Liver transplantation for transthyretin amyloidosis: experience of a single center in Italy

Liver transplantation is the only definitive treatment for transthyretin amyloidosis, with an excellent 5-year survival in endemic countries where the Met30 mutation is predominant. We report our experience of liver transplantation for transthyretin amyloidosis. We reviewed the clinical records of 17 transplanted patients (11 males, 6 females; age at liver transplant: 45.7±11.7 years). We had a wide spectrum of non-Met30 mutations (52.9%), with a predominance of Gln89 (23.5%). Five-year survival after transplantation was 43.8%; at multivariate analysis, both non-Met30 mutations (HR 17.3, 95% CI 1.03-291.7) and modified BMI (HR 0.50, 95% CI 0.29-0.87) showed significant and independent prognostic roles (P=0.048 and P=0.015, respectively). Five out of the 9 non-Met30 carriers received combined heart transplantation because of severe cardiomyopathy; they showed a trend towards a better prognosis vs. the 4 patients who did not receive combined heart transplantation (although not statistically significant; P=0.095). At follow-up, no significant improvement of transthyretin amyloidosis manifestations was observed. The results of liver transplantation for transthyretin amyloidosis in our population are poorer than those reported in the literature probably because of the high prevalence of non-Met30 mutations.

Il problema del risparmio energetico nei data center

Con la crescente diffusione del web e dei servizi informatici offerti via internet, è aumentato in questi anni l’utilizzo dei data center e conseguentemente, il consumo di energia elettrica degli stessi. Il problema ambientale che comporta l’alto fabbisogno energetico, porta gli operatori di data center ad utilizzare tecniche a basso consumo e sistemi efficienti. Organizzazioni ambientali hanno rilevato che nel 2011 i consumi derivanti dai data center raggiungeranno i 100 milioni di kWh, con un costo complessivo di 7,4 milioni di dollari nei soli Stati Uniti, con una proiezione simile anche a livello globale. La seguente tesi intende valutare le tecniche in uso per diminuire il consumo energetico nei data center, e quali tecniche vengono maggiormente utilizzate per questo scopo. Innanzitutto si comincerà da una panoramica sui data center, per capire il loro funzionamento e per mostrare quali sono i componenti fondamentali che lo costituiscono; successivamente si mostrerà quali sono le parti che incidono maggiormente nei consumi, e come si devono effettuare le misurazioni per avere dei valori affidabili attraverso la rilevazione del PUE, unità di misura che valuta l’efficienza di un data center. Dal terzo capitolo si elencheranno le varie tecniche esistenti e in uso per risolvere il problema dell’efficienza energetica, mostrando alla fine una breve analisi sui metodi che hanno utilizzato le maggiori imprese del settore per risolvere il problema dei consumi nei loro data center. Lo scopo di questo elaborato è quello di capire quali sono le tecniche e le strategie per poter ridurre i consumi e aumentare l’efficienza energetica dei data center.

Factors predicting mortality after tips for refractory ascites: a single center experience

Introduction: Transjugular intrahepatic porto-systemic shunt (TIPS) is an accepted indication for treating refractory ascites. Different models have been proposed for the prediction of survival after TIPS; aim of present study was to evaluate the factors associated with mortality after TIPS for refractory ascites. Methods: Seventy-three consecutive patients undergoing a TIPS for refractory ascites in our centre between 2003 and 2008, were prospectively recorded in a database ad were the subject of the study. Mean follow-up was 17±2 months. Forty patients were awaiting liver transplantation (LT) and 12 (16.4%) underwent LT during follow-up. Results: Mean MELD at the moment of TIPS was 15.7±5.3. Overall mortality was 23.3% (n=17) with a mean survival after TIPS of 17±14 months. MELD score (B=0.161, p=0.042), AST (B= 0.020, p=0.090) and pre-TIPS HVPG (B=0.016, p=0.093) were independent predictors of overall mortality. On multivariate analysis MELD (B=0.419, p=0.018) and pre-TIPS HVPG (B=0.223, p=0.060) independently predicted 1 year survival. Patients were stratified into categories of death risk, using ROC curves for the variables MELD and HVPG. Patients with MELD<10 had a low probability of death after TIPS (n=6, 16% mortality); patients with HVPG <16 mmHg (n=6) had no mortality. Maximum risk of death was found in patients with MELD score 19 (n=16, 31% mortality) and in those with HVPG 25 mmHg (n=27, 26% mortality). Conclusions: TIPS increases overall survival in patients with refractory ascites. Liver function (assessed by MELD), necroinflammation (AST) and portal hypertension (HVPG) are independent predictors of survival; patients with MELD>19 and HVPG>25 mmHg are at highest risk of death after TIPS

Development of a new galaxy classification technique and its application to the zCOSMOS survey

The purpose of this Thesis is to develop a robust and powerful method to classify galaxies from large surveys, in order to establish and confirm the connections between the principal observational parameters of the galaxies (spectral features, colours, morphological indices), and help unveil the evolution of these parameters from $z \sim 1$ to the local Universe. Within the framework of zCOSMOS-bright survey, and making use of its large database of objects ($\sim 10\,000$ galaxies in the redshift range $0 < z \lesssim 1.2$) and its great reliability in redshift and spectral properties determinations, first we adopt and extend the \emph{classification cube method}, as developed by Mignoli et al. (2009), to exploit the bimodal properties of galaxies (spectral, photometric and morphologic) separately, and then combining together these three subclassifications. We use this classification method as a test for a newly devised statistical classification, based on Principal Component Analysis and Unsupervised Fuzzy Partition clustering method (PCA+UFP), which is able to define the galaxy population exploiting their natural global bimodality, considering simultaneously up to 8 different properties. The PCA+UFP analysis is a very powerful and robust tool to probe the nature and the evolution of galaxies in a survey. It allows to define with less uncertainties the classification of galaxies, adding the flexibility to be adapted to different parameters: being a fuzzy classification it avoids the problems due to a hard classification, such as the classification cube presented in the first part of the article. The PCA+UFP method can be easily applied to different datasets: it does not rely on the nature of the data and for this reason it can be successfully employed with others observables (magnitudes, colours) or derived properties (masses, luminosities, SFRs, etc.). The agreement between the two classification cluster definitions is very high. ``Early'' and ``late'' type galaxies are well defined by the spectral, photometric and morphological properties, both considering them in a separate way and then combining the classifications (classification cube) and treating them as a whole (PCA+UFP cluster analysis). Differences arise in the definition of outliers: the classification cube is much more sensitive to single measurement errors or misclassifications in one property than the PCA+UFP cluster analysis, in which errors are ``averaged out'' during the process. This method allowed us to behold the \emph{downsizing} effect taking place in the PC spaces: the migration between the blue cloud towards the red clump happens at higher redshifts for galaxies of larger mass. The determination of $M_{\mathrm{cross}}$ the transition mass is in significant agreement with others values in literature.

Stellar Relics of the hierarchical assembly of the Galaxy

This PhD Thesis is part of a long-term wide research project, carried out by the "Osservatorio Astronomico di Bologna (INAF-OABO)", that has as primary goal the comprehension and reconstruction of formation mechanism of galaxies and their evolution history. There is now substantial evidence, both from theoretical and observational point of view, in favor of the hypothesis that the halo of our Galaxy has been at least partially, built up by the progressive accretion of small fragments, similar in nature to the present day dwarf galaxies of the Local Group. In this context, the photometric and spectroscopic study of systems which populate the halo of our Galaxy (i.e. dwarf spheroidal galaxy, tidal streams, massive globular cluster, etc) permits to discover, not only the origin and behaviour of these systems, but also the structure of our Galactic halo, combined with its formation history. In fact, the study of the population of these objects and also of their chemical compositions, age, metallicities and velocity dispersion, permit us not only an improvement in the understanding of the mechanisms that govern the Galactic formation, but also a valid indirect test for cosmological model itself. Specifically, in this Thesis we provided a complete characterization of the tidal Stream of the Sagittarius dwarf spheroidal galaxy, that is the most striking example of the process of tidal disruption and accretion of a dwarf satellite in to our Galaxy. Using Red Clump stars, extracted from the catalogue of the Sloan Digital Sky Survey (SDSS) we obtained an estimate of the distance, the depth along the line of sight and of the number density for each detected portion of the Stream (and more in general for each detected structure along our line of sight). Moreover comparing the relative number (i.e. the ratio) of Blue Horizontal Branch stars and Red Clump stars (the two features are tracers of different age/different metallicity populations) in the main body of the galaxy and in the Stream, in order to verify the presence of an age-metallicity gradient along the Stream. We also report the detection of a population of Red Clump stars probably associated with the recently discovered Bootes III stellar system. Finally, we also present the results of a survey of radial velocities over a wide region, extending from r ~ 10' out to r ~ 80' within the massive star cluster Omega Centauri. The survey was performed with FLAMES@VLT, to study the velocity dispersion profile in the outer regions of this stellar system. All the results presented in this Thesis, have already been published in refeered journals.

X-ray and lensing mass estimates in galaxy clusters

In this Thesis we have presented our work on the analysis of galaxy clusters through their X-ray emission and the gravitational lensing effect that they induce. Our research work was mainly finalised to verify and possibly explain the observed mismatch between the galaxy cluster mass distributions estimated through two of the most promising techniques, i.e. the X-ray and the gravitational lensing analyses. Moreover, it is an established evidence that combined, multi-wavelength analyses are extremely effective in addressing and explaining the open issues in astronomy: however, in order to follow this approach, it is crucial to test the reliability and the limitations of the individual analysis techniques. In this Thesis we also assessed the impact of some factors that could affect both the X-ray and the strong lensing analyses.

Sviluppo di un simulatore per la propagazione del calore nei data center

Questa tesi tratta lo sviluppo di un software in grado di simulare le dinamiche tra fluidi e oggetti considerando la propagazione del calore in vista di possibili applicazioni rivolte ad ambienti in cui lo stato termico del sistema e' critico (data center).

Early-type galaxies as probes of galaxy formation and cosmology

The goal of this thesis is to analyze the possibility of using early-type galaxies to place evolutionary and cosmological constraints, by both disentangling what is the main driver of ETGs evolution between mass and environment, and developing a technique to constrain H(z) and the cosmological parameters studying the ETGs age-redshift relation. The (U-V) rest-frame color distribution is studied as a function of mass and environment for two sample of ETGs up to z=1, extracted from the zCOSMOS survey with a new selection criterion. The color distributions and the slopes of the color-mass and color-environment relations are studied, finding a strong dependence on mass and a minor dependence on environment. The spectral analysis performed on the D4000 and Hδ features gives results validating the previous analysis. The main driver of galaxy evolution is found to be the galaxy mass, the environment playing a subdominant but non negligible role. The age distribution of ETGs is also analyzed as a function of mass, providing strong evidences supporting a downsizing scenario. The possibility of setting cosmological constraints studying the age-redshift relation is studied, discussing the relative degeneracies and model dependencies. A new approach is developed, aiming to minimize the impact of systematics on the “cosmic chronometer” method. Analyzing theoretical models, it is demonstrated that the D4000 is a feature correlated almost linearly with age at fixed metallicity, depending only minorly on the models assumed or on the SFH chosen. The analysis of a SDSS sample of ETGs shows that it is possible to use the differential D4000 evolution of the galaxies to set constraints to cosmological parameters in an almost model-independent way. Values of the Hubble constant and of the dark energy EoS parameter are found, which are not only fully compatible, but also with a comparable error budget with the latest results.

Hydrodynamical simulations of galaxy clusters in dark energy cosmologies

In this work we investigate the influence of dark energy on structure formation, within five different cosmological models, namely a concordance $\Lambda$CDM model, two models with dynamical dark energy, viewed as a quintessence scalar field (using a RP and a SUGRA potential form) and two extended quintessence models (EQp and EQn) where the quintessence scalar field interacts non-minimally with gravity (scalar-tensor theories). We adopted for all models the normalization of the matter power spectrum $\sigma_{8}$ to match the CMB data. For each model, we perform hydrodynamical simulations in a cosmological box of $(300 \ {\rm{Mpc}} \ h^{-1})^{3}$ including baryons and allowing for cooling and star formation. We find that, in models with dynamical dark energy, the evolving cosmological background leads to different star formation rates and different formation histories of galaxy clusters, but the baryon physics is not affected in a relevant way. We investigate several proxies for the cluster mass function based on X-ray observables like temperature, luminosity, $M_{gas}$, and $Y_{X}$. We confirm that the overall baryon fraction is almost independent of the dark energy models within few percentage points. The same is true for the gas fraction. This evidence reinforces the use of galaxy clusters as cosmological probe of the matter and energy content of the Universe. We also study the $c-M$ relation in the different cosmological scenarios, using both dark matter only and hydrodynamical simulations. We find that the normalization of the $c-M$ relation is directly linked to $\sigma_{8}$ and the evolution of the density perturbations for $\Lambda$CDM, RP and SUGRA, while for EQp and EQn it depends also on the evolution of the linear density contrast. These differences in the $c-M$ relation provide another way to use galaxy clusters to constrain the underlying cosmology.

Spektroelektrochemische Untersuchungen mittels oberflächenverstärkter Infrarotabsorptionsspektroskopie (SEIRAS) an Multi-Redox-Center-Proteinen in einer biomimetischen Membranumgebung

Die optische Eigenschaften sowie der Oberflächenverstärkungseffekt von rauen Metalloberflächen sowie Nanopartikeln wurden intensiv für den infraroten Bereich des Spektrums in der Literatur diskutiert. Für die Präparation solcher Oberflächen gibt es prinzipiell zwei verschiedene Strategien, zum einen können die Nanopartikel zuerst ex-situ synthetisiert werden, der zweite Ansatz beruht darauf, dass die Nanopartikel in-situ hergestellt und aufgewachsen werden. Hierbei wurden beide Ansätze ausgetestet, dabei stellte sich heraus, dass man nur mittels der in-situ Synthese der Goldnanopartikel in der Lage ist nanostrukturierte Oberflächen zu erhalten, welche elektronisch leitfähig sind, nicht zu rau sind, um eine Membranbildung zu ermöglichen und gleichzeitig einen optimalen Oberflächenverstärkungseffekt zeigen. Obwohl keine ideale Form der Nanopartikel mittels der in-situ Synthese erhalten werden können, verhalten sich diese dennoch entsprechend der Theorie des Oberflächenverstärkungseffekts. Optimierungen der Form und Grösse der Nanopartikel führten in dieser Arbeit zu einer Optimierung des Verstärkungseffekts. Solche optimierten Oberflächen konnten einfach reproduziert werden und zeichnen sich durch eine hohe Stabilität aus. Der so erhaltene Oberflächenverstärkungseffekt beträgt absolut 128 verglichen mit dem belegten ATR-Kristall ohne Nanopartikel oder etwa 6 mal, verglichen mit der Oberfläche, die bis jetzt auch in unserer Gruppe verwendet wurde. Daher können nun Spektren erhalten werden, welche ein deutlich besseres Signal zu Rauschverhältnis (SNR) aufweisen, was die Auswertung und Bearbeitung der erhaltenen Spektren deutlich vereinfacht und verkürzt.rnNach der Optimierung der verwendeten Metalloberfläche und der verwendeten Messparameter am Beispiel von Cytochrom C wurde nun an der Oberflächenbelegung der deutlich größeren Cytochrom c Oxidase gearbeitet. Hierfür wurde der DTNTA-Linker ex-situ synthetisiert. Anschließend wurden gemischte Monolagen (self assembeld monolayers) aus DTNTA und DTP hergestellt. Die NTA-Funktionalität ist für die Anbindung der CcO mit der his-tag Technologie verantwortlich. Die Kriterien für eine optimale Linkerkonzentration waren die elektrischen Parameter der Schicht vor und nach Rekonstitution in eine Lipidmembran, sowie Elektronentransferraten bestimmt durch elektrochemische Messungen. Erst mit diesem optimierten System, welches zuverlässig und reproduzierbar funktioniert, konnten weitere Messungen an der CcO begonnen werden. Aus elektrochemischen Messungen war bekannt, dass die CcO durch direkten Elektronentransfer unter Sauerstoffsättigung in einen aktivierten Zustand überführt werden kann. Dieser aktivierte Zustand zeichnet sich durch eine Verschiebung der Redoxpotentiale um etwa 400mV gegenüber dem aus Gleichgewichts-Titrationen bekannten Redoxpotential aus. Durch SEIRAS konnte festgestellt werden, dass die Reduktion bzw. Oxidation aller Redoxzentren tatsächlich bei den in der Cyclovoltammetrie gemessenen Potentialen erfolgt. Außerdem ergaben die SEIRA-Spektren, dass durch direkten Elektronentransfer gravierende Konformationsänderungen innerhalb des Proteins stattfinden. rnBisher war man davon ausgegangen, aufgrund des Elektronentransfers mittels Mediatoren, dass nur minimale Konformationsänderungen beteiligt sind. Vor allem konnte erstmaligrnder aktivierte und nicht aktivierte Zustand der Cytochrom c Oxidase spektroskopisch nachweisen werden.rn

Riorganizzazione di un distribution center mediante le tecniche di lean production: il caso Gambro Dasco spa

La Lean Production è un tema di estrema attualità per tutte le aziende che abbiano compreso l’importanza di produrre di più, con le risorse che si hanno a disposizione, eliminando sistematicamente tutte le attività che non creano valore aggiunto. La Produzione Snella è diventato un metodo per incrementare la competitività, riducendo l’incertezza e aumentando il servizio fornito al cliente. Nella realtà attuale vi è ancora una scarsa diffusione dei concetti Lean. Le cause di questo problema sono imputabili soprattutto alla cultura del management aziendale, alla mancanza di efficaci strumenti tecnologici a supporto, e in alcuni casi, la scarsa disponibilità delle imprese ad abbracciare la filosofica “snella”. La presente tesi, dopo una panoramica introduttiva su l’origine e l’evoluzione del Pensiero Snello e l’analisi di tutti i tools disponibili per combattere lo spreco; si propone di analizzare l’applicazione degli stessi in Gambro Dasco, multinazionale biomedicale leader nella vendita delle sue apparecchiature per dialisi.

Hydrodynamical simulations of early-type galaxies: effects of galaxy shape and stellar dynamics on hot coronae

Early-Type galaxies (ETGs) are embedded in hot (10^6-10^7 K), X-ray emitting gaseous haloes, produced mainly by stellar winds and heated by Type Ia supernovae explosions, by the thermalization of stellar motions and occasionally by the central super-massive black hole (SMBH). In particular, the thermalization of the stellar motions is due to the interaction between the stellar and the SNIa ejecta and the hot interstellar medium (ISM) already residing in the ETG. A number of different astrophysical phenomena determine the X-ray properties of the hot ISM, such as stellar population formation and evolution, galaxy structure and internal kinematics, Active Galactic Nuclei (AGN) presence, and environmental effects. With the aid of high-resolution hydrodynamical simulations performed on state-of-the-art galaxy models, in this Thesis we focus on the effects of galaxy shape, stellar kinematics and star formation on the evolution of the X-ray coronae of ETGs. Numerical simulations show that the relative importance of flattening and rotation are functions of the galaxy mass: at low galaxy masses, adding flattening and rotation induces a galactic wind, thus lowering the X-ray luminosity; at high galaxy masses the angular momentum conservation keeps the central regions of rotating galaxies at low density, whereas in non-rotating models a denser and brighter atmosphere is formed. The same dependence from the galaxy mass is present in the effects of star formation (SF): in light galaxies SF contributes to increase the spread in Lx, while at high galaxy masses the halo X-ray properties are marginally sensitive to SF effects. In every case, the star formation rate at the present epoch quite agrees with observations, and the massive, cold gaseous discs are partially or completely consumed by SF on a time-scale of few Gyr, excluding the presence of young stellar discs at the present epoch.

Radio halos in a mass-selected sample of galaxy clusters

A fraction of galaxy clusters host Mpc-scale Radio Halos (RH), generated by ultrarelativistic electrons in the magnetized intra cluster medium (ICM). In the current view they trace turbulent regions in merging clusters, where relativistic particles are trapped and accelerated. This model has clear expectations about the statistical properties of RHs. To test these expectations large mass-selected samples of galaxy clusters with adequate radio and X-ray data are necessary. We used the Planck SZ cluster catalogue as suitable starting point of our investigation, selecting clusters with M500>6x10^14 Msun at 0.08