Constraints on neutrino mass fraction using Redshift Space Distortions

Redshift Space Distortions (RSD) are an apparent anisotropy in the distribution of galaxies due to their peculiar motion. These features are imprinted in the correlation function of galaxies, which describes how these structures distribute around each other. RSD can be represented by a distortions parameter $\beta$, which is strictly related to the growth of cosmic structures. For this reason, measurements of RSD can be exploited to give constraints on the cosmological parameters, such us for example the neutrino mass. Neutrinos are neutral subatomic particles that come with three flavours, the electron, the muon and the tau neutrino. Their mass differences can be measured in the oscillation experiments. Information on the absolute scale of neutrino mass can come from cosmology, since neutrinos leave a characteristic imprint on the large scale structure of the universe. The aim of this thesis is to provide constraints on the accuracy with which neutrino mass can be estimated when expoiting measurements of RSD. In particular we want to describe how the error on the neutrino mass estimate depends on three fundamental parameters of a galaxy redshift survey: the density of the catalogue, the bias of the sample considered and the volume observed. In doing this we make use of the BASICC Simulation from which we extract a series of dark matter halo catalogues, characterized by different value of bias, density and volume. This mock data are analysed via a Markov Chain Monte Carlo procedure, in order to estimate the neutrino mass fraction, using the software package CosmoMC, which has been conveniently modified. In this way we are able to extract a fitting formula describing our measurements, which can be used to forecast the precision reachable in future surveys like Euclid, using this kind of observations.

Galaxy evolution in the VIMOS public extragalactic redshift survey (VIPERS)

In this work I present the first measurements of the galaxy stellar mass function (GSMF) from the first public release of the VIPERS catalogue, containing ∼55,000 objects. First, I present the survey design, its scientific goal, the redshift measurements and validation. Then, I provide details about the estimate of galaxy stellar masses, star formation rates, and other physical quantities. I derive the GSMF of different galaxy types (e.g. active and passive galaxies) and as a function of the environment (defined through the local galaxy density contrast). These estimates represent new observational evidence useful to characterise the mechanism of galaxy evolution.

Caratteristiche principali dell'emissione di galassie a spirale

Lo spazio fra le stelle nelle galassie non è vuoto, ma è composto da gas rarefatto, particelle di polvere, un campo magnetico, elettroni, protoni e altri nuclei atomici relativistici; spesso questi elementi possono essere considerati come un’unica entità di- namica: il mezzo interstellare o più semplicemente ISM. Nel primo capitolo vedremo come il mezzo si distribuisce generalmente all’interno delle galassie a spirale, in fasce di temperatura sempre minore man mano che ci si allontana dal centro (HIM, WIM, WNM, CNM). La conoscenza della distribuzione del mezzo è utile per poter comprendere maggiormente i processi di emissione e le varie zone in cui questi avvengono in una tipica galassia a spirale, che è lo scopo di questa tesi. L’ISM infatti entra in gioco in quasi tutti i processi emissivi, in tutte le bande di emis- sione dello spettro elettromagnetico che andremo ad analizzare. Il nostro modo di vedere le galassie dell’universo è molto cambiato infatti nel corso dell’ultimo secolo: l’utilizzo di nuovi telescopi ci ha permesso di andare ad osservare le galassie anche in bande dello spettro diverse da quella visibile, in modo da raccogliere informazioni impossibili da ottenere con la sola banda ottica. Nel secondo capitolo andremo ad analizzare cinque bande di emissione (banda X, ot- tica, radio, gamma e infrarossa) e vedremo come appaiono tipicamente le galassie a spirale a lunghezze d’onda differenti, quali sono i processi in gioco e come il mezzo interstellare sia fondamentale in quasi ogni tipo di processo. A temperature elevate, esso è responsabile dell’emissione X della galassia, mentre re- gioni più fredde, formate da idrogeno ionizzato, sono responsabili delle righe di emis- sione presenti nello spettro ottico. Il campo magnetico, tramite le sue interazioni con elettroni relativistici è la principale fonte dell’emissione radio nel continuo di una galas- sia a spirale, mentre quella in riga è dovuta a idrogeno atomico o a gas freddo. Vedremo infine come raggi cosmici e polvere, che fanno sempre parte del mezzo inter- stellare, siano rispettivamente la causa principale dell’emissione gamma e infrarossa.

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.

Black Hole and Galaxy Growth over Cosmic Time: the Chandra COSMOS Legacy Survey

The study of supermassive black hole (SMBH) accretion during their phase of activity (hence becoming active galactic nuclei, AGN), and its relation to the host-galaxy growth, requires large datasets of AGN, including a significant fraction of obscured sources. X-ray data are strategic in AGN selection, because at X-ray energies the contamination from non-active galaxies is far less significant than in optical/infrared surveys, and the selection of obscured AGN, including also a fraction of heavily obscured AGN, is much more effective. In this thesis, I present the results of the Chandra COSMOS Legacy survey, a 4.6 Ms X-ray survey covering the equatorial COSMOS area. The COSMOS Legacy depth (flux limit f=2x10^(-16) erg/s/cm^(-2) in the 0.5-2 keV band) is significantly better than that of other X-ray surveys on similar area, and represents the path for surveys with future facilities, like Athena and X-ray Surveyor. The final Chandra COSMOS Legacy catalog contains 4016 point-like sources, 97% of which with redshift. 65% of the sources are optically obscured and potentially caught in the phase of main BH growth. We used the sample of 174 Chandra COSMOS Legacy at z>3 to place constraints on the BH formation scenario. We found a significant disagreement between our space density and the predictions of a physical model of AGN activation through major-merger. This suggests that in our luminosity range the BH triggering through secular accretion is likely preferred to a major-merger triggering scenario. Thanks to its large statistics, the Chandra COSMOS Legacy dataset, combined with the other multiwavelength COSMOS catalogs, will be used to answer questions related to a large number of astrophysical topics, with particular focus on the SMBH accretion in different luminosity and redshift regimes.

Study of cosmic nuclei fluxes with AMS-02: implication for dark matter search

L’Alpha Magnetic Spectrometer (AMS-02) é un rivelatore per raggi cosmici (CR) progettato e costruito da una collaborazione internazionale di 56 istituti e 16 paesi ed installato il 19 Maggio del 2011 sulla Stazione Spaziale Internazionale (ISS). Orbitando intorno alla Terra, AMS-02 sará in grado di studiare con un livello di accuratezza mai raggiunto prima la composizione dei raggi cosmici, esplorando nuove frontiere nella fisica delle particelle, ricercando antimateria primordiale ed evidenze indirette di materia oscura. Durante il mio lavoro di tesi, ho utilizzato il software GALPROP per studiare la propagazione dei CR nella nostra Galassia attraverso il mezzo interstellare (ISM), cercando di individuare un set di parametri in grado di fornire un buon accordo con i dati preliminari di AMS-02. In particolare, mi sono dedicata all’analisi del processo di propagazione di nuclei, studiando i loro flussi e i relativi rapporti. Il set di propagazione ottenuto dall’analisi é stato poi utilizzato per studiare ipotetici flussi da materia oscura e le possibili implicazioni per la ricerca indiretta attraverso AMS-02.

Suche nach Dunkler Materie in Galaxien und Galaxienhaufen mit dem Neutrinoteleskop IceCube

Trotz zahlreicher Hinweise auf die Existenz von Dunkler Materie, konnten entsprechende Teilchen bisher nicht nachgewiesen werden. Eine große Anzahl an Experimenten wird durchgeführt, um die Eigenschaften möglicher Kandidatenteilchen zu untersuchen. Eine Strategie ist die Suche nach einem Neutrinosignal aus den Annihilationen von schwach wechselwirkenden massiven Teilchen (WIMPs) in Regionen mit hoher Dichte von Dunkler Materie. Mögliche Zielobjekte dieser Suchen sind die Erde, die Sonne, das Zentrum und der Halo der Milchstraße sowie entfernte Objekte, die einen hohen Anteil Dunkler Materie aufweisen.In der vorliegenden Arbeit wird die erste Suche nach einem Neutrinosignal von Zwerggalaxien, größeren Galaxien und Galaxienhaufen beschrieben. Da kein Signal nachgewiesen wurde, konnten obere Grenzen auf den Annihilationsquerschnitt von WIMPs gesetzt werden. Die stärksten Grenzen wurden aus der Beobachtung des Virgo-Haufens unter der Annahme einer großen Signalverstärkung durch Unterstrukturen in der Dichteverteilung abgeleitet. Für WIMP-Massen oberhalb von einigen TeV ist das Ergebnis vergleichbar mit Grenzen, die aus der Suche mit Gammateleskopen abgeleitet wurden. Für den direkten Annihilationskanal in zwei Neutrinos konnte der Wirkungsquerschnitt stärker eingeschränkt werden, als in bisherigen Analysen.

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.

Multifrequency VLBA observations of two compact symmetric objects

In this thesis the results of the multifrequency VLBA observations of the GPS 1944+5448 and the HFP J0111+3906 are presented. They are compact objects smaller than about 100 pc, completely embedded in the host galaxy. The availability of multi-epoch VLBI observations spanning more than 10 years, allowed us to compute the hot spot advance speed in order to obtain the kinematic age of both sources. Both radio sources are young, in agreement with the idea that they are in an early evolutionary stage. The spectral analysis of each source component, such as the lobes, the hot spots, the core and the jets, making a comparison with the theoretical ones is described. In addition the physical parameters derived from VLBA images as the magnetic field, the luminosity, the energy and the ambient medium density of both sources are discussed.

Caratteristiche principali dell'emissione di galassie a spirale

Le galassie spirali hanno la forma di un disco, con un nucleo globulare più o meno prominente detto bulge e alcune braccia a spirale che si avvolgono attorno ad esso. Il tutto è in rotazione attorno all'asse del disco, con una velocità angolare che varia dal centro alla periferia. Le spirali vengono designate con la lettera S, seguita da una lettera (a, b o c) a seconda dell'importanza dei bracci. Nelle spirali di tipo Sa, i bracci sono piuttosto stretti e il nucleo è preponderante, nelle Sb invece i bracci sono più prominenti e nelle Sc sono ancora più importanti rispetto al nucleo e hanno anche un aspetto piu' "diffuso". Le spirali barrate, che si indicano con la notazione SB seguita dalle lettere a, b o c, sono identiche alle precedenti, salvo per il fatto che le braccia partono dalle estremità di una barra di stelle e gas che attraversa diametralmente il bulge, anziché direttamente da questo. Il contenuto di queste galassie a spirale è piuttosto disomogeneo; la densità della materia diminuisce dal centro verso la periferia. Inoltre possiedono una grande quantità di gas mischiato a polvere, dal quale si formano tutt'ora molte nuove stelle. Le stelle sono concentrate nel nucleo, nei bracci e in un alone di ammassi globulari disposti intorno alla galassia. Inoltre, questo gas è soggetto a processi violenti come l'esplosione di supernoavae, che vi immettono grandi quantità di energia e altro materiale, perciò la materia interstellare è disposta in modo piuttosto irregolare, concentrata in nubi di varie dimensioni. E da queste nubi si formano le stelle. Nella prima parte dell'elaborato ci occuperemo del mezzo interstellare: temperatura e densità differenziano le fasi dell' ISM, da qui discendono i vari processi di emissione/assorbimento che vedremo nella seconda parte. Principalmente andremo ad analizzare cinque bande di emissione (banda X, ottica, radio, gamma e infrarossa) e vedremo come appaiono tipicamente le galassie a spirale a lunghezze d'onda differenti, quali sono i processi in gioco e come il mezzo interstellare sia fondamentale in quasi ogni tipo di processo. A temperature elevate, esso è responsabile dell'emissione X della galassia, mentre regioni più fredde, formate da idrogeno ionizzato, sono responsabili delle righe di emissione presenti nello spettro ottico. Il campo magnetico, tramite le sue interazioni con elettroni relativistici è la principale fonte dell'emissione radio nel continuo di una galassia a spirale, mentre quella in riga è dovuta a idrogeno atomico o a gas freddo. Vedremo infine come raggi cosmici e polvere, che fanno sempre parte del mezzo interstellare, siano rispettivamente la causa principale dell'emissione gamma e infrarossa.

Post-project assessment and follow-up support for community managed rural water systems in Panama

The Environmental Health (EH) program of Peace Corps (PC) Panama and a non-governmental organization (NGO) Waterlines have been assisting rural communities in Panama gain access to improved water sources through the practice of community management (CM) model and participatory development. Unfortunately, there is little information available on how a water system is functioning once the construction is complete and the volunteer leaves the community. This is a concern when the recent literature suggests that most communities are not able to indefinitely maintain a rural water system (RWS) without some form of external assistance (Sara and Katz, 1997; Newman et al, 2002; Lockwood, 2002, 2003, 2004; IRC, 2003; Schweitzer, 2009). Recognizing this concern, the EH program director encouraged the author to complete a postproject assessment of the past EH water projects. In order to carry out the investigation, an easy to use monitoring and evaluation tool was developed based on literature review and the author’s three years of field experience in rural Panama. The study methodology consists of benchmark scoring systems to rate the following ten indicators: watershed, source capture, transmission line, storage tank, distribution system, system reliability, willingness to pay, accounting/transparency, maintenance, and active water committee members. The assessment of 28 communities across the country revealed that the current state of physical infrastructure, as well as the financial, managerial and technical capabilities of water committees varied significantly depending on the community. While some communities are enjoying continued service and their water committee completing all of its responsibilities, others have seen their water systems fall apart and be abandoned. Overall, the higher score were more prevalent for all ten indicators. However, even the communities with the highest scores requested some form of additional assistance. The conclusion from the assessment suggests that the EH program should incorporate an institutional support mechanism (ISM) to its sector policy in order to systematically provide follow-up support to rural communities in Panama. A full-time circuit rider with flexible funding would be able to provide additional technical support, training and encouragement to those communities in need.

Filtration and oxidation characteristics of a diesel oxidation catalyst and a catalyzed particulate filter : development of a 1-D 2-layer model

The emissions, filtration and oxidation characteristics of a diesel oxidation catalyst (DOC) and a catalyzed particulate filter (CPF) in a Johnson Matthey catalyzed continuously regenerating trap (CCRT ®) were studied by using computational models. Experimental data needed to calibrate the models were obtained by characterization experiments with raw exhaust sampling from a Cummins ISM 2002 engine with variable geometry turbocharging (VGT) and programmed exhaust gas recirculation (EGR). The experiments were performed at 20, 40, 60 and 75% of full load (1120 Nm) at rated speed (2100 rpm), with and without the DOC upstream of the CPF. This was done to study the effect of temperature and CPF-inlet NO2 concentrations on particulate matter oxidation in the CCRT ®. A previously developed computational model was used to determine the kinetic parameters describing the oxidation characteristics of HCs, CO and NO in the DOC and the pressure drop across it. The model was calibrated at five temperatures in the range of 280 – 465° C, and exhaust volumetric flow rates of 0.447 – 0.843 act-m3/sec. The downstream HCs, CO and NO concentrations were predicted by the DOC model to within ±3 ppm. The HCs and CO oxidation kinetics in the temperature range of 280 - 465°C and an exhaust volumetric flow rate of 0.447 - 0.843 act-m3/sec can be represented by one ’apparent’ activation energy and pre-exponential factor. The NO oxidation kinetics in the same temperature and exhaust flow rate range can be represented by ’apparent’ activation energies and pre-exponential factors in two regimes. The DOC pressure drop was always predicted within 0.5 kPa by the model. The MTU 1-D 2-layer CPF model was enhanced in several ways to better model the performance of the CCRT ®. A model to simulate the oxidation of particulate inside the filter wall was developed. A particulate cake layer filtration model which describes particle filtration in terms of more fundamental parameters was developed and coupled to the wall oxidation model. To better model the particulate oxidation kinetics, a model to take into account the NO2 produced in the washcoat of the CPF was developed. The overall 1-D 2-layer model can be used to predict the pressure drop of the exhaust gas across the filter, the evolution of particulate mass inside the filter, the particulate mass oxidized, the filtration efficiency and the particle number distribution downstream of the CPF. The model was used to better understand the internal performance of the CCRT®, by determining the components of the total pressure drop across the filter, by classifying the total particulate matter in layer I, layer II, the filter wall, and by the means of oxidation i.e. by O2, NO2 entering the filter and by NO2 being produced in the filter. The CPF model was calibrated at four temperatures in the range of 280 – 465 °C, and exhaust volumetric flow rates of 0.447 – 0.843 act-m3/sec, in CPF-only and CCRT ® (DOC+CPF) configurations. The clean filter wall permeability was determined to be 2.00E-13 m2, which is in agreement with values in the literature for cordierite filters. The particulate packing density in the filter wall had values between 2.92 kg/m3 - 3.95 kg/m3 for all the loads. The mean pore size of the catalyst loaded filter wall was found to be 11.0 µm. The particulate cake packing densities and permeabilities, ranged from 131 kg/m3 - 134 kg/m3, and 0.42E-14 m2 and 2.00E-14 m2 respectively, and are in agreement with the Peclet number correlations in the literature. Particulate cake layer porosities determined from the particulate cake layer filtration model ranged between 0.841 and 0.814 and decreased with load, which is about 0.1 lower than experimental and more complex discrete particle simulations in the literature. The thickness of layer I was kept constant at 20 µm. The model kinetics in the CPF-only and CCRT ® configurations, showed that no ’catalyst effect’ with O2 was present. The kinetic parameters for the NO2-assisted oxidation of particulate in the CPF were determined from the simulation of transient temperature programmed oxidation data in the literature. It was determined that the thermal and NO2 kinetic parameters do not change with temperature, exhaust flow rate or NO2 concentrations. However, different kinetic parameters are used for particulate oxidation in the wall and on the wall. Model results showed that oxidation of particulate in the pores of the filter wall can cause disproportionate decreases in the filter pressure drop with respect to particulate mass. The wall oxidation model along with the particulate cake filtration model were developed to model the sudden and rapid decreases in pressure drop across the CPF. The particulate cake and wall filtration models result in higher particulate filtration efficiencies than with just the wall filtration model, with overall filtration efficiencies of 98-99% being predicted by the model. The pre-exponential factors for oxidation by NO2 did not change with temperature or NO2 concentrations because of the NO2 wall production model. In both CPF-only and CCRT ® configurations, the model showed NO2 and layer I to be the dominant means and dominant physical location of particulate oxidation respectively. However, at temperatures of 280 °C, NO2 is not a significant oxidizer of particulate matter, which is in agreement with studies in the literature. The model showed that 8.6 and 81.6% of the CPF-inlet particulate matter was oxidized after 5 hours at 20 and 75% load in CCRT® configuration. In CPF-only configuration at the same loads, the model showed that after 5 hours, 4.4 and 64.8% of the inlet particulate matter was oxidized. The increase in NO2 concentrations across the DOC contributes significantly to the oxidation of particulate in the CPF and is supplemented by the oxidation of NO to NO2 by the catalyst in the CPF, which increases the particulate oxidation rates. From the model, it was determined that the catalyst in the CPF modeslty increases the particulate oxidation rates in the range of 4.5 – 8.3% in the CCRT® configuration. Hence, the catalyst loading in the CPF of the CCRT® could possibly be reduced without significantly decreasing particulate oxidation rates leading to catalyst cost savings and better engine performance due to lower exhaust backpressures.

Bluetooth Enabled Ad-hoc Networks: Performance Evaluation of a Self-healing Scatternet Formation Protocol

Bluetooth wireless technology is a robust short-range communications system designed for low power (10 meter range) and low cost. It operates in the 2.4 GHz Industrial Scientific Medical (ISM) band and it employs two techniques for minimizing interference: a frequency hopping scheme which nominally splits the 2.400 - 2.485 GHz band in 79 frequency channels and a time division duplex (TDD) scheme which is used to switch to a new frequency channel on 625 μs boundaries. During normal operation a Bluetooth device will be active on a different frequency channel every 625 μs, thus minimizing the chances of continuous interference impacting the performance of the system. The smallest unit of a Bluetooth network is called a piconet, and can have a maximum of eight nodes. Bluetooth devices must assume one of two roles within a piconet, master or slave, where the master governs quality of service and the frequency hopping schedule within the piconet and the slave follows the master’s schedule. A piconet must have a single master and up to 7 active slaves. By allowing devices to have roles in multiple piconets through time multiplexing, i.e. slave/slave or master/slave, the Bluetooth technology allows for interconnecting multiple piconets into larger networks called scatternets. The Bluetooth technology is explored in the context of enabling ad-hoc networks. The Bluetooth specification provides flexibility in the scatternet formation protocol, outlining only the mechanisms necessary for future protocol implementations. A new protocol for scatternet formation and maintenance - mscat - is presented and its performance is evaluated using a Bluetooth simulator. The free variables manipulated in this study include device activity and the probabilities of devices performing discovery procedures. The relationship between the role a device has in the scatternet and it’s probability of performing discovery was examined and related to the scatternet topology formed. The results show that mscat creates dense network topologies for networks of 30, 50 and 70 nodes. The mscat protocol results in approximately a 33% increase in slaves/piconet and a reduction of approximately 12.5% of average roles/node. For 50 node scenarios the set of parameters which creates the best determined outcome is unconnected node inquiry probability (UP) = 10%, master node inquiry probability (MP) = 80% and slave inquiry probability (SP) = 40%. The mscat protocol extends the Bluetooth specification for formation and maintenance of scatternets in an ad-hoc network.