Resolved stellar populations in milky way and andromeda's new satellites

This thesis concerns the study of the variable stars and resolved stellar populations in four recently discovered dSphs, namely, Hercules and Ursa Major I (UMa I), which are UFD satellites of the MW; Andromeda XIX (And XIX) and Andromeda XXI (And XXI), which are satellites of M31. The main aim is to obtain detailed informations on the properties (age, metallicity, distance, and Oosterhoff type) of the stellar populations in these galaxies, to compare them with those of other satellites around the MW and M31, both ''classical'' dSphs and UFDs. The observables used to achieve these goals are the pulsating variables, especially the RR Lyrae stars, and the color magnitude diagram (CMD) of the resolved stellar populations. In particular, for UMa I, we combined B, V time-series observations from four different ground-based telescopes (Cassini, TLS, TT1 and Subaru) and for Hercules, we used archival data acquired with the Advanced Camera for Surveys (ACS) on board the HST. We used, instead B and V times-series photometry obtained with the Large Binocular Telescope (LBT) for And XIX and And XXI .

Analytic modelling of the galactic fountain in the Milky Way potential

Le galassie a spirale, come la Via Lattea, sono caratterizzate dalla presenza di gas freddo e formazione stellare e vengono perciò chiamate star-forming. Per creare nuove stelle è necessaria una sufficiente riserva di gas, la cui disponibilità governa l’evoluzione della galassia stessa. Finora, non è stato individuato con certezza un meccanismo che possa alimentare la formazione di nuove stelle nelle galassie star-forming. Una delle possibili sorgenti di tale gas è l’alone galattico caldo (corona galattica) il cui raffreddamento e successivo accrescimento possono essere stimolati dal processo di fontana galattica. L’esplosione di supernovae porta nubi di gas freddo in orbita al di sopra del disco stellare; queste nubi raggiungono altezze dell’ordine del kiloparsec, interagendo con la corona di gas caldo. Il moto delle nubi all’interno di un mezzo meno denso comporta l’instaurarsi dell’instabilità di Kelvin-Helmholtz, che ’strappa’ gas dalle nubi e causa la condensazione di materia coronale. Quest’ultima viene quindi accresciuta e, ricadendo sul disco, trasferisce nuovo materiale alla galassia e ne alimenta la formazione stellare. Lo scopo di questa tesi è derivare un modello analitico di fontana galattica che consenta di ottenere una formulazione analitica per il tempo orbitale, cioè il tempo richiesto alle nubi per ricadere sul disco galattico. Infatti, più u tempo le nubi impiegano per attraversare il materiale coronale caldo e ricadere sul disco, più materiale viene accresciuto durante l’orbita. Conoscendo i tempi orbitali sarebbe possibile calcolare il tasso di accrescimento legato al fenomeno di fontana e studiarne l’andamento con il raggio del disco. Questo modello potrebbe rivelarsi utile per lo studio dell’impatto della fontana nell’evoluzione globale del disco galattico e della chimica dell’intera galassia.

Mock HI observations of Milky Way-like simulated galaxies

L'obiettivo di questo lavoro di tesi consiste nel descrivere sia il processo necessario per la creazione di osservazioni sintetiche di galassie simulate simili alla Via Lattea nella riga di emissione a 21 cm dell'idrogeno neutro (HI), sia il lavoro di analisi fondamentale che serve a confrontare in modo efficace l'output generato con delle osservazioni di galassie reali. Come prima cosa è descritta la teoria quantistica che sta alla base dell'emissione a 21 cm di HI, illustrando l'importanza di tale riga di emissione nell'ambito dell'astronomia e come si possano ottenere informazioni fondamentali sulle sorgenti di questa radiazione a partire dai dati osservativi. Il lavoro poi si focalizza sull'utilizzo del software MARTINI per la creazione di osservazioni sintetiche della linea a 21 cm per una galassia simulata con proprietà simili alla Via Lattea generata utilizzando il modello numerico SMUGGLE. Infine, si passa ad una breve descrizione dell'analisi dei dati sintetici creati, e al loro confronto con dei dati provenienti da osservazioni reali di galassie con proprietà simili, per ottenere una valutazione qualitativa della bontà del modello SMUGGLE impiegato nella simulazione numerica.

Spatio-temporal variation of macrofaunal assemblages in the deep Blanes submarine canyon

The spatio-temporal variations in diversity and abundance of deep-sea macrofaunal assemblages (excluding meiofaunal taxa, as Nematoda, Copepoda and Ostracoda) from the Blanes Canyon (BC) and adjacent open slope are described. The Catalan Sea basin is characterized by the presence of numerous submarine canyons, which are globally acknowledged as biodiversity hot-spots, due to their disturbance regime and incremented conveying of organic matter. This area is subjected to local deep-sea fisheries activities, and to recurrent cold water cascading events from the shelf. The upper canyon (~900 m), middle slope (~1200 m) and lower slope (~1500 m) habitats were investigated during three different months (October 2008, May 2009 and September 2009). A total of 624 specimens belonging to 16 different taxa were found into 67 analyzed samples, which had been collected from the two study areas. Of these, Polychaeta, Mollusca and Crustacea were always the most abundant groups. As expected, the patterns of species diversity and evenness were different in time and space. Both in BC and open slope, taxa diversity and abundance are higher in the shallowest depth and lowest at -1500 m depth. This is probably due to different trophic regimes at these depths. The abundance of filter-feeders is higher inside BC than in the adjacent open slope, which is also related with an increment of predator polychaetes. Surface deposit-feeders are more abundant in the open slope than in BC, along with a decrement of filter-feeders and their predators. Probably these differences are due to higher quantities of suspended organic matter reaching the canyon. The multivariate analyses conducted on major taxa point out major differences effective taxa richness between depths and stations. In September 2009 the analyzed communities double their abundances, with a corresponding increase in richness of taxa. This could be related to a mobilizing event, like the release of accumulated food-supply in a nepheloid layer associated to the arrival of autumn. The highest abundance in BC is detected in the shallowest depth and in late summer (September), probably due to higher food availability caused by stronger flood events coming from Tordera River. The effects of such events seemed to involve adjacent open slope too. The nMDS conducted on major taxa abundance shows a slight temporal difference between the three campaigns samples, with a clear clustering between samples of Sept 09. All depth and all months were dominated by Polychaeta, which have been identified to family level and submitted to further analysis. Family richness have clearly minimum at the -1200 m depth of BC, highlighting the presence of a general impact affecting the populations in the middle slope. Three different matrices have been created, each with a different taxonomic level (All Taxa “AT”, Phylum Level “PL” and Polychaeta Families “PF”). Multivariate analysis (MDS, SIMPER) conducted on PL matrix showed a clear spatial differences between stations (BC and open slope) and depths. MDSs conducted on other two matrices (AT and PF) showed similar patterns, but different from PL analysis. A 2 nd stage analysis have been conducted to understand differences between different taxonomic levels, and PL level has been chosen as the most representative of variation. The faunal differences observed were explained by depth, station and season. All work has been accomplished in the Centre d’estudis avançats de Blanes (CEAB-CSIC), within the framework of Spanish PROMETEO project "Estudio Integrado de Cañones y Taludes PROfundos del MEdiTErráneo Occidental: un hábitat esencial", Ref. CTM2007-66316-C02- 01/MAR.

Genetic characterisation and global comparison of ancient Mediterranean Great White Sharks population (Carcharodon carcharias, L.1758)

This study poses as its objective the genetic characterization of the ancient population of the Great White shark, Carcharodon carcharias, L.1758, present in the Mediterranean Sea. Using historical evidence, for the most part buccal arches but also whole, stuffed examples from various national museums, research institutes and private collections, a dataset of 18 examples coming from the Mediterranean Sea has been created, in order to increase the informations regarding this species in the Mediterranean. The importance of the Mediterranean provenance derives from the fact that a genetic characterization of this species' population does not exist, and this creates gaps in the knowledge of this species in the Mediterranean. The genetic characterization of the individuals will initially take place by the extraction of the ancient DNA and the analysis of the variations in the sequence markers of the mitochondrial DNA. This approach has allowed the genetic comparison between ancient populations of the Mediterranean and contemporary populations of the same geographical area. In addition, the genetic characterization of the population of white sharks of the Mediterranean, has allowed a genetic comparison with populations from global "hot spots", using published sequences in online databases (NCBI, GenBank). Analyzing the variability of the dataset, both in terms space and time, I assessed the evolutionary relationships of the Mediterranean population of Great Whites with the global populations (Australia/New Zealand, South Africa, Pacific USA, West Atlantic), and the temporal trend of the Mediterranean population variability. This method based on the sequencing of two portions of mitochondrial DNA genes, markers showed us how the population of Great White Sharks in the Mediterranean, is genetically more similar to the populations of the Australia Pacific ocean, American Pacific Ocean, rather than the population of South Africa, and showing also how the population of South Africa is abnormally distant from all other clusters. Interestingly, these results are inconsistent with the results from tagging of this species. In addition, there is evidence of differences between the ancient population of the Mediterranean with the modern one. This differentiation between the ancient and modern population of white shark can be the result of events impacting on this species occurred over the last two centuries.

Preparazione di catalizzatori strutturati per la reazione di ossidazione parziale del metano

Questo lavoro di tesi ha avuto come obiettivo la preparazione di catalizzatori attivi nella reazione di ossidazione parziale catalitica, CPO, del metano per produrre gas di sintesi. I catalizzatori sono stati preparati tramite sintesi elettrochimica di composti di tipo idrotalcite a base di Rh/Mg/Al utilizzando come supporto schiume metalliche costituite da FeCrAlY. L’impiego di questo tipo di supporto comporta una serie di vantaggi, dallo sviluppo del catalizzatore all’ottimizzazione del processo catalitico in termini di prestazioni catalitiche, diminuzione degli “hot spots” termici, diminuzione delle perdite di carico e costi del catalizzatore. La sintesi del catalizzatore è stata effettuata per mezzo di una cella elettrochimica innovativa, che lavora in flusso, e quindi permette la continua rigenerazione della soluzione di sintesi, a differenza di quanto avviene in una cella elettrochimica standard a singolo comparto. La precipitazione dei composti di tipo idrotalcite si ottiene grazie alla tecnica di elettrogenerazione di basi, ovvero grazie alla generazione di un pH basico all’interno della cella elettrochimica a seguito dell’applicazione di un potenziale catodico. Il pH generato è il parametro più importante e determina la natura e la qualità del materiale depositato. È sorta quindi la necessità di sviluppare un sensore potenziometrico miniaturizzato per la determinazione istantanea del pH durante la sintesi, da installare all’interno della schiuma stessa. È possibile correlare le prestazioni catalitiche dei catalizzatori sintetizzati con la cella elettrochimica in flusso, alle loro caratteristiche di morfologia superficiale ed alla composizione chimica, e confrontare le stesse prestazioni catalitiche con quelle ottenute sintetizzando i catalizzatori con la cella elettrochimica standard a singolo comparto.

Multifrequency VLBA observations of two compact symmetric objects

In this thesis the results of the multifrequency VLBA observations of the GPS 1944+5448 and the HFP J0111+3906 are presented. They are compact objects smaller than about 100 pc, completely embedded in the host galaxy. The availability of multi-epoch VLBI observations spanning more than 10 years, allowed us to compute the hot spot advance speed in order to obtain the kinematic age of both sources. Both radio sources are young, in agreement with the idea that they are in an early evolutionary stage. The spectral analysis of each source component, such as the lobes, the hot spots, the core and the jets, making a comparison with the theoretical ones is described. In addition the physical parameters derived from VLBA images as the magnetic field, the luminosity, the energy and the ambient medium density of both sources are discussed.

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.

Stationary states in random walks on networks

In this thesis we dealt with the problem of describing a transportation network in which the objects in movement were subject to both finite transportation capacity and finite accomodation capacity. The movements across such a system are realistically of a simultaneous nature which poses some challenges when formulating a mathematical description. We tried to derive such a general modellization from one posed on a simplified problem based on asyncronicity in particle transitions. We did so considering one-step processes based on the assumption that the system could be describable through discrete time Markov processes with finite state space. After describing the pre-established dynamics in terms of master equations we determined stationary states for the considered processes. Numerical simulations then led to the conclusion that a general system naturally evolves toward a congestion state when its particle transition simultaneously and we consider one single constraint in the form of network node capacity. Moreover the congested nodes of a system tend to be located in adjacent spots in the network, thus forming local clusters of congested nodes.