical quality. Future optical communications and telemetry stations will be forced to meet the same
requirements.
Studying small bodies in our solar system is fundamental for understanding its youth and evolution. These small "primitive" bodies are "undifferentiated" (they did not undergo phase density separation, irreversibly altering their mineralogy). They have evolved little since their creation, spurring a composition relatively close to the primordial proto-planetary disk. However, other processes, such as thermal alteration, aqueous alteration, shocks, or space-weathering, can affect these bodies' surfaces.
Pubblica selezione per titoli ed eventuale colloquio per il conferimento di un assegno di ricerca di professionalizzazione, della durata di 12 mesi, eventualmente prorogabili, dal titolo “Sviluppo tecnico-scientifico array CTA”, […]
Bando di selezione per titoli ed eventuale colloquio per il conferimento di n. 3 assegni di ricerca di "professionalizzazione" nell'ambito del progetto denominato “NATIONAL CENTRE FOR HPC, BIG DATA AND […]
Less than a decade after the first historical Gravitational Wave (GW) detection GW150914, the field of GW astronomy has grown at a phenomenal pace, going from less than an event per month, to the currently observed rate of few events a week.
Despite the exceptional contributions the field has brought to fundamental physics, astronomy, cosmology, computational physics as well as the unavoidable collateral progress in fields related to the experimental development of GW detectors, the picture is anything but complete.
Amongst the missing pieces of the puzzle we find Continuous Gravitational Waves (CGWs).
In this seminar I am going to talk about CGWs, what are they and what astrophysical sources and mechanisms can produce them, with a particular focus on non-axisymmetric spinning Neutron Stars.
I will also briefly discuss the different search implementations, what is done, or can be done, to increase our chances to arrive to what is probably going to be the next breakthrough in GW Astronomy, the first CGW detection, including a discussion about prospects in view of future observation runs as well as GW detectors operational in the close future.