Multiple stellar populations in globular clusters with photometry and low resolution spectroscopy

Our view of Globular Clusters has deeply changed in the last decade. Modern spectroscopic and photometric data have conclusively established that globulars are neither coeval nor monometallic, reopening the issue of the formation of such systems. Their formation is now schematized as a two-step process, during which the polluted matter from the more massive stars of a first generation gives birth, in the cluster innermost regions, to a second generation of stars with the characteristic signature of fully CNO-processed matter. To date, star-to-star variations in abundances of the light elements (C, N, O, Na) have been observed in stars of all evolutionary phases in all properly studied Galactic globular clusters. Multiple or broad evolutionary sequences have also been observed in nearly all the clusters that have been observed with good signal-to-noise in the appropriate photometric bands. The body of evidence suggests that spreads in light-element abundances can be fairly well traced by photometric indices including near ultraviolet passbands, as CNO abundance variations affect mainly wavelengths shorter than ~400 nm owing to the rise of some NH and CN molecular absorption bands. Here, we exploit this property of near ultraviolet photometry to trace internal chemical variations and combined it with low resolution spectroscopy aimed to derive carbon and nitrogen abundances in order to maximize the information on the multiple populations. This approach has been proven to be very effective in (i) detecting multiple population, (ii) characterizing their global properties (i.e., relative fraction of stars, location in the color-magnitude diagram, spatial distribution, and trends with cluster parameters) and (iii) precisely tagging their chemical properties (i.e., extension of the C-N anticorrelation, bimodalities in the N content).

Chemical and kinematical properties of Blue Straggler stars in Galactic globular clusters

Blue straggler stars (BSSs) are brighter and bluer (hotter) than the main-sequence (MS) turnoff and they are known to be more massive than MS stars.Two main scenarios for their formation have been proposed:collision-induced stellar mergers (COL-BSSs),or mass-transfer in binary systems (MT-BSSs).Depleted surface abundances of C and O are expected for MT-BSSs,whereas no chemical anomalies are predicted for COL-BSSs.Both MT- and COL-BSSs should rotate fast, but braking mechanisms may intervene with efficiencies and time-scales not well known yet,thus preventing a clear prediction of the expected rotational velocities.Within this context,an extensive survey is ongoing by using the multi-object spectrograph FLAMES@VLT,with the aim to obtain abundance patterns and rotational velocities for representative samples of BSSs in several Galactic GCs.A sub-population of CO-depleted BSSs has been identified in 47 Tuc,with only one fast rotating star detected.For this PhD Thesis work I analyzed FLAMES spectra of more than 130 BSSs in four GCs:M4,NGC 6397,M30 and ω Centauri.This is the largest sample of BSSs spectroscopically investigated so far.Hints of CO depletion have been observed in only 4-5 cases (in M30 and ω Centauri),suggesting either that the majority of BSSs have a collisional origin,or that the CO-depletion is a transient phenomenon.Unfortunately,no conclusions in terms of formation mechanism could be drawn in a large number of cases,because of the effects of radiative levitation. Remarkably,however,this is the first time that evidence of radiative levitation is found in BSSs hotter than 8200 K.Finally, we also discovered the largest fractions of fast rotating BSSs ever observed in any GCs:40% in M4 and 30% in ω Centauri.While not solving the problem of BSS formation,these results provide invaluable information about the BSS physical properties,which is crucial to build realistic models of their evolution.

Ruolo dell'elettrocardiogramma standard nella stratificazione prognostica della cardiomiopatia ipertrofica. Studio multicentrico

Lo scopo di questo studio è di valutare il significato prognostico dell'elettrocardiogramma standard in un'ampia casistica di pazienti affetti da cardiomiopatia ipertrofica. In questo studio multicentrico sono stati considerati 841 pazienti con cardiomiopatia ipertrofica (66% uomini, età media 48±17 anni) per un follow-up di 7.1±7.1 anni, per ognuno è stato analizzato il primo elettrocardiogramma disponibile. I risultati hanno dimostrato come fattori indipendentemente correlati a morte cardiaca improvvisa la sincope inspiegata (p 0.004), il sopraslivellamento del tratto ST e/o la presenza di onde T positive giganti (p 0.048), la durata del QRS >= 120 ms (p 0.017). Sono stati costruiti due modelli per predire il rischio di morte improvvisa: il primo basato sui fattori di rischio universalmente riconosciuti (spessore parietale >= 30 mm, tachicardie ventricolari non sostenute all'ECG Holter 24 ore, sincope e storia familiare di morte improvvisa) e il secondo con l'aggiunta delle variabili sopraslivellamento del tratto ST/onde T positive giganti e durata del QRS >= 120 ms. Entrambi i modelli stratificano i pazienti in base al numero dei fattori di rischio, ma il secondo modello risulta avere un valore predittivo maggiore (chi-square da 12 a 22, p 0.002). In conclusione nella cardiomiopatia ipertrofica l'elettrocardiogramma standard risulta avere un valore prognostico e migliora l'attuale modello di stratificazione per il rischio di morte improvvisa.

Cosmic-Lab: Optical companions to binary Millisecond Pulsars

Millisecond Pulsars (MSPs) are fast rotating, highly magnetized neutron stars. According to the "canonical recycling scenario", MSPs form in binary systems containing a neutron star which is spun up through mass accretion from the evolving companion. Therefore, the final stage consists of a binary made of a MSP and the core of the deeply peeled companion. In the last years, however an increasing number of systems deviating from these expectations has been discovered, thus strongly indicating that our understanding of MSPs is far to be complete. The identification of the optical companions to binary MSPs is crucial to constrain the formation and evolution of these objects. In dense environments such as Globular Clusters (GCs), it also allows us to get insights on the cluster internal dynamics. By using deep photometric data, acquired both from space and ground-based telescopes, we identified 5 new companions to MSPs. Three of them being located in GCs and two in the Galactic Field. The three new identifications in GCs increased by 50% the number of such objects known before this Thesis. They all are non-degenerate stars, at odds with the expectations of the "canonical recycling scenario". These results therefore suggest either that transitory phases should also be taken into account, or that dynamical processes, as exchange interactions, play a crucial role in the evolution of MSPs. We also performed a spectroscopic follow-up of the companion to PSRJ1740-5340A in the GC NGC 6397, confirming that it is a deeply peeled star descending from a ~0.8Msun progenitor. This nicely confirms the theoretical expectations about the formation and evolution of MSPs.

Riabilitazione del mascellare posteriore atrofico mediante impianti corti (6-8 mm) o rialzo di seno con contestuale inserimento di impianti di lunghezza standard: studio retrospettivo con follow up a 3 anni

Background: sebbene la letteratura recente abbia suggerito che l’utilizzo degli impianti corti possa rappresentare una alternative preferibile alle procedure di rigenerazione ossea nelle aree posteriori atrofiche, perché è un trattamento più semplice e con meno complicazioni, esistono solo pochi studi a medio e lungo termine che abbiano comparato queste tecniche. Scopo: lo scopo di questo studio retrospettivo è quello di valutare se gli impianti corti (6-8 mm) (gruppo impianti corti) possano presentare percentuali di sopravvivenza e valori di riassorbimento osseo marginali simili a impianti di dimensioni standard (≥11 mm) inseriti contemporaneamente ad una grande rialzo di seno mascellare. Materiali e Metodi: in totale, 101 pazienti sono stati inclusi: 48 nel gruppo impianti corti e 53 nel gruppo seno. In ciascun paziente da 1 a 3 impianti sono stati inseriti e tenuti sommersi per 4-6 mesi. I parametri clinici e radiografici valutati sono: i fallimenti implantari, le complicazioni, lo stato dei tessuti molli, e il riassorbimento osseo marginale. Tutti i pazienti sono stati seguiti per almeno 3 anni dal posizionamento implantare. Risultati: il periodo di osservazione medio è stato di 43.47 ± 6.1 mesi per il gruppo impianti corti e 47.03 ± 7.46 mesi per il gruppo seno. Due su 101 impianti corti e 6 su 108 impianti standard sono falliti. Al follow-up finale, si è riscontrato un riassorbimento osseo medio di 0.47 ± 0.48 mm nel gruppo impianti corti versus 0.64 ± 0.58 mm nel gruppo seno. Non sono presenti differenze statisticamente significative fra i gruppi in termini di fallimenti implantari, complicazioni protesiche, tessuti molli, e riassorbimento osseo. Il gruppo seno ha presentato, invece, un maggior numero di complicazioni chirurgiche. Conclusioni: entrambe le tecniche hanno dimostrato un simile tasso di successo clinico e radiografico, ma gli impianti corti hanno ridotto il numero di complicazioni chirurgiche.

COSMIC-LAB: Terzan 5 as a fossil remnant of the Galactic bulge formation epoch

The formation and evolution of galaxy bulges is a greatly debated topic in modern astrophysics. An approach to address this issue is to look at the Galactic bulge, the closest to us. According to some theoretical models, our bulge built-up from the merger of substructures formed from the instability and fragmentation of a proto-disk in the early phases of Galactic evolution. We may have discovered the remnant of one of these substructures: the stellar system Terzan 5. Terzan 5 hosts two stellar populations with different iron abundances, thus suggesting it once was far more massive than today. Moreover, its peculiar chemistry resembles that observed only in the Galactic bulge. In this Thesis we perform a detailed photometric and spectroscopic analysis of this cluster to determine its formation and evolutionary histories. Form the photometric point of view we built a high-resolution differential reddening map in Terzan 5 direction and we measured relative proper motions to separate its member population from the contaminating field stars. This information represents the necessary work to measure the absolute ages of Terzan 5 populations via the Turn-off luminosity method. From the spectroscopic point of view we measured abundances for more than 600 stars belonging to Terzan 5 and its surroundings in order to build the largest field-decontaminated metallicity distribution for this system. We find that the metallicity distribution is extremely wide (more than 1 dex) and we discovered a third, metal-poor and alpha-enhanced population with average [Fe/H]=-0.8. The striking similarity between Terzan 5 and the bulge in terms of their chemical formation and evolution revealed by this Thesis suggests that Terzan 5 formed in situ with the bulge itself. In particular its metal-poor populations trace the early stages of the bulge formation, while its most metal-rich component contains crucial information on the bulge more recent evolution.

Nuovi protocolli chemioterapici per i sarcomi dei tessuti molli ad alto grado di malignita' negli adulti: Risultati clinici, radiologici e istologici comparando chemioterapia standard e orientata sull'isotopo

I sarcomi dei tessuti molli sono un gruppo eterogeneo di tumori maligni di origine mesenchimale che si sviluppa nel tessuto connettivo. Il controllo locale mediante escissione chirurgica con margini ampi associato alla radioterapia e chemioterapia è il trattamento di scelta. Negli ultimi anni le nuove scoperte in campo biologico e clinico hanno sottolineato che i diversi istotipi posso essere considerati come entità distinte con differente sensibilità alla chemioterapia pertanto questa deve essere somministrata come trattamento specifico basato sull’istologia. Tra Ottobre 2011 e Settembre 2014 sono stati inclusi nel protocollo di studio 49 pazienti con sarcomi dei tessuti molli di età media alla diagnosi 48 anni (range: 20 - 68 anni). I tumori primitivi più frequenti sono: liposarcoma mixoide, sarcoma pleomorfo indifferenziato, sarcoma sinoviale. Le sedi di insorgenza del tumore erano più frequentemente la coscia, il braccio e la gamba. 35 pazienti sono stati arruolati nel Braccio A e trattati con chemioterapia standard con epirubicina+ifosfamide, 14 sono stati arruolati nel Braccio B e trattati con chemioterapia basata sull’istotipo. I dati emersi da questo studio suggeriscono che le recidive locali sembrano essere correlate favorevolmente alla radioterapia ed ai margini chirurgici adeguati mentre la chemioterapia non sembra avere un ruolo sul controllo locale della malattia. Anche se l'uso di terapie mirate, che hanno profili di tossicità più favorevoli e sono quindi meglio tollerate rispetto ai farmaci citotossici è promettente, tali farmaci hanno prodotto finora risultati limitati. Apparentemente l’insieme delle terapie mirate non sembra funzionare meglio delle terapie standard, tuttavia esse devono essere esaminate per singolo istotipo e confrontate con il braccio di controllo. Sono necessari studi randomizzati controllati su ampie casistiche per valutare l’efficacia delle terapie mirate sui differenti istotipi di sarcomi dei tessuti molli. Inoltre, nuovi farmaci, nuove combinazioni e nuovi schemi posologici dovranno essere esaminati per ottimizzare la terapia.

COSMIC-LAB: Unexpected Results from High-resolution Spectra of AGB Stars in Globular Clusters

We have used high-resolution spectra, acquired with UVES@ESO-VLT, to determine the chemical abundances of different samples of AGB and RGB stars in 4 Galactic globular clusters, namely 47Tuc, NGC3201, M22 and M62. For almost all the analyzed AGB stars we found a clear discrepancy between the iron abundance measured from neutral lines and that obtained from single ionized lines, while this discrepancy is not obtained for the RGB samples observed in the same clusters and analyzed with the same procedure. Such a behavior exactly corresponds to what expected in the case of Non-Local Thermodynamical Equilibrium (NLTE) in the star atmosphere. These results have a huge impact on the proper determination of GC chemistry. In fact, one of the most intriguing consequences is that, at odds with previous claims, no iron spread is found in NGC3201 and M22 if the iron abundance is obtained from ionized lines only.

On the Luminous and Dark Matter Distribution in Early-Type Galaxies

The way mass is distributed in galaxies plays a major role in shaping their evolution across cosmic time. The galaxy's total mass is usually determined by tracing the motion of stars in its potential, which can be probed observationally by measuring stellar spectra at different distances from the galactic centre, whose kinematics is used to constrain dynamical models. A class of such models, commonly used to accurately determine the distribution of luminous and dark matter in galaxies, is that of equilibrium models. In this Thesis, a novel approach to the design of equilibrium dynamical models, in which the distribution function is an analytic function of the action integrals, is presented. Axisymmetric and rotating models are used to explain observations of a sample of nearby early-type galaxies in the Calar Alto Legacy Integral Field Area survey. Photometric and spectroscopic data for round and flattened galaxies are well fitted by the models, which are then used to get the galaxies' total mass distribution and orbital anisotropy. The time evolution of massive early-type galaxies is also investigated with numerical models. Their structural properties (mass, size, velocity dispersion) are observed to evolve, on average, with redshift. In particular, they appear to be significantly more compact at higher redshift, at fixed stellar mass, so it is interesting to investigate what drives such evolution. This Thesis focuses on the role played by dark-matter haloes: their mass-size and mass-velocity dispersion correlations evolve similarly to the analogous correlations of ellipticals; at fixed halo mass, the haloes are more compact at higher redshift, similarly to massive galaxies; a simple model, in which all the galaxy's size and velocity-dispersion evolution is due to the cosmological evolution of the underlying halo population, reproduces the observed size and velocity-dispersion of massive compact early-type galaxies up to redshift of about 2.