“Event-Related Spectral Perturbations” nel segnale EEG durante un compito di reaching

Questo elaborato ha analizzato le Event Related Spectral Perturbation (ERSP), cioè le variazioni nella potenza del segnale in corrispondenza di una frequenza o una banda di frequenze, suddivisi in Event Related Synchronization (ERS) nel caso di incremento di potenza e Event Related Desynchronization (ERD) nel caso di decremento di potenza, relative a movimenti di reaching eseguiti con l’arto superiore. In particolare, sono state prese in considerazione le potenze nel ritmo alpha (8-12 Hz) e ritmo beta (12-30 Hz), in quanto ritmi associati alla preparazione ed esecuzione del movimento. I segnali EEG analizzati (60 canali) sono relativi a 14 soggetti a cui è stato chiesto di compiere movimenti di reaching verso una posizione target, secondo una tempistica definita dall’accensione di uno stimolo visivo informativo (CUE, corrispondente al led nella posizione target) e un secondo stimolo visivo imperativo (GO) che dà il via libera all’esecuzione del movimento verso il target. Sono codificate 5 posizioni discrete, a 0°, 45°, 90°, 135° e 180°, su una semicirconferenza il cui centro rappresenta il punto di partenza e ritorno, chiamato base. I segnali preventivamente preprocessati, sono stati decomposti tramite trasformata wavelet ed elaborati con la tecnica dell’averaging, con lo scopo di evidenziare ERS e ERD in banda alpha e beta associati a eventi visivi e motori. È stata presentata l’evoluzione nel tempo della distribuzione topologica delle ERSP a livello dello scalpo e sono state svolte analisi suddividendo i dati secondo la direzione (destra, centro, sinistra) del target e secondo la profondità (vicino, medio, lontano) del target. I risultati mostrano una desincronizzazione (ERD) nella fase di preparazione del movimento (immediatamente prima dello stimolo GO), sia in banda alpha che beta e suggeriscono una modulazione dell’ERD in funzione della direzione/profondità del target.

Changes in the microbial community based on seawater pH variations

Ocean acidification is an effect of the rise in atmospheric CO2, which causes a reduction in the pH of the ocean and generates a number of changes in seawater chemistry and consequently potentially impacts seawater life. The effect of ocean acidification on metabolic processes (such as net community production and community respiration and on particulate organic carbon (POC) concentrations was investigated in summer 2012 at Cap de la Revellata in Corsica (Calvi, France). Coastal surface water was enclosed in 9 mesocosms and subjected to 6 pCO2 levels (3 replicated controls and 6 perturbations) for approximately one month. No trend was found in response to increasing pCO2 in any of the biological and particulate analyses. Community respiration was relatively stable throughout the experiment in all mesocosms, and net community production was most of the time close to zero. Similarly, POC concentrations were not affected by acidification during the whole experimental period. Such as the global ocean, the Mediterranean Sea has an oligotrophic nature. Based on present results, it seems likely that seawater acidification will not have significant effects on photosynthetic rates, microbial metabolism and carbon transport.

Ex situ X-­Ray absorption study of Li-­rich layered cathode material Li[Li0.2Mn0.56Ni0.16Co0.08]O2

The Li-rich layered transition metal oxides (LLOs) Li2MnO3-LiMO2 (M=Mn, Co, Ni, etc.) have drawn considerable attention as cathode materials for rechargeable lithium batteries. They generate large reversible capacities but the fundamental reaction mechanism and structural perturbations during cycling remain controversial. In the present thesis, ex situ X-ray absorption spectroscopy (XAS) measurements were performed on Li[Li0.2Mn0.56Ni0.16Co0.08]O2 at different stage of charge during electrochemical oxidation/reduction. K-edge spectra of Co, Mn and Ni were recorded through a voltage range of 3.7-4.8V vs. Li/Li+, which consist of X-ray absorption near edge structure (XANES) and extended X-ray absorption fine structure (EXAFS). Oxidation states during initial charge were discussed based on values from literature as well as XANES analysis. Information about bond distance, coordination number as well as corresponding Debye-Waller factor were extracted from Gnxas analysis of raw data in the EXAFS region. The possibility of oxygen participation in the initial charge was discussed. Co and Ni prove to take part in the oxidation/reduction process while Mn remain in the tetravalent state. The cathode material appears to retain good structural short-range order during charge-discharge. A resemblance of the pristine sample and sample 4 was discovered which was firstly reported for similar compounds.

Origin of cold gas and dust in massive elliptical galaxies

The recent availability of multi-wavelength data revealed the presence of large reservoirs of warm and cold gas and dust in the innermost regions of the majority of massive elliptical galaxies. To prove an internal origin of cold and warm gas, the investigation of the spatially distributed cooling process which occurs because of non-linear density perturbations and subsequent thermal instabilities is of crucial importance. The first goal of this work of thesis is to investigate the internal origin of warm and cold phases. Numerical simulations are the powerful tool of analysis. The way in which a spatially distributed cooling process originates has been examined and the off-centre amount of gas mass which cools when different and differently characterized AGN feedback mechanisms operate has been quantified. This thesis demonstrates that the aforementioned non-linear density perturbations originate and develop from AGN feedback mechanisms in a natural fashion. An internal origin of the warm phase from the once hot gas is shown to be possible. Computed velocity dispersions of ionized and hot gas are similar. The cold gas as well can originate from the cooling process: indeed, it has been estimated that the surrounding stellar radiation, which is one of the most feasible sources of ionization of the warm gas, does not manage to keep ionized all the gas at 10^4 K. Therefore, cooled gas does undergo a further cooling which can lead the warm phase to lower temperatures. However, the gas which has cooled from the hot phase is expected to be dustless; nonetheless, a large fraction of early type galaxies has detectable dust in their cores, both concentrated in filamentary and disky structures and spread over larger regions. Therefore a regularly rotating disk of cold and dusty gas has been included in the simulations. A new quantitative investigation of the spatially distributed cooling process has therefore been essential: the contribution of the included amount of dust which is embedded in the cold gas does have a role in promoting and enhancing the cooling. The fate of dust which was at first embedded in cold gas has been investigated. The role of AGN feedback mechanisms in dragging (if able) cold and dusty gas from the core of massive ellipticals up to large radii has been studied.

Galactic fountain flows in high-resolution hydrodynamical simulations of galaxy disks

Feedback from the most massive components of a young stellar cluster deeply affects the surrounding ISM driving an expanding over-pressured hot gas cavity in it. In spiral galaxies these structures may have sufficient energy to break the disk and eject large amount of material into the halo. The cycling of this gas, which eventually will fall back onto the disk, is known as galactic fountains. We aim at better understanding the dynamics of such fountain flow in a Galactic context, frame the problem in a more dynamic environment possibly learning about its connection and regulation to the local driving mechanism and understand its role as a metal diffusion channel. The interaction of the fountain with a hot corona is hereby analyzed, trying to understand the properties and evolution of the extraplanar material. We perform high resolution hydrodynamical simulations with the moving-mesh code AREPO to model the multi-phase ISM of a Milky Way type galaxy. A non-equilibrium chemical network is included to self consistently follow the evolution of the main coolants of the ISM. Spiral arm perturbations in the potential are considered so that large molecular gas structures are able to dynamically form here, self shielded from the interstellar radiation field. We model the effect of SN feedback from a new-born stellar cluster inside such a giant molecular cloud, as the driving force of the fountain. Passive Lagrangian tracer particles are used in conjunction to the SN energy deposition to model and study diffusion of freshly synthesized metals. We find that both interactions with hot coronal gas and local ISM properties and motions are equally important in shaping the fountain. We notice a bimodal morphology where most of the ejected gas is in a cold $10^4$ K clumpy state while the majority of the affected volume is occupied by a hot diffuse medium. While only about 20\% of the produced metals stay local, most of them quickly diffuse through this hot regime to great scales.