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.

La cinematica nel core dell'ammasso globulare NGC 6441 da osservazioni SINFONI

In questo elaborato viene presentata l'analisi cinematica delle regioni centrali di NGC 6441, uno degli ammassi globulari più massivi (M ~10^6 Msol) della nostra Galassia. L'ammasso è stato selezionato, insieme ad altri 18, all'interno dell'ESO Large Program “Unveiling the kinematics in the core of high-density globular clusters with SINFONI" (PI: Ferraro) per cercare evidenze di buchi neri di massa intermedia (IMBH), la cui esistenza è ancora controversa. Poichè la misura della dispersione di velocità da spettri integrati può essere affetta dalla contaminazione di poche stelle brillanti, in questo lavoro si sono misurate le velocità radiali (RV) di stelle individuali, utilizzando lo spettrografo IFU SINFONI dell'ESO, dotato di un sistema di ottiche adattive. Sono state misurate le RV di 709 stelle giganti nei primi 17" dal centro, da cui è stato estratto un sotto-campione di alta qualità di circa 200 stelle. Queste misure sono state poi combinate con un campione di RV nelle regioni più esterne dell'ammasso, ottenute con gli spettrografi multi-oggetto KMOS e FLAMES dell'ESO. Tali dati sono stati utilizzati per il calcolo del profilo di dispersione di velocità e per la ricerca di rotazione lungo l'intera estensione radiale nell'ammasso. I risultati ottenuti sembrano escludere sia l'esistenza di un IMBH, che la presenza di forte rotazione interna. Inoltre hanno evidenziato una significativa decrescita della dispersione di velocita` nelle regioni centrali (parzialmente confermata anche da misure di moti propri ottenute con HST), che potrebbe suggerire la presenza di anisotropia tangenziale nel centro del sistema. Un simile comportamento (sebbene di minore entita`) e’ stato evidenziato in altri ammassi, suggerendo che potrebbe trattarsi di una caratteristica comune in questi sistemi stellari.

Investigating stellar mixing processes through the study of the Red-Giant Branch bump

Extra mixing at the borders of convective zones in stellar interiors takes on an important role in the chemical evolution of stars and galaxies through the transport of chemical elements towards the stellar surface: knowing the overshooting mechanism can therefore lead to a better understanding of the observed chemical abundances in stellar photospheres. The comprehension of this phenomenon is quite uncertain and currently object of many studies. In particular, concerning low mass stars, in the past decades several works highlighted a discrepancy between the observed luminosity of the Red-Giant Branch bump and its prediction from simulations, which can be fixed including overshooting at the base of the convective envelope. This work, studying the Red-Giant Branch bump and using it as a diagnostic for extra mixing processes, tries to classify two different types of overshooting, instantaneous and diffusive, using both simulations from stellar models and Globular Clusters’ data. The aim is to understand which one of the two mixing processes is the most suitable in reproducing the observed stellar behaviour and, in case both of them provide reliable results, what are the conditions under which they produce the same effects on the Red-Giant Branch bump luminosity function and are consequently indistinguishable. Finally, possible dependences of overshooting efficiency on stellar parameters, such as chemical composition, are analysed.

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 0.0833. We cross checked our sample with the NVSS for clusters at z<0.2 and with the Extended GMRT RH Survey for 0.233. We find significant statistical evidence (at 3.26σ) of an increase of the fraction of clusters with RH with the mass of the parent cluster and show that this increase is in line with statistical calculations based on the re-acceleration scenario. We confirm earlier findings that RHs are exclusively found in merging systems.

Temporal variation of genetic diversity and differentiation of albacore, Thunnus alalunga, in the Mediterranean Sea

This study is on albacore (Thunnus alalunga, Bonnaterre 1788), an epi- and mesopelagic oceanic tuna species cosmopolitan in the tropical and temperate waters of all oceans including the Mediterranean Sea, extending in a broad band between 40°N and 40°S. What it’s known about albacore population structure is based on different studies that used fisheries data, RFLP, mtDNA control region and nuDNA markers, blood lectins analysis, individual tags and microsatellite. At the moment, for T. alalunga six management units are recognized: the North Pacific, South Pacific, Indian, North Atlantic, South Atlantic and Mediterranean stocks. In this study I have done a temporal and spatial comparison of genetic variability between different Mediterranean populations of Thunnus alalunga matching an historical dataset ca. from 1920s composed of 43 individuals divided in 3 populations (NADR, SPAIN and CMED) with a modern dataset composed of 254 individuals and 7 populations (BAL, CYP, LIG, TYR, TUR, ADR, ALB). The investigation was possible using a panel of 94 nuclear SNPs, built specifically for the target species at the University of Basque Country UPV/EHU. First analysis done was the Hardy-Weinberg, then the number of clusters (K) was determined using STRUCTURE and to assess the genetic variability, allele frequencies, the average number of alleles per locus, expected (He) and observed (Ho) heterozygosis, and the index of polymorphism (P) was used the software Genetix. Historical and modern samples gives different results, showing a clear loss of genetic diversity over time leading to a single cluster in modern albacore instead of the two found in historical samples. What this study reveals is very important for conservation concerns, and additional research endeavours are needed.

Basilea 3: La ricezione della terminologia finanziaria nel settore bancario. Analisi della variazione linguistica in corpora italiani e tedeschi

Il punto di partenza del presente lavoro di ricerca terminologica è stato il soggiorno formativo presso la Direzione generale della Traduzione (DGT) della Commissione Europea di Lussemburgo. Il progetto di tirocinio, ovvero l’aggiornamento e la revisione di schede IATE afferenti al dominio finanziario, e gli aspetti problematici riscontrati durante la compilazione di tali schede hanno portato alla definizione della presente tesi. Lo studio si prefigge di analizzare la ricezione della terminologia precipua della regolamentazione di Basilea 3, esaminando il fenomeno della variazione linguistica in corpora italiani e tedeschi. Nel primo capitolo si descrive brevemente l’esperienza di tirocinio svolto presso la DGT, si presenta la banca dati IATE, l’attività terminologica eseguita e si illustrano le considerazioni che hanno portato allo sviluppo del progetto di tesi. Nel secondo capitolo si approfondisce il dominio investigato, descrivendo a grandi linee la crisi finanziaria che ha portato alla redazione della nuova normativa di Basilea 3, e si presentano i punti fondamentali degli Accordi di Basilea 3. Il terzo capitolo offre una panoramica sulle caratteristiche del linguaggio economico-finanziario e sulle conseguenze della nuova regolamentazione dal punto di vista linguistico, sottolineando le peculiarità della terminologia analizzata. Nel quarto capitolo si descrivono la metodologia seguita e le risorse utilizzate per il progetto di tesi, ovvero corpora ad hoc in lingua italiana e tedesca per l’analisi dei termini e le relative schede terminologiche. Il quinto capitolo si concentra sul fenomeno della variazione linguistica, fornendo un quadro teorico dei diversi approcci alla terminologia, cui segue l’analisi dei corpora e il commento dei risultati ottenuti; si considerano quindi le riflessioni teoriche alla luce di quanto emerso dalla disamina dei corpora. Infine, nell'appendice sono riportate le schede terminologiche IATE compilate durante il periodo di tirocinio e le schede terminologiche redatte a seguito dell’analisi del presente elaborato.

Radio relics and magnetic fields in galaxy clusters

Radio relics are diffuse synchrotron sources generally located in the peripheries of galaxy clusters in merging state. According to the current leading scenario, relics trace gigantic cosmological shock waves that cross the intra-cluster medium where particle acceleration occurs. The relic/shock connection is supported by several observational facts, including the spatial coincidence between relics and shocks found in the X-rays. Under the assumptions that particles are accelerated at the shock front and are subsequently deposited and then age downstream of the shock, Markevitch et al. (2005) proposed a method to constrain the magnetic field strength in radio relics. Measuring the thickness of radio relics at different frequencies allows to derive combined constraints on the velocity of the downstream flow and on the magnetic field, which in turns determines particle aging. We elaborate this idea to infer first constraints on magnetic fields in cluster outskirts. We consider three models of particle aging and develop a geometric model to take into account the contribution to the relic transverse size due to the projection of the shock-surface on the plane of the sky. We selected three well studied radio relics in the clusters A 521, CIZA J2242.8+5301 and 1RXS J0603.3+4214. These relics have been chosen primarily because they are almost seen edge-on and because the Mach number of the shock that is associated with these relics is measured by X-ray observations, thus allowing to break the degeneracy between magnetic field and downstream velocity in the method. For the first two clusters, our method is consistent with a pure radiative aging model allowing us to derive constraints on the relics magnetic field strength. In the case of 1RXS J0603.3+4214 we find that particle life-times are consistent with a pure radiative aging model under some conditions, however we also collect evidences for downstream particle re-acceleration in the relic W-region and for a magnetic field decaying downstream in its E-region. Our estimates of the magnetic field strength in the relics in A 521 and CIZA J2242.8+5301 provide unique information on the field properties in cluster outskirts. The constraints derived for these relics, together with the lower limits to the magnetic field that we derived from the lack of inverse Compton X-ray emission from the sources, have been combined with the constraints from Faraday rotation studies of the Coma cluster. Overall results suggest that the spatial profile of the magnetic field energy density is broader than that of the thermal gas, implying that the ε_th /ε_B ratio decreases with cluster radius. Alternatively, radio relics could trace dynamically active regions where the magnetic field strength is biased high with respect to the average value in the cluster volume.

Axion-like particles and the 3.5 keV line in 4D string models

This work is focused on axions and axion like particles (ALPs) and their possible relation with the 3.55 keV photon line detected, in recent years, from galaxy clusters and other astrophysical objects. We focus on axions that come from string compactification and we study the vacuum structure of the resulting low energy 4D N=1 supergravity effective field theory. We then provide a model which might explain the 3.55 keV line through the following processes. A 7.1 keV dark matter axion decays in two light axions, which, in turn, are transformed into photons thanks to the Primakoff effect and the existence of a kinetic mixing between two U(1)s gauge symmetries belonging respectively to the hidden and the visible sector. We present two models, the first one gives an outcome inconsistent with experimental data, while the second can yield the desired result.