Proprietà degli ammassi di galassie

In questa tesi di laurea triennale vengono esposte le conoscenze fondamentali che descrivono gli ammassi di galassie. I galaxy clusters sono strutture gravitazionalmente legate composte di galassie, gas denominato ICM (Intra Cluster Medium) e materia oscura. Queste 3 diverse componenti sono responsabili rispettivamente del 5%, 15% e 80% circa della massa totale dell’ammasso; per la maggior parte degli ammassi la massa totale è 10^{14-15} masse solari. Nella prima parte della tesi si illustrano brevemente queste 3 componenti e le si inquadrano nelle diverse classificazioni morfologiche degli ammassi. Nella seconda parte ho passato in rassegna alcune delle funzioni più importanti per descrivere un ammasso di galassie. Nella terza ed ultima parte sono esposti i principali meccanismi grazie ai quali conosciamo gli ammassi di galassie.

A study of extended radio galaxies in the Shapley concentration core

Extended cluster radio galaxies show different morphologies com- pared to those found isolated in the field. Indeed, symmetric double radio galaxies are only a small percentage of the total content of ra- dio loud cluster galaxies, which show mainly tailed morphologies (e.g. O’Dea & Owen, 1985). Moreover, cluster mergers can deeply affect the statistical properties of their radio activity. In order to better understand the morphological and radio activity differences of the radio galaxies in major mergeing and non/tidal-merging clusters, we performed a multifrequency study of extended radio galax- ies inside two cluster complexes, A3528 and A3558. They belong to the innermost region of the Shapley Concentration, the most massive con- centration of galaxy clusters (termed supercluster) in the local Universe, at average redshift z ≈ 0.043. We analysed low frequency radio data performed at 235 and 610 MHz with Giant Metrewave Radio Telescope (GMRT) and we combined them with proprietary and literature observations, in order to have a wide frequency range (150 MHz to 8.4 GHz) to perform the spectral analysis. The low frequency images allowed us to carry out a detailed study of the radio tails and diffuse emission found in some cases. The results in the radio band were also qualitatively compared with the X-ray information coming from XMM-Newton observations, in order to test the interaction between radio galaxies and cluster weather. We found that the brightest central galaxies (BCGs) in the A3528 cluster complex are powerful and present substantial emission from old relativistic plasma characterized by a steep spectrum (α > 2). In the light of observational pieces of evidence, we suggest they are possible re-started radio galaxies. On the other hand, the tailed radio galaxies trace the host galaxy motion with respect to the ICM, and our find- ings is consistent with the dynamical interpretation of a tidal interaction (Gastaldello et al. 2003). On the contrary, the BCGs in the A3558 clus- ter complex are either quiet or very faint radio galaxies, supporting the hypothesis that clusters mergers quench the radio emission from AGN.

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 0.08clusters at z<0.2 and with the Extended GMRT RH Survey for 0.2clusters 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.

Constraining mass and shape of galaxy clusters through large scale structures

The mass estimation of galaxy clusters is a crucial point for modern cosmology, and can be obtained by several different techniques. In this work we discuss a new method to measure the mass of galaxy clusters connecting the gravitational potential of the cluster with the kinematical properties of its surroundings. We explore the dynamics of the structures located in the region outside virialized cluster, We identify groups of galaxies, as sheets or filaments, in the cluster outer region, and model how the cluster gravitational potential perturbs the motion of these structures from the Hubble fow. This identification is done in the redshift space where we look for overdensities with a filamentary shape. Then we use a radial mean velocity profile that has been found as a quite universal trend in simulations, and we fit the radial infall velocity profile of the overdensities found. The method has been tested on several cluster-size haloes from cosmological N-body simulations giving results in very good agreement with the true values of virial masses of the haloes and orientation of the sheets. We then applied the method to the Coma cluster and even in this case we found a good correspondence with previous. It is possible to notice a mass discrepancy between sheets with different alignments respect to the center of the cluster. This difference can be used to reproduce the shape of the cluster, and to demonstrate that the spherical symmetry is not always a valid assumption. In fact, if the cluster is not spherical, sheets oriented along different axes should feel a slightly different gravitational potential, and so give different masses as result of the analysis described before. Even this estimation has been tested on cosmological simulations and then applied to Coma, showing the actual non-sphericity of this cluster.

Non-thermal properties of two galaxy filament candidates from JVLA observations

Large-scale structures can be considered an interesting and useful "laboratory" to better investigate the Universe; in particular the filaments connecting clusters and superclusters of galaxies can be a powerful tool for this intent, since they are not virialised systems yet. The large structures in the Universe have been studied in different bands, in particular the present work takes into consideration the emission in the radio band. In the last years both compact and diffuse radio emission have been detected, revealing to be associated to single objects and clusters of galaxies respectively. The detection of these sources is important, because the radiation process is the synchrotron emission, which in turn is linked to the presence of a magnetic field: therefore studying these radio sources can help in investigating the magnetic field which permeates different portions of space. Furthermore, radio emission in optical filaments have been detected recently, opening new chances to further improve the understanding of structure formation. Filaments can be seen as the net which links clusters and superclusters. This work was made with the aim of investigating non-thermal properties in low-density regions, looking for possible filaments associated to the diffuse emission. The analysed sources are 0917+75, which is located at a redshift z = 0.125, and the double cluster system A399-A401, positioned at z = 0.071806 and z = 0.073664 respectively. Data were taken from VLA/JVLA observations, and reduced and calibrated with the package AIPS, following the standard procedure. Isocountour and polarisation maps were yielded, allowing to derive the main physical properties. Unfortunately, because of a low quality data for A399-A401, it was not possible to see any radio halo or bridge.

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.

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.

Cluster carbonilici di platino contenenti fosfine

Nel corso di questa Tesi sono state studiate le reazioni di cluster carbonil anionici di Platino con fosfine. In particolare, sono state investigate nel dettaglio le reazioni dei cluster [Pt3n(CO)6n]2– (n = 3,4) e [Pt19(CO)22]n– (n = 3,4) con PPh3. Sono state poi preliminarmente studiate anche le reazioni di [Pt24(CO)30]2– e [Pt38(CO)44]2– con PPh3. Questo ha portato alla sintesi e alla completa caratterizzazione mediante diffrazione di raggi X su cristallo singolo delle specie [NBu4]2[Pt9(CO)16(PPh3)2] e [NBu4]x[Pt22(CO)22(PPh3)6]2•yCH3CN, contenenti gli anioni [Pt9(CO)16(PPh3)2]2– e [Pt22(CO)22(PPh3)6]2–. È stato inoltre preparato un nuovo composto tentativamente formulato come [Pt19(CO)20(PPh3)2]4–, sulla base dei dati IR, 31P NMR e ESI-MS. Questi rappresentano i primi esempi di cluster carbonilici anionici di Platino contenenti fosfine. Nel caso delle reazioni di [Pt24(CO)30]2– e [Pt38(CO)44]2– con PPh3 i prodotti sono stati caratterizzati al momento solo mediante spettroscopia IR, e quindi è molto difficile ipotizzare una loro struttura. I composti [Pt9(CO)16(PPh3)2]2– e [Pt19(CO)20(PPh3)2]4– sono stati investigati mediante spettroscopia 31P NMR in soluzione a temperatura variabile. Il primo mostra un unico segnale 31P NMR, in accordo con la struttura allo stato solido, mentre [Pt19(CO)20(PPh3)2]4– è risultato essere flussionale. È stato poi studiato nel dettaglio il comportamento fotochimico dei cluster [Pt3n(CO)6n]2– (n = 3-6) in funzione della concentrazione, confermando la loro natura di “Double emitting quantum dots”. Infine è stato preparato e caratterizzato strutturalmente il sale [DAMS]2[Pt9(CO)18]•dmf, contenente il catione [DAMS]+.

Sintesi, caratterizzazione e reattività di nuovi Cluster Carbonilici Ni-P

The aim of this work is to explore the chemistry of new heteroatomic molecular compounds never reported in the scientific literature so far: Ni-P carbonyl clusters. First, an attempt was made to illustrate the reasons which brought to the choice of this specific metal-pnictogen couple, such as the interesting properties of Ni-P binary phases, the difficulties related in obtaining structural data for this bulk compounds and the absence of references about nickel-phosphorus molecular compounds (e.g. carbonyl clusters) reported in literature. Then, the general criteria chosen for the reactions between precursors [Ni6(CO)12]2- and PCl3 or POCl3 have been reported. This work has permitted to individuate many new products, of which some have also been isolated and characterised: [Ni11P(CO)18]3-, [Ni23-xP2(CO)30-x]6- (x=0, 1), [HNi31P4(CO)39]5- e [H2Ni31P4(CO)39]4-. Except for the former, a reproducible synthetic path has been refined for all those new Ni-P carbonyl clusters; furthermore some chemical reactivity has been carried out in order to test their characteristics.

Studio mediante spettroscopia di assorbimento di raggi x con luce di sincrotrone di cluster di argento su ceria

si vuole studiare la struttura atomica di cluster di argento su ceria, si è utilizzata la spettroscopia di assorbimento di raggi x con luce di sincrotrone. Le misure sono state effettuate all'Esrf di Grenoble e si sono analizzati gli spettri EXAFS di diversi spessori equivalenti di argento (1.5Å , 0.7Å, 0.2Å, 0.1Å). Si tratta il processo di produzione della luce di sincrotrone e le sue proprietà caratteristiche. In particolare si descrive la strumentazione ottica utilizzata: specchi riflettenti per raggi X e monocromatore con geometria a doppio cristallo.

Cluster carbonilici eterometallici di rodio: Sintesi di nuove specie molecolari e studio della loro reattività

Durante il mio periodo di Tesi ho lavorato nel campo dei cluster eterometallici di Rh stabilizzati da leganti carbonilici. Inizialmente mi sono occupato della reazione di idrogenazione del cluster [Rh12Sn(CO)27]4- e della specie insatura [Rh12Sn(CO)25]4-, che ho sintetizzato per la prima volta con reattore a microonde. Ho poi testato il prodotto [Rh12Sn(CO)27/25-xHy]4- come catalizzatore nella reazione di idrogenazione di stirene ad etilbenzene. Le prove hanno evidenziato la sua scarsa attività catalitica, anzi il catalizzatore si è rivelato instabile sia in atmosfera di H2, dove si trasforma in [Rh14(CO)25]4-, che di CO/H2, dove genera una specie ancora non ben caratterizzata. Nella seconda parte del mio progetto ho cercato di sintetizzare nuovi cluster carbonilici Rh-Bi. Dopo alcune prove sono riuscito ad isolare e caratterizzare il nuovo cluster icosaedrico [Rh12Bi(CO)27]3-. Ne ho poi studiato la reattività trattandolo con BiCl3, HCl e irraggiandolo con le microonde. Dalla prima reazione ho ottenuto due nuove specie molecolari cioè il dimero [(Rh12Bi(CO)26)2Bi]5-, in cui due unità icosaedriche sono legate insieme da uno ione Bi+, e [Rh14Bi3(CO)27]3-, in cui sono presenti legami incipienti intermolecolari Bi-Bi. Nelle altre due prove sono stati identificati nuovi prodotti non ancora identificati ma tuttora in fase di studio.

Interazione di cluster carbonilici FE-CU con complessi di metalli di transizione e leganti azotati

Nel corso di questa Tesi sono state studiate reazioni di cluster carburo-carbonilici Fe/Cu con composti azotati di varia natura: complessi fosforescenti di metalli di transizione, 1-10 fenantrolina, L-amminoacidi e Chinolina. In particolare la reazione tra Fe4C(CO)12Cu2(CH3CN)2 e [Ru(tpy)(bpy)(N4C-C6H4-CN)]+ ha portato alla sintesi dell’addotto Fe4C(CO)12{Cu2Cl[Ru(tpy)(bpy)(N4C-C6H4-CN)]}, sul quale sono state condotte misure di luminescenza (emissione, eccitazione e misura dei tempi di vita degli stati eccitati). Per confronto degli spettri registrati su campioni di adotto in soluzione con quelli del complesso cationico di Ru(II), si è ipotizzato che l’addotto sintetizzato in soluzione dia origine ad un sistema in equilibrio tra le specie legate e dissociate. Le reazioni di Fe4C(CO)12Cu2(CH3CN)2 e [NEt4][Fe5C(CO)14Cu(CH3CN)] con 1-10 fenantrolina hanno permesso di isolare le nuove specie [Fe4C(CO)12(Cuphen)]–, [Fe4C(CO)12(Cuphen)] e [Fe5C(CO)14(Cuphen)]–, sottoforma dei loro sali [Cu(phen)2][Fe4C(CO)12(Cuphen)], [NEt4] [Fe4C(CO)12(Cuphen)], [Fe4C(CO)12(Cuphen)], [NEt4][Fe5C(CO)14(Cuphen)]• CH2Cl2 e [NEt4][Fe5C(CO)14(Cuphen)]•THF. In tali cluster si nota come la natura bidentata di phen e il suo ingombro sterico abbiano causato notevoli riarrangiamenti strutturali rispetto alle specie iniziali contenenti acetonitrile. La sintesi di Fe4C(CO)12(CuQ)2 e [NEt4][Fe5C(CO)14(CuQ)] è avvenuta inaspettatamente a partire dalle reazioni condotte tra Fe4C(CO)12Cu2(CH3CN)2 e [NEt4][Fe5C(CO)14Cu(CH3CN)] con le molecole L-prolina, L-metionina e guanina, a causa della chinolina contenuta come impurezza nei reagenti di partenza. L’esito di questa reazione ha comunque mostrato l’elevata affinità dei cluster per il legante chinolina, sebbene presente in ambiente di reazione in misura sensibilmente inferiore rispetto agli altri reagenti. Tutte le nuove specie sintetizzate sono stati caratterizzate mediante spettroscopia IR e le strutture molecolari sono state determinate mediante diffrazione di raggi X su cristallo singolo.

The relation between mass and concentration in x-ray galaxy clusters at high-redshift.

In this Thesis work we have studied the properties of high-redshift galaxy clusters through the X-ray emission from their intracluster gas. In particular, we have focused on the relation between concentration and mass that is related to the density of the universe at the formation time of the clusters and therefore, it is a powerful cosmological probe. Concentration is expected to be a decreasing function of mass but a complete characterization of this relation has not been reached yet. We have analysed 22 clusters observed withe the Chandra satellite at high redshift and we have investigated the concentration-mass relation.