Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory

We report a measurement of the flux of cosmic rays with unprecedented precision and Statistics using the Pierre Auger Observatory Based on fluorescence observations in coincidence with at least one Surface detector we derive a spectrum for energies above 10(18) eV We also update the previously published energy spectrum obtained with the surface detector array The two spectra are combined addressing the systematic uncertainties and, in particular. the influence of the energy resolution on the spectral shape The spectrum can be described by a broken power law E(-gamma) with index gamma = 3 3 below the ankle which is measured at log(10)(E(ankle)/eV) = 18 6 Above the ankle the spectrum is described by a power law with index 2 6 followed by a flux suppression, above about log(10)(E/eV) = 19 5, detected with high statistical significance (C) 2010 Elsevier B V All rights reserved

A study of the effect of molecular and aerosol conditions in the atmosphere on air fluorescence measurements at the Pierre Auger Observatory

The air fluorescence detector of the Pierre Auger Observatory is designed to perforin calorimetric measurements of extensive air showers created by Cosmic rays of above 10(18) eV. To correct these measurements for the effects introduced by atmospheric fluctuations, the Observatory contains a group Of monitoring instruments to record atmospheric conditions across the detector site, ail area exceeding 3000 km(2). The atmospheric data are used extensively in the reconstruction of air showers, and are particularly important for the correct determination of shower energies and the depths of shower maxima. This paper contains a summary of the molecular and aerosol conditions measured at the Pierre Auger Observatory since the start of regular operations in 2004, and includes a discussion of the impact of these measurements oil air shower reconstructions. Between 10(18) and 10(20) eV, the systematic Uncertainties due to all atmospheric effects increase from 4% to 8% in measurements of shower energy, and 4 g cm(-2) to 8 g cm(-2) in measurements of the shower maximum. (C) 2010 Elsevier B.V. All rights reserved.

Édipo-Rei e Antígone, adaptações da tragédia sofocleana para o leitor juvenil brasileiro

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

A judicialização da saúde e o controle judicial de políticas públicas: uma análise de como o poder judiciário pode contribuir para a efetivação do direito à saúde na sociedade brasileira. -

Pós-graduação em Direito - FCHS

A frente nacional contra a privatização da s��ude: direito garantido, não se compra, não se vende

Pós-graduação em Serviço Social - FCHS

Habitação social em centros urbanos consolidados: análise dialógica desde o percurso do projeto ao uso social: S��o Paulo (Brasil) e Roma (Itália)

Fundação de Amparo à Pesquisa do Estado de S��o Paulo (FAPESP)

A search for anisotropy in the arrival directions of ultra high energy cosmic rays recorded at the Pierre Auger Observatory

Observations of cosmic rays arrival directions made with the Pierre Auger Observatory have previously provided evidence of anisotropy at the 99% CL using the correlation of ultra high energy cosmic rays (UHECRs) with objects drawn from the Veron-Cetty Veron catalog. In this paper we report on the use of three catalog independent methods to search for anisotropy. The 2pt-L, 2pt+ and 3pt methods, each giving a different measure of self-clustering in arrival directions, were tested on mock cosmic ray data sets to study the impacts of sample size and magnetic smearing on their results, accounting for both angular and energy resolutions. If the sources of UHECRs follow the same large scale structure as ordinary galaxies in the local Universe and if UHECRs are deflected no more than a few degrees, a study of mock maps suggests that these three method can efficiently respond to the resulting anisotropy with a P-value = 1.0% or smaller with data sets as few as 100 events. using data taken from January 1, 2004 to July 31, 2010 we examined the 20, 30, ... , 110 highest energy events with a corresponding minimum energy threshold of about 49.3 EeV. The minimum P-values found were 13.5% using the 2pt-L method, 1.0% using the 2pt+ method and 1.1% using the 3pt method for the highest 100 energy events. In view of the multiple (correlated) scans performed on the data set, these catalog-independent methods do not yield strong evidence of anisotropy in the highest energy cosmic rays.

The rapid atmospheric monitoring system of the Pierre Auger Observatory

The Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 10(17) eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals ranging from several minutes (for cloud identification) to several hours (for aerosol conditions) to several days (for vertical profiles of temperature, pressure, and humidity). In 2009, the monitoring program was upgraded to allow for additional targeted measurements of atmospheric conditions shortly after the detection of air showers of special interest, e. g., showers produced by very high-energy cosmic rays or showers with atypical longitudinal profiles. The former events are of particular importance for the determination of the energy scale of the Observatory, and the latter are characteristic of unusual air shower physics or exotic primary particle types. The purpose of targeted (or "rapid") monitoring is to improve the resolution of the atmospheric measurements for such events. In this paper, we report on the implementation of the rapid monitoring program and its current status. The rapid monitoring data have been analyzed and applied to the reconstruction of air showers of high interest, and indicate that the air fluorescence measurements affected by clouds and aerosols are effectively corrected using measurements from the regular atmospheric monitoring program. We find that the rapid monitoring program has potential for supporting dedicated physics analyses beyond the standard event reconstruction.

SEARCH FOR POINT-LIKE SOURCES OF ULTRA-HIGH ENERGY NEUTRINOS AT THE PIERRE AUGER OBSERVATORY AND IMPROVED LIMIT ON THE DIFFUSE FLUX OF TAU NEUTRINOS

The surface detector array of the Pierre Auger Observatory can detect neutrinos with energy E-nu between 10(17) eV and 10(20) eV from point-like sources across the sky south of +55 degrees and north of -65 degrees declinations. A search has been performed for highly inclined extensive air showers produced by the interaction of neutrinos of all flavors in the atmosphere (downward-going neutrinos), and by the decay of tau leptons originating from tau neutrino interactions in Earth's crust (Earth-skimming neutrinos). No candidate neutrinos have been found in data up to 2010 May 31. This corresponds to an equivalent exposure of similar to 3.5 years of a full surface detector array for the Earth-skimming channel and similar to 2 years for the downward-going channel. An improved upper limit on the diffuse flux of tau neutrinos has been derived. Upper limits on the neutrino flux from point-like sources have been derived as a function of the source declination. Assuming a differential neutrino flux k(PS) . E-nu(-2). from a point-like source, 90% confidence level upper limits for k(PS) at the level of approximate to 5x10(-7) and 2.5x10(-6) GeV cm(-2) s(-1) have been obtained over a broad range of declinations from the searches for Earth-skimming and downward-going neutrinos, respectively.

A search for point sources of EeV neutrons

A thorough search of the sky exposed at the Pierre Auger Cosmic Ray Observatory reveals no statistically significant excess of events in any small solid angle that would be indicative of a flux of neutral particles from a discrete source. The search covers from -90 degrees to +15 degrees in declination using four different energy ranges above 1 EeV (10(18) eV). The method used in this search is more sensitive to neutrons than to photons. The upper limit on a neutron flux is derived for a dense grid of directions for each of the four energy ranges. These results constrain scenarios for the production of ultrahigh energy cosmic rays in the Galaxy.

LARGE-SCALE DISTRIBUTION OF ARRIVAL DIRECTIONS OF COSMIC RAYS DETECTED ABOVE 10(18) eV AT THE PIERRE AUGER OBSERVATORY

A thorough search for large-scale anisotropies in the distribution of arrival directions of cosmic rays detected above 10(18) eV at the Pierre Auger Observatory is presented. This search is performed as a function of both declination and right ascension in several energy ranges above 10(18) eV, and reported in terms of dipolar and quadrupolar coefficients. Within the systematic uncertainties, no significant deviation from isotropy is revealed. Assuming that any cosmic-ray anisotropy is dominated by dipole and quadrupole moments in this energy range, upper limits on their amplitudes are derived. These upper limits allow us to test the origin of cosmic rays above 10(18) eV from stationary Galactic sources densely distributed in the Galactic disk and predominantly emitting light particles in all directions.

Measurement of the proton-air cross section at root s=57 TeV with the Pierre Auger Observatory

We report a measurement of the proton-air cross section for particle production at the center-of-mass energy per nucleon of 57 TeV. This is derived from the distribution of the depths of shower maxima observed with the Pierre Auger Observatory: systematic uncertainties are studied in detail. Analyzing the tail of the distribution of the shower maxima, a proton-air cross section of [505 +/- 22(stat)(-36)(+28)(syst)] mb is found.

Sviluppo di metodologie per l'analisi in tempo reale delle prestazioni di un motore automobilistico

Durante il periodo di dottorato, l’attività di ricerca di cui mi sono occupato è stata finalizzata allo sviluppo di metodologie per la diagnostica e l’analisi delle prestazioni di un motore automobilistico. Un primo filone di ricerca è relativo allo sviluppo di strategie per l’identificazione delle mancate combustioni (misfires) in un motore a benzina. La sperimentazione si è svolta nella sala prove della Facoltà di Ingegneria dell’Università di Bologna, nei quali è presente un motore Fiat 1.200 Fire, accoppiato ad un freno a correnti parassite, e comandato da una centralina virtuale, creata mediante un modello Simulink, ed interfacciata al motore tramite una scheda di input/output dSpace. Per quanto riguarda la campagna sperimentale, sono stati realizzati delle prove al banco in diverse condizioni di funzionamento (sia stazionarie, che transitorie), durante le quali sono stati indotti dei misfires, sia singoli che multipli. Durante tali test sono stati registrati i segnali provenienti sia dalla ruota fonica usata per il controllo motore (che, nel caso in esame, era affacciata al volano), sia da quella collegata al freno a correnti parassite. Partendo da tali segnali, ed utilizzando un modello torsionale del sistema motoregiunto-freno, è possibile ottenere una stima sia della coppia motrice erogata dal motore, sia della coppia resistente dissipata dal freno. La prontezza di risposta di tali osservatori è tale da garantirci la possibilità di effettuare una diagnosi misfire. In particolare, si è visto che l’indice meglio correlato ala mancata combustione risultaessere la differenza fra la coppia motrice e la coppia resistente; tale indice risulta inoltre essere quello più semplice da calibrare sperimentalmente, in quanto non dipende dalle caratteristiche del giunto, ma solamente dalle inerzie del sistema. Una seconda attività della quale mi sono occupato è relativa alla stima della coppia indicata in un motore diesel automobilistico. A tale scopo, è stata realizzata una campagna sperimentale presso i laboratori della Magneti Marelli Powertrain (Bologna), nella quale sono state effettuati test in molteplici punti motori, sia in condizioni di funzionamento “nominale”, sia variando artificiosamente alcuni dei fattori di controllo (quali Start of Injection, pressione nel rail e, nei punti ove è stato possibile, tasso di EGR e pressione di sovralimentazione), sia effettuando degli sbilanciamenti di combustibile fra un cilindro e l’altro. Utilizzando il solo segnale proveniente da una ruota fonica posta sul lato motore, e sfruttando un modello torsionale simile a quello utilizzato nella campagna di prove relativa alla diagnosi del misfire, è possibile correlare la componente armonica con frequenza di combustione della velocità all’armonica di pari ordine della coppia indicata; una volta stimata tale componente in frequenza, mediante un’analisi di tipo statistico, è possibile eseguire una stima della coppia indicata erogata dal motore. A completamento dell’algoritmo, sfruttando l’analisi delle altre componenti armoniche presenti nel segnale, è possibile avere una stima dello sbilanciamento di coppia fra i vari cilindri. Per la verifica dei risultati ottenuti, sono stati acquisiti i segnali di pressione provenienti da tutti e quattro i cilindri del motore in esame.