Una rassegna di protocolli di routing per reti radio cognitive ad hoc

Questa tesi si propone di presentare e classificare per caratteristiche simili i protocolli di routing che ad oggi sono utilizzati nelle Cognitive Radio Ad Hoc Networks. Pertanto dapprima nel Capitolo 1 si introdurranno le radio cognitive con i concetti che sono alla base di questa tecnologia e le principali motivazioni che hanno portato alla loro nascita e poi al loro sviluppo. Nel Capitolo 2 si parlerà delle cognitive networks o meglio delle cognitive radio networks, e delle loro peculiarità. Nel terzo e nel quarto capitolo si affronteranno le CRAHNs e in particolare quali sono le sfide a cui devono far fronte i protocolli di routing che operano su di essa, partendo dall'esaminare quali sono le differenze che distinguono questa tipologia di rete da una classica rete wireless ad hoc con nodi in grado di muoversi nello spazio (una MANET). Infine nell'ultimo capitolo si cercherà di classificare i protocolli in base ad alcune loro caratteristiche, vedendo poi più nel dettaglio alcuni tra i protocolli più usati.

Essays on vessel emissions and externality costs in Las Palmas Port

Doctorado en la Insularidad : Turismo, interculturalidad y desarrollo sostenible

Radio via Web per le Università: un approccio alle infrastrutture tecnologiche

Linea guida per lo sviluppo e la messa in opera di una Web Radio istituzionale per le Università, completa di confronti con altre Web Radio universitare e descrizione di una funzionalità sviluppata.

Analysis of the nuclear properties of Brightest Cluster Galaxies and comparison with "normal" radio galaxies.

The aim of this PhD thesis is the study of the nuclear properties of radio loud AGN. Multiple and/or recent mergers in the host galaxy and/or the presence of cool core in galaxy clusters can play a role in the formation and evolution of the radio source. Being a unique class of objects (Lin & Mohr 2004), we focus on Brightest Cluster Galaxies (BCGs). We investigate their parsec scale radio emission with VLBI (Very Long Baseline Interferometer) observations. From literature or new data , we collect and analyse VLBA (Very Long Baseline) observations at 5 GHz of a complete sample of BCGs and ``normal'' radio galaxies (Bologna Complete Sample , BCS). Results on nuclear properties of BCGs are coming from the comparison with the results for the Bologna COmplete Sample (BCS). Our analysis finds a possible dichotomy between BCGs in cool-core clusters and those in non-cool-core clusters. Only one-sided BCGs have similar kinematic properties with FRIs. Furthermore, the dominance of two-sided jet structures only in cooling clusters suggests sub-relativistic jet velocities. The different jet properties can be related to a different jet origin or to the interaction with a different ISM. We larger discuss on possible explanation of this.

Very Long Baseline Interferometry in Italy Wide-field VLBI imaging and astrometry and prospects for an Italian VLBI network including the Sardinia Radio Telescope

In this thesis the use of widefield imaging techniques and VLBI observations with a limited number of antennas are explored. I present techniques to efficiently and accurately image extremely large UV datasets. Very large VLBI datasets must be reduced into multiple, smaller datasets if today’s imaging algorithms are to be used to image them. I present a procedure for accurately shifting the phase centre of a visibility dataset. This procedure has been thoroughly tested and found to be almost two orders of magnitude more accurate than existing techniques. Errors have been found at the level of one part in 1.1 million. These are unlikely to be measurable except in the very largest UV datasets. Results of a four-station VLBI observation of a field containing multiple sources are presented. A 13 gigapixel image was constructed to search for sources across the entire primary beam of the array by generating over 700 smaller UV datasets. The source 1320+299A was detected and its astrometric position with respect to the calibrator J1329+3154 is presented. Various techniques for phase calibration and imaging across this field are explored including using the detected source as an in-beam calibrator and peeling of distant confusing sources from VLBI visibility datasets. A range of issues pertaining to wide-field VLBI have been explored including; parameterising the wide-field performance of VLBI arrays; estimating the sensitivity across the primary beam both for homogeneous and heterogeneous arrays; applying techniques such as mosaicing and primary beam correction to VLBI observations; quantifying the effects of time-average and bandwidth smearing; and calibration and imaging of wide-field VLBI datasets. The performance of a computer cluster at the Istituto di Radioastronomia in Bologna has been characterised with regard to its ability to correlate using the DiFX software correlator. Using existing software it was possible to characterise the network speed particularly for MPI applications. The capabilities of the DiFX software correlator, running on this cluster, were measured for a range of observation parameters and were shown to be commensurate with the generic performance parameters measured. The feasibility of an Italian VLBI array has been explored, with discussion of the infrastructure required, the performance of such an array, possible collaborations, and science which could be achieved. Results from a 22 GHz calibrator survey are also presented. 21 out of 33 sources were detected on a single baseline between two Italian antennas (Medicina to Noto). The results and discussions presented in this thesis suggest that wide-field VLBI is a technique whose time has finally come. Prospects for exciting new science are discussed in the final chapter.

Emissions of volatile organic compounds from tropical savanna vegetation and biomass burning

This dissertation focuses on characterizing the emissions of volatile organic compounds (VOCs) from grasses and young trees, and the burning of biomass mainly from Africa and Indonesia. The measurements were performed with a proton-transfer-reaction mass spectrometer (PTR-MS). The biogenic emissions of tropical savanna vegetation were studied in Calabozo (Venezuela). Two field campaigns were carried out, the first during the wet season (1999) and the second during the dry season (2000). Three grass species were studied: T. plumosus, H. rufa and A. canescens, and the tree species B. crassifolia, C. americana and C. vitifolium. The emission rates were determined with a dynamic plant enclosure system. In general, the emissions increased exponentially with increasing temperature and solar radiation. Therefore, the emission rates showed high variability. Consequently, the data were normalized to a standard temperature of 30°C, and standard emission rates thus determined allowed for interspecific and seasonal comparisons. The range of average daytime (10:00-16:00) emission rates of total VOCs measured from green (mature and young) grasses was between 510-960 ngC/g/h. Methanol was the primary emission (140-360 ngC/g/h), followed by acetaldehyde, butene and butanol and acetone with emission rates between 70-200 ngC/g/h. The emissions of propene and methyl ethyl ketone (MEK) were <80 ngC/g/h, and those of isoprene and C5-alcohols were between 10-130 ngC/g/h. The oxygenated species represented 70-75% of the total. The emission of VOCs was found to vary by up to a factor of three between plants of the same species, and by up to a factor of two between the different species. The annual source of methanol from savanna grasses worldwide estimated in this work was 3 to 4.4 TgC, which could represent up to 12% of the current estimated global emission from terrestrial vegetation. Two of the studied tree species, were isoprene emitters, and isoprene was also their primary emission (which accounted for 70-94% of the total carbon emitted) followed by methanol and butene + butanol. The daytime average emission rate of isoprene measured in the wet season was 27 mgC/g/h for B. crassifolia, and 123 mgC/g/h for C. vitifolium. The daytime emissions of methanol and butene + butanol were between 0.3 and 2 mgC/g/h. The total sum of VOCs emission measured during the day in the wet season was between 30 and 130 mgC/g/h. In the dry season, in contrast, the methanol emissions from C. vitifolium saplings –whose leaves were still developing– were an order of magnitude higher than in the wet season (15 mgC/g/h). The isoprene emission from B. crassifolia in the dry season was comparable to the emission in the wet season, whereas isoprene emission from C. vitifolium was about a factor of three lower (~43 mgC/g/h). Biogenic emission inventories show that isoprenoids are the most prominent and best-studied compounds. The standard emission rates of isoprene and monoterpenes of the measured savanna trees were in the lower end of the range found in the literature. The emission of other biogenic VOCs has been sparsely investigated, but in general, the standard emissions from trees studied here were within the range observed in previous investigations. The biomass burning study comprised the measurement of VOCs and other trace-gas emissions of 44 fires from 15 different fuel types, primarily from Africa and Indonesia, in a combustion laboratory. The average sum of emissions (excluding CO2, CO and NO) from African fuels was ~18 g(VOC)/kg. Six of the ten most important emissions were oxygenated VOCs. Acetic acid was the major emission, followed by methanol and formaldehyde. The emission of methane was of the same order as the methanol emission (~5 g/kg), and that of nitrogen-containing compounds was ~1 g/kg. An estimate of the VOC source from biomass burning of savannas and grasslands worldwide suggests that the sum of emissions is about 56 Tg/yr, of which 34 Tg correspond to oxygenated VOCs, 14 Tg to unsaturated and aromatic compounds, 5 Tg to methane and 3 Tg to N-compounds. The estimated emissions of CO, CO2 and NO are 216, 5117 and 9.4 Tg/yr, respectively. The emission factors reported here for Indonesian fuels are the first results of laboratory fires using Indonesian fuels. Acetic acid was the highest organic emission, followed by acetol, a compound not previously reported in smoke, methane, mass 97 (tentatively identified as furfural, dimethylfuran and ethylfuran), and methanol. The sum of total emissions of Indonesian fuels was 91 g/kg, which is 5 times higher than the emissions from African fuels. The results of this study reinforces the importance of oxygenated compounds. Due to the vast area covered by tropical savannas worldwide, the biogenic and biomass burning emission of methanol and other oxygenated compounds may be important for the regional and even global tropospheric chemistry.

Die 18 F-Fluorierung verschiedener Aminosäuren als Tracer für die Tumor-Diagnostik mittels Positronen-Emissions-Tomographie

Die Zielsetzung dieser Arbeit war die Synthese und Markierung, sowie die in vitro- und in vivo-Evaluierung zweier markierter Aminosäure. Es wurden die PET-Tumor-Tracer C1-(2-[18F]Fluoreth- ylamino)-asparagin und S-2-Amino-4-[18F]fluor-butansäure synthetisiert. Die Markierung zum C1-(2-[18F]Fluorethylamino)-asparagin wurde mit 2-[18F]Fluorethylamin als Precursor durchgeführt. Ausgehend von N,N-Dibenzyl-(2-bromethyl)-amin wurde zunächst N,N-Dibenzyl-(2-[18F]fluorethyl)-amin in einer nukleophilen Substiution mit [18F]Fluorid in Acetonitril bei 80 °C mit einer Reaktionsdauer von 5 min dargestellt. Zur Abtrennung überschüssigen [18F]Fluorids wurde das Roh-Produkt auf einer Sep-Pak Plus Kartusche (C18) fixiert und mit Acetonitril eluiert. Die Abspaltung der Benzyl-Schutzgruppen erfolgte durch die Zugabe von Pd/C zu dem eluierten N,N-Dibenzyl-(2-[18F]fluorethyl)-amin und Behandelung der Lösung im leichten Wasserstoffstrom. Im finalen Aufreinigungsschritt wird der Katalysator Pd/C mittels eines Membranfilters abgetrennt. Das 2-[18F]Fluorethylamin wird im Sauren in das Amino-Salz überführt und im Vakuum vom Lösungsmittel befreit. Die Markierung zum C1-(2-[18F]Fluorethylamino)-asparagin wurde in DMF durchgeführt. Die höchsten Ausbeuten werden nach 4 min bei 60 °C erhalten. Die Abspaltung der Schutzgruppe erfolgt durch Trifluoressigsäure bei Raumtemperatur in 8 min. Die Aufreinigung des C1-(2-[18F]Fluorethylamino)-asparagin mittels HPLC und Festphasenextraktion liegt das Produkt in einer isotonischne isotonischen Kochsalzlösung vor. Die in vitro-Versuche wurden mit C1-(2-[18F]Fluorethylamino)-asparagin an 5 verschiedenen Zelllinen durchgeführt, 3 Plattenepitele und 2 Melanome. Hierbei konnte eine erhöhte Akkumulation von C1 -(2-[18F]Fluorethylamino)-asparagin beobachtet werden, die innerhalb von 20 min einen konstanten Wert erreicht. Ein Blockade-Experiment zeigte, dass sich die Aufnahme von C1 -(2-[18F]Fluorethylamino)-asparagin durch gesättinge Asparagin-Lösung bei den Plattenepitelen gar nicht und bei den Melanomen nur leicht vermindern ließ. Da die Aufnahme von C1-(2-[18F]Fluorethylamino)-asparagin in die Zellen höher war als bei FDG bei dem gleichen Versuchsaufbau, wurden in vivo-Versuche angesetzt. Die in vivo-Versuche an Sprague Dawley Ratten mit C1-(2-[18 F]Fluorethylamino)-asparagin zeigten keine messbare Anreicherung von C1-(2-[18F]Fluorethylamino)-asparagin in Tumoren. Fast die komplette Aktivität wurde in der Niere und Blase wiedergefunden. Die Synthese von S-2-Amino-4-[18F]fluor-butansäure wurde über stereodirigierende Auxilliare realisiert. Dazu wurden die geeignetsten Auxillare ausgewählt und auf ihre Eignung verglichen. Der Vergleich der stereodirigierenden Auxilare zeigte, dass das (1R,2R,5R)-2-Hydroxy-2,6,6-trimethyl- bicyclo[3.1.1]hept-3-ylidenamino)-essigsäure tert.-butylester (Laue-Auxillar) am geeignetesten ist. Die 18F-Markierung von S-2-Amino-4-[18F]fluor-butansäure wurde so optimiert, dass eine möglichst hohe stereochemische Reinheit des Produktes erzielt wird. Die optische Reinheit von S-2-Amino-4-[18 F]fluor-butansäure wurde mit > 93 % ee berechnet. Die Synthese des Markierungsvorläufers wurde ausgehend vom Laue-Auxilliar aufgebaut. Als Abgangsgruppe hat sich die Tosylgruppe besonders bewährt. Sie lässt sich unter besonders schonenden Bedingungen in den säurelabilen (1R,2R,5R)-4-Hydroxy-2-(2-hydroxy-2,6,6-trimethyl-bi- cyclo[3.1.1]hept-3-ylidenamino) butansäure tert.-butylester einführen. Bei der 18F-Markierung von S-2-Amino-4-[18F]fluor-butansäure mittels n.c.a. [18F]Fluorid hat sich die Wahl des Basensystems als besonders wichtig erwiesen. Die maximale Ausbeuten von 55% wurde mit Oxalat als Basensystem in Acetonitril bei 80 °C und einer Reaktionszeit von 15 min erzielen. Die Abspaltung der Schutzgruppen und die Abtrennung des Produktes wird in mehreren Schritten durchgeführt einschließlich einer HPLC-Abtrennung. Es wird nach 150 min Synthesedauer das gereinigte S-2-Amino-4-[18F]fluor-butansäure in isotonischer Kochsalzlösung mit einer Ausbeute von > 10 % RCA erhalten. Bei in vivo-Versuchen an Sprague Dawley Ratten reicherte sich der Hauptteil der Aktivität in der Niere an und nur weniger als ein halbes Prozent der applizierten Aktivität fand sich in den Tumoren wieder. Nach 10 min wurde ein maximaler Wert erreicht, der sich bis zum Ende der Messung nicht verändert. Das Verhältnis von Tumoraktivität zu unspezifisch-gebundener Aktivität betrug 2,2. Damit liegt das Verhältnis im Bereich der meisten klinisch eingesetzten PET-Tumor-Tracer wie dem des O-(2-[18F]Fluorethyl)-L-tyrosin mit 1,5.

Magnetic fields around radio galaxies from Faraday rotation measure analysis

The purpose of this thesis is to investigate the strength and structure of the magnetized medium surrounding radio galaxies via observations of the Faraday effect. This study is based on an analysis of the polarization properties of radio galaxies selected to have a range of morphologies (elongated tails, or lobes with small axial ratios) and to be located in a variety of environments (from rich cluster core to small group). The targets include famous objects like M84 and M87. A key aspect of this work is the combination of accurate radio imaging with high-quality X-ray data for the gas surrounding the sources. Although the focus of this thesis is primarily observational, I developed analytical models and performed two- and three-dimensional numerical simulations of magnetic fields. The steps of the thesis are: (a) to analyze new and archival observations of Faraday rotation measure (RM) across radio galaxies and (b) to interpret these and existing RM images using sophisticated two and three-dimensional Monte Carlo simulations. The approach has been to select a few bright, very extended and highly polarized radio galaxies. This is essential to have high signal-to-noise in polarization over large enough areas to allow computation of spatial statistics such as the structure function (and hence the power spectrum) of rotation measure, which requires a large number of independent measurements. New and archival Very Large Array observations of the target sources have been analyzed in combination with high-quality X-ray data from the Chandra, XMM-Newton and ROSAT satellites. The work has been carried out by making use of: 1) Analytical predictions of the RM structure functions to quantify the RM statistics and to constrain the power spectra of the RM and magnetic field. 2) Two-dimensional Monte Carlo simulations to address the effect of an incomplete sampling of RM distribution and so to determine errors for the power spectra. 3) Methods to combine measurements of RM and depolarization in order to constrain the magnetic-field power spectrum on small scales. 4) Three-dimensional models of the group/cluster environments, including different magnetic field power spectra and gas density distributions. This thesis has shown that the magnetized medium surrounding radio galaxies appears more complicated than was apparent from earlier work. Three distinct types of magnetic-field structure are identified: an isotropic component with large-scale fluctuations, plausibly associated with the intergalactic medium not affected by the presence of a radio source; a well-ordered field draped around the front ends of the radio lobes and a field with small-scale fluctuations in rims of compressed gas surrounding the inner lobes, perhaps associated with a mixing layer.

The gaseous environment of radio galaxies: a new perspective from high-resolution x-ray spectroscopy

It is known that massive black holes have a profound effect on the evolution of galaxies, and possibly on their formation by regulating the amount of gas available for the star formation. However, how black hole and galaxies communicate is still an open problem, depending on how much of the energy released interacts with the circumnuclear matter. In the last years, most studies of feedback have primarily focused on AGN jet/cavity systems in the most massive galaxy clusters. This thesis intends to investigate the feedback phenomena in radio--loud AGNs from a different perspective studying isolated radio galaxies, through high-resolution spectroscopy. In particular one NLRG and three BLRG are studied, searching for warm gas, both in emission and absorption, in the soft X-ray band. I show that the soft spectrum of 3C33 originates from gas photoionized by the central engine. I found for the first time WA in 3C382 and 3C390.3. I show that the observed warm emitter/absorbers is not uniform and probably located in the NLR. The detected WA is slow implying a mass outflow rate and kinetic luminosity always well below 1% the L(acc) as well as the P(jet). Finally the radio--loud properties are compared with those of type 1 RQ AGNs. A positive correlation is found between the mass outflow rate/kinetic luminosity, and the radio loudness. This seems to suggest that the presence of a radio source (the jet?) affects the distribution of the absorbing gas. Alternatively, if the gas distribution is similar in Seyferts and radio galaxies, the M(out) vs rl relation could simply indicate a major ejection of matter in the form of wind in powerful radio AGNs.