Non-hierarchical cluster analysis for body weight, age at first egg, egg production and egg weight in a laying hen strain.

2016

Sintesi e caratterizzazione di cluster Ag-Cu-Fe, Au-Cu-Fe e Ni-Pd

Durante il mio periodo di tirocinio mi sono occupato della sintesi e caratterizzazione di cluster carbonilici eterometallici, ed in particolare di cluster Ag-Cu-Fe, Au-Cu-Fe, e Ni-Pd. In un primo momento il lavoro si è concentrato sullo studio della reazione tra cluster Cu-Fe e sali di Ag e Au, con lo scopo di ottenere specie Ag-Cu-Fe, e Au-Cu-Fe. Nella seconda parte l’attività è stata incentrata sulla sintesi di cluster Ni-Pd ad elevata nuclearità, attraverso reazioni tra [Ni6(CO)12]2- e composti di Pd(II). In entrambi i casi le sintesi sono state condotte variando i rapporti stechiometrici dei reagenti e i solventi, permettendo l’ottenimento di specie, caratterizzate spettroscopicamente mediante tecnica IR. In alcuni casi è stato anche possibile ottenere cristalli caratterizzati strutturalmente tramite diffrattometria a raggi X. Le reazioni di [Cu3Fe3(CO)12]3- con quantità crescenti di M=Ag, Au danno luogo alla formazione in sequenza di [Cu5Fe4(CO)16]3-, [MxCu5-xFe4(CO)16]3- (x = 0-5), [M5Fe4(CO)16]3-, [M6Fe4(CO)16]2-. Successivamente, nel caso in cui M= Ag, un ulteriore aggiunta di sali di M+ porta alla formazione di [Ag13Fe8(CO)32]3-, mentre se M= Au si formano i cosiddetti “bruni d’oro” e alla fine, [AuFe4(CO)16]-. Le specie [MxCu5-xFe4(CO)16]3- risultano particolarmente interessanti dato che possono essere viste come leghe molecolari M/Cu, che mostrano disordine sia sostituzionale che composizionale. Per quanto riguarda i cluster Ni-Pd sono state ottenute tre nuove specie carboniliche ad elevata nuclearità, ovvero [Ni37-xPd7+x(CO)48]6- (x= 0,69), [HNi37-xPd7+x(CO)48]5- (x= 0,53) and [Ni22-xPd20+x(CO)48]6- (x = 0.63). In tutte queste strutture il Pd tende ad occupare posizioni che minimizzano le interazioni Pd-CO massimizzando le interazioni M-M, mentre l’opposto risulta per il Ni. Ciò si traduce in una parziale segregazione dei due metalli, anche se alcuni fenomeni di disordine (sostituzionale e composizionale) sono presenti in tali strutture.

Sintesi e studio dell'attività catalitica, in reazioni di idrogenazione e trasferimento di idrogeno, di cluster carbonilici idrurici di rutenio e iridio

Il presente elaborato finale è incentrato sulla sintesi, caratterizzazione e studio della reattività di nuovi cluster idrurici carbonilici di rutenio e iridio a bassa nuclearità; inoltre, l’attività catalitica di suddetti cluster è stata valutata in modo preliminare in reazioni di idrogenazione e trasferimento di idrogeno. In particolare è stata ottimizzata la sintesi del composto [NEt4][H2Ru3Ir(CO)12] (2), cluster principale dello studio catalitico, e sono stati sintetizzati altri cinque cluster bimetallici Ru-Ir di cui non risulta nota la struttura in letteratura: [H3Ru3Ir(CO)12] (3), [PPN]2[H2Ru3Ir(CO)12] (4a) ([PPN]+= [N(PPh3)2]+), [NEt4][HRu3Ir2(CO)12(COD)] (5) (COD = C8H12) e [H2Ru3Ir2(CO)10(COD)2]-[HRu2Ir3(CO)12(COD)2] (miscela 1:1) (6). Tutte le specie ottenute sono state caratterizzate mediante diffrazione a raggi X su cristallo singolo (SC-XRD), spettrometria di massa ESI-MS, spettroscopia IR e 1H-NMR. Il cluster 2 è risultato attivo nella reazione di idrogenazione di doppi legami polari mediante meccanismo di H transfer, utilizzando iPrOH come fonte di idrogeno, e 4-fluoro acetofenone come substrato modello; inoltre, con l'utilizzo di un'autoclave, si sono condotte prove di idrogenazione sotto pressione di idrogeno molecolare H2 utilizzando come substrato trans-cinnamaldeide, al fine di valutare l'effetto del catalizzatore sia in presenza di gruppi C=O che di un doppio legame C=C (aldeide α,β insatura).

Studio della reattività di cluster carbonilici di Rh con sali di Au(I)

Il progetto di tesi si è focalizzato sullo studio della reattività del cluster carbonilico [Rh7(CO)16]3- in presenza del sale Au(Et2S)Cl. Ogni reazione investigata è stata svolta in atmosfera controllata di CO, modificando i rapporti stechiometrici tra il precursore e il sale di Au(I) in diversi solventi. Inizialmente si è tentato di riprodurre la sintesi del cluster bimetallico [Rh20Au7(CO)45]5- già noto, utilizzando Au(Et2S)Cl. Si è poi amplificato lo studio con l’obiettivo principale di sintetizzare nuovi cluster bimetallici ad alta nuclearità. È stato ottenuto un composto nuovo analizzato tramite diffrattometria ai raggi X a cristallo singolo: [Rh22Au3(CO)x]n-. Tramite i dati cristallografici è stato possibile definirne la sola struttura metallica, e nonostante i diversi tentativi, il composto non ha prodotto cristalli migliori per una completa caratterizzazione. Viste le quantità significative di sottoprodotti a bassa nuclearità ottenute nelle reazioni studiate, parallelamente sono state condotte prove di recupero del rodio in quanto metallo prezioso. Infine, è stato ottimizzato un metodo per separare due specie già note con carica negativa simile, [Rh10Au(CO)26]3- e [Rh16Au6(CO)36]4-. Tutti i composti sono stati caratterizzati tramite spettroscopia IR, mentre sul nuovo cluster è stata effettuata anche un’analisi alla spettrometria di massa.

Exploring the internal kinematics of Galactic Globular Cluster cores

Globular clusters (GCs) are traditionally described as simple quasi-relaxed non-rotating stellar systems, characterized by spherical symmetry and isotropy in velocity space. However, recent studies have shown deviations from isotropic velocity distributions and significant internal rotation in many GCs, suggesting that their internal structure and kinematics are more complex than previously thought. The aim of this thesis is to investigate the internal kinematics of Galactic Globular Clusters (GGCs) as part of the Multi-Instrument Kinematic Survey (MIKiS), which exploits the capabilities of different ESO-VLT spectrographs to obtain comprehensive velocity dispersion (VD) and rotation profiles of GGCs. Moreover, this thesis has the particular goal of unraveling the kinematics of GC cores, which are still largely unexplored, by taking advantage of the exceptional spatial resolution of the adaptive-optics assisted integral-field spectrograph MUSE/NFM. The thesis presents a thorough kinematic study of three GGCs NGC 1904, NGC 6440, and NGC 6569. By combining the data sets acquired with four different spectrographs, we obtained the radial velocity (RV) of more than 1000 individual stars in each cluster, sampling from the innermost to the outermost regions. This allowed us to obtain the entire VD profile of each cluster and exclude the presence of an intermediate-mass black hole in the core of NGC 1904, at odds with previous findings obtained from integrated-light spectra. The studies also revealed signatures of internal rotation in each of the GCs studied. These results, supported by those of N-body simulations, prove that GCs were born with a significant initial rotation that they gradually lost through internal two-body relaxation and angular momentum loss carried away by escaping stars. Furthermore, we derived the structural parameters of NGC 6440 and NGC 6569, obtaining a comprehensive overview of the internal kinematics and structure of these GCs, which is necessary to properly reconstruct the evolutionary history of these systems.

New indicators of star cluster dynamical evolution

This thesis presents a study of globular clusters (GCs), based on analysis of Monte Carlo simulations of globular clusters (GCs) with the aim to define new empirical parameters measurable from observations and able to trace the different phases of their dynamical evolution history. During their long term dynamical evolution, due to mass segregation and and dynamical friction, massive stars transfer kinetic energy to lower-mass objects, causing them to sink toward the cluster center. This continuous transfer of kinetic energy from the core to the outskirts triggers the runaway contraction of the core, known as "core collapse" (CC), followed by episodes of expansion and contraction called gravothermal oscillations. Clearly, such an internal dynamical evolution corresponds to significant variations also of the structure of the system. Determining the dynamical age of a cluster can be challenging as it depends on various internal and external properties. The traditional classification of GCs as CC or post-CC systems relies on detecting a steep power-law cusp in the central density profile, which may not always be reliable due to post-CC oscillations or other processes. In this thesis, based on the normalized cumulative radial distribution (nCRD) within a fraction of the half-mass radius is analyzed, and three diagnostics (A5, P5, and S2.5) are defined. These diagnostics show sensitivity to dynamical evolution and can distinguish pre-CC clusters from post-CC clusters.The analysis performed using multiple simulations with different initial conditions, including varying binary fractions and the presence of dark remnants showed the time variations of the diagnostics follow distinct patterns depending on the binary fraction and the retention or ejection of black holes. This analysis is extended to a larger set of simulations matching the observed properties of Galactic GCs, and the parameters show a potential to distinguish the dynamical stages of the observed clusters as well.

Galaxy cluster cosmology in KiDS, Planck, and Euclid surveys

In this Thesis, we present a series of works that encompass the fundamental steps of cosmological analyses based on galaxy clusters, spanning from mass calibration to deriving cosmological constraints through counts and clustering. Firstly, we focus on the 3D two-point correlation function (2PCF) of the galaxy cluster sample by Planck Collaboration XXVII (2016). The masses of these clusters are expected to be underestimated, as they are derived from a scaling relation calibrated through X-ray observations. We derived a mass bias which disagrees with simulation predictions, consistent with what derived by Planck Collaboration VI (2020). Furthermore, in this Thesis we analyse the cluster counts and 2PCF, respectively, of the photometric galaxy cluster sample developed by Maturi et al. (2019), based on the third data release of KiDS (KiDS-DR3, de Jong et al. 2017). We derived constraints on fundamental cosmological parameters which are consistent and competitive, in terms of uncertainties, with other state-of-the-art cosmological analyses. Then, we introduce a novel approach to establish galaxy colour-redshift relations for cluster weak-lensing analyses, regardless of the specific photometric bands in use. This method optimises the selection completeness of cluster background galaxies while maintaining a defined purity threshold. Based on the galaxy sample by Bisigello et al. (2020), we calibrated two colour selections, one relying on the ground-based griz bands, and the other including the griz and Euclid YJH bands. In addition, we present the preliminary work on the weak-lensing mass calibration of the clusters detected by Maturi et al. (in prep.) in the fourth data release of KiDS (KiDS-1000, Kuijken et al. 2019). This mass calibration will enable the cosmological analyses based on cluster counts and clustering, from which we expect remarkable improvements in the results compared to those derived in KiDS-DR3.

Investigating the origin of radio emission from the intra-cluster bridge A399-A401

Radio bridges are a newly observed class of phenomena, they are large scale filamentary structures that span between pairs of clusters in a pre-merger phase. In my Thesis, starting from the observed synchrotron emission in the bridge A399-A401, I apply a Fermi I shock re-acceleration model under different conditions to the bridge. The purpose of my work is to check the likelihood of the above mentioned model. In particular the Inverse Compton emission that the model predicts is above the current observational constraints on Inverse Compton for the bridge A399-A401, this means that a Fermi I re-acceleration model is unlikely to describe the emission from the bridge, while a Fermi II turbulent re-acceleration model could still explain the origin of the emission in the bridge.

Dynamics of galaxies in the cluster environment: a resonant origin for the ISP?

The internal dynamics of elliptical galaxies in clusters depends on many factors, including the environment in which the galaxy is located. In addition to the strong encounters with the other galaxies, we can also consider the gravitational interaction with the ubiquitous Cluster Tidal Field (CTF). As recognized in many studies, one possible way in which CTF affects the dynamics of galaxies inside the cluster is related to the fact that they may start oscillating as “rigid bodies” around their equilibrium positions in the field, with the periods of these oscillations curiously similar to those of stellar orbits in the outer parts of galaxies. Resonances between the two motions are hence expected and this phenomenon could significantly contribute to the formation of the Intracluster Stellar Population (ISP), whose presence is abundantly confirmed by observations. In this thesis work, we propose to study the motion of an elliptical galaxy, modelled as a rigid body, in the CTF, especially when its center of mass traces a quasi-circular orbit in the cluster gravitational potential. This case extends and generalizes the previous models and findings, proceeding towards a much more realistic description of galaxy motion. In addition to this, the presence of a further oscillation, namely that of the entire galaxy along its orbit, will possibly increase the probability of having resonances and, consequently, the rate of ISP production nearly to observed values. Thus, after reviewing the dynamics of a rigid body in a generic force field, we will assess some physically relevant studies and report their main results, discussing their implications with respect to our problem. We will conclude our discussion focusing on the more realistic scenario of an elliptical galaxy whose center of mass moves on a quasi-circular orbit in a spherically symmetric potential. The derivation of the fundamental equations of motion will serve as the basis for future modelling and discussions.

analisi delle prestazioni del cluster risc-v: monte cimone

Gli sforzi di ricerca relativi all'High Performance Computing, nel corso degli anni, hanno prodotto risultati importanti inerenti all'incremento delle prestazioni sia in termini di numero di operazioni effettuate per periodo temporale, sia introducendo o migliorando algoritmi paralleli presenti in letteratura. Tali traguardi hanno comportato cambiamenti alla struttura interna delle macchine; si è assistito infatti ad un'evoluzione delle architetture dei processori utilizzati e all'impiego di GPU come risorse di calcolo aggiuntive. La conseguenza di un continuo incremento di prestazioni è quella di dover far fronte ad un grosso dispendio energetico, in quanto le macchine impiegate nell'HPC sono ideate per effettuare un'intensa attività di calcolo in un periodo di tempo molto prolungato; l'energia necessaria per alimentare ciascun nodo e dissipare il calore generato comporta costi elevati. Tra le varie soluzioni proposte per limitare il consumo di energia, quella che ha riscosso maggior interesse, sia a livello di studio che di mercato, è stata l'integrazione di CPU di tipologia RISC (Reduced Instruction Set Computer), in quanto capaci di ottenere prestazioni soddisfacenti con un impiego energetico inferiore rispetto alle CPU CISC (Complex Instruction Set Computer). In questa tesi è presentata l'analisi delle prestazioni di Monte Cimone, un cluster composto da 8 nodi di calcolo basati su architettura RISC-V e distribuiti in 4 piattaforme (\emph{blade}) dual-board. Verranno eseguiti dei benchmark che ci permetteranno di valutare: le prestazioni dello scambio di dati a lunga e corta distanza; le prestazioni nella risoluzione di problemi che presentano un principio di località spaziale ridotto; le prestazioni nella risoluzione di problemi su grafi e, nello specifico, ricerca in ampiezza e cammini minimi da sorgente singola.

Gravitational microscope in MACSJ1206: unveiling galaxy cluster member mass distribution

Gravitational lensing is a powerful tool to investigate the properties of the distribution of matter, be it barionic or dark. In this work we take advantage of Strong Gravitational Lensing to infer the properties of one of the galaxy-scale substructures that makes up the cluster MACSJ1206. It is relatively easy to model the morphology of the visible components of a galaxy, while the morphology of the dark matter distribution cannot be so easily constrained. Being sensitive to the whole mass, strong lensing provides a way to probe DM distribution, and this is the reason why it is the best tool to study the substructure. The goal of this work consists of performing an analysis of the substructure previously mentioned, an early type galaxy (ETG), by analyzing the highly magnified Einstein ring around it, in order to put stringent constraints on its matter distribution, that, for an ETG, is commonly well described by an isothermal profilele. This turns out to be interesting for three main different reasons. It is well known that galaxies in clusters are subject to interaction processes, both dynamic and hydrodynamic, that can significantly modify the distribution of matter within them. Therefore, finding a different profile from the one usually expected could be a sign that the galaxy has undergone processes that have changed its structure. Studying the mass distribution also means studying the dark matter component, which not only still presents great questions today, but which is also not obviously distributed in the same way as in an isolated galaxy. What emerges from the analysis is that the total mass distribution of the galaxy under examination turns out to have a slope much steeper than the isothermal usually expected.

Stellar mass loss from the Fornax dwarf spheroidal galaxy

Dwarf galaxies often experience gravitational interactions from more massive companions. These interactions can deform galaxies, turn star formation on or off, or give rise to mass loss phenomena. In this thesis work we propose to study, through N-body simulations, the stellar mass loss suffered by the dwarf spheroid galaxy (dSph) Fornax orbiting in the Milky Way gravitational potential. Which is a key phenomenon to explain the mass budget problem: the Fornax globular clusters together have a stellar mass comparable to that of Fornax itself. If we look at the stellar populations which they are made of and we apply the scenarios of stellar population formation we find that, originally, they must have been >= 5 times more massive. For this reason, they must have lost or ejected stars through dynamic interactions. However, as presented in Larsen et al (2012), field stars alone are not sufficient to explain this scenario. We may assume that some of those stars fell into Fornax, and later were stripped by Milky Way. In order to study this solution we built several illustrative single component simulations, with a tabulated density model using the P07ecc orbit studied from Battaglia et al (2015). To divide the single component into stellar and dark matter components we have defined a posterior the probability function P(E), where E is the initial energy distribution of the particles. By associating each particle with a fraction of stellar mass and dark matter. In this way we built stellar density profiles without repeating simulations. We applied the method to Fornax using the profile density tables obtained in Pascale et al (2018) as observational constraints and to build the model. The results confirm the results previously obtained with less flexible models by Battaglia et al (2015). They show a stellar mass loss < 4% within 1.6 kpc and negligible within 3 kpc, too small to solve the mass budget problem.

The Burden Of Eclampsia: Results From A Multicenter Study On Surveillance Of Severe Maternal Morbidity In Brazil.

Maternal mortality (MM) is a core indicator of disparities in women's rights. The study of Near Miss cases is strategic to identifying the breakdowns in obstetrical care. In absolute numbers, both MM and occurrence of eclampsia are rare events. We aim to assess the obstetric care indicators and main predictors for severe maternal outcome from eclampsia (SMO: maternal death plus maternal near miss). Secondary analysis of a multicenter, cross-sectional study, including 27 centers from all geographic regions of Brazil, from 2009 to 2010. 426 cases of eclampsia were identified and classified according to the outcomes: SMO and non-SMO. We classified facilities as coming from low- and high-income regions and calculated the WHO's obstetric health indicators. SPSS and Stata softwares were used to calculate the prevalence ratios (PR) and respective 95% confidence interval (CI) to assess maternal characteristics, clinical and obstetrical history, and access to health services as predictors for SMO, subsequently correlating them with the corresponding perinatal outcomes, also applying multiple regression analysis (adjusted for cluster effect). Prevalence of and mortality indexes for eclampsia in higher and lower income regions were 0.2%/0.8% and 8.1%/22%, respectively. Difficulties in access to health care showed that ICU admission (adjPR 3.61; 95% CI 1.77-7.35) and inadequate monitoring (adjPR 2.31; 95% CI 1.48-3.59) were associated with SMO. Morbidity and mortality associated with eclampsia were high in Brazil, especially in lower income regions. Promoting quality maternal health care and improving the availability of obstetric emergency care are essential actions to relieve the burden of eclampsia.

Delays In Receiving Obstetric Care And Poor Maternal Outcomes: Results From A National Multicentre Cross-sectional Study.

The vast majority of maternal deaths in low-and middle-income countries are preventable. Delay in obtaining access to appropriate health care is a fairly common problem which can be improved. The objective of this study was to explore the association between delay in providing obstetric health care and severe maternal morbidity/death. This was a multicentre cross-sectional study, involving 27 referral obstetric facilities in all Brazilian regions between 2009 and 2010. All women admitted to the hospital with a pregnancy-related cause were screened, searching for potentially life-threatening conditions (PLTC), maternal death (MD) and maternal near-miss (MNM) cases, according to the WHO criteria. Data on delays were collected by medical chart review and interview with the medical staff. The prevalence of the three different types of delays was estimated according to the level of care and outcome of the complication. For factors associated with any delay, the PR and 95%CI controlled for cluster design were estimated. A total of 82,144 live births were screened, with 9,555 PLTC, MNM or MD cases prospectively identified. Overall, any type of delay was observed in 53.8% of cases; delay related to user factors was observed in 10.2%, 34.6% of delays were related to health service accessibility and 25.7% were related to quality of medical care. The occurrence of any delay was associated with increasing severity of maternal outcome: 52% in PLTC, 68.4% in MNM and 84.1% in MD. Although this was not a population-based study and the results could not be generalized, there was a very clear and significant association between frequency of delay and severity of outcome, suggesting that timely and proper management are related to survival.

Last Instar Larvae And Pupae Of Ourocnemis Archytas And Anteros Formosus (lepidoptera: Riodinidae), With A Summary Of Known Host Plants For The Tribe Helicopini.

Last instar larvae and pupae of Ourocnemis archytas (Lepidoptera: Riodinidae) are described for the first time and compared with those of Anteros formosus, which are also described in detail. Last instars of both species present body covered with long white plumose setae, a row of orange balloon setae on the prothoracic shield, and clusters of perforated cupola organs (PCOs) near the spiracles; differences are the black cephalic capsule, the placement and format of balloon setae cluster, and the presence of enlarged black tips on some plumose setae. Pupae of O. archytas resemble that of Anteros, covered with the last instar setae and with no balloon setae. Characteristics of the immature stages of these two genera could be useful to establish the still unresolved relationship between them. A summary of the host plants of Helicopini is presented, showing a polyphagous pattern for Anteros, recorded in 21 host plant families, which contrasts with the specialized diet observed in Helicopis and Sarota.