KRONBERGER 49: A NEW LOW-MASS GLOBULAR CLUSTER OR AN UNPRECEDENTED BULGE WINDOW?

We employ optical and near-infrared photometry to study the stars in the direction of the star cluster candidate Kronberger 49. The optical color-magnitude diagrams (V, I, and Gunn z photometry obtained with the Galileo Telescope) are tight and present evidence of a main-sequence turnoff. We may be dealing with a low-mass, metal-rich globular cluster located in the bulge at a distance from the Sun of d(circle dot) = 8 +/- 1 kpc. Alternatively, it may be a dust hole through which we are sampling the bulge stellar population affected by a very low amount of differential reddening.

THE INFRARED COLORS OF THE SUN

Solar infrared colors provide powerful constraints on the stellar effective temperature scale, but they must be measured with both accuracy and precision in order to do so. We fulfill this requirement by using line-depth ratios to derive in a model-independent way the infrared colors of the Sun, and we use the latter to test the zero point of the Casagrande et al. effective temperature scale, confirming its accuracy. Solar colors in the widely used Two Micron All Sky Survey (2MASS) JHK(s) and WISE W1-4 systems are provided: (V - J)(circle dot) = 1.198, (V - H)(circle dot) = 1.484, (V - K-s)(circle dot) = 1.560, (J - H)(circle dot) = 0.286, (J - K-s)(circle dot) = 0.362, (H - K-s)(circle dot) = 0.076, (V - W1)(circle dot) = 1.608, (V - W2)(circle dot) = 1.563, (V - W3)(circle dot) = 1.552, and (V - W4)(circle dot) = 1.604. A cross-check of the effective temperatures derived implementing 2MASS or WISE magnitudes in the infrared flux method confirms that the absolute calibration of the two systems agrees within the errors, possibly suggesting a 1% offset between the two, thus validating extant near-and mid-infrared absolute calibrations. While 2MASS magnitudes are usually well suited to derive T-eff, we find that a number of bright, solar-like stars exhibit anomalous WISE colors. In most cases, this effect is spurious and can be attributed to lower-quality measurements, although for a couple of objects (3%+/- 2% of the total sample) it might be real, and may hint at the presence of warm/hot debris disks.

OXYGEN ABUNDANCES IN LOW- AND HIGH-alpha FIELD HALO STARS AND THE DISCOVERY OF TWO FIELD STARS BORN IN GLOBULAR CLUSTERS

Oxygen abundances of 67 dwarf stars in the metallicity range -1.6 < [Fe/H] < -0.4 are derived from a non-LTE analysis of the 777 nm O I triplet lines. These stars have precise atmospheric parameters measured by Nissen and Schuster, who find that they separate into three groups based on their kinematics and alpha-element (Mg, Si, Ca, Ti) abundances: thick disk, high-alpha halo, and low-alpha halo. We find the oxygen abundance trends of thick-disk and high-alpha halo stars very similar. The low-alpha stars show a larger star-to-star scatter in [O/Fe] at a given [Fe/H] and have systematically lower oxygen abundances compared to the other two groups. Thus, we find the behavior of oxygen abundances in these groups of stars similar to that of the a elements. We use previously published oxygen abundance data of disk and very metal-poor halo stars to present an overall view (-2.3 < [Fe/H] < +0.3) of oxygen abundance trends of stars in the solar neighborhood. Two field halo dwarf stars stand out in their O and Na abundances. Both G53-41 and G150-40 have very low oxygen and very high sodium abundances, which are key signatures of the abundance anomalies observed in globular cluster (GC) stars. Therefore, they are likely field halo stars born in GCs. If true, we estimate that at least 3% +/- 2% of the local field metal-poor star population was born in GCs.

The relationship between gamma Cassiopeiae's X-ray emission and its circumstellar environment

gamma Cas is the prototypical classical Be star and is recently best known for its variable hard X-ray emission. To elucidate the reasons for this emission, we mounted a multiwavelength campaign in 2010 centered around four XMM-Newton observations. The observational techniques included long baseline optical interferometry (LBOI) from two instruments at CHARA, photometry carried out by an automated photometric telescope and H alpha observations. Because gamma Cas is also known to be in a binary, we measured radial velocities from the H alpha line and redetermined its period as 203.55 +/- 0.20 days and its eccentricity as near zero. The LBOI observations suggest that the star's decretion disk was axisymmetric in 2010, has an system inclination angle near 45 degrees, and a larger radius than previously reported. In addition, the Be star began an "outburst" at the beginning of our campaign, made visible by a brightening and reddening of the disk during our campaign and beyond. Our analyses of the new high resolution spectra disclosed many attributes also found from spectra obtained in 2001 (Chandra) and 2004 (XMM-Newton). As well as a dominant hot (approximate to 14 keV) thermal component, the familiar attributes included: (i) a fluorescent feature of Fe K even stronger than observed at previous times; (ii) strong lines of N VII and Ne XI lines indicative of overabundances; and (iii) a subsolar Fe abundance from K-shell lines but a solar abundance from L-shell ions. We also found that two absorption columns are required to fit the continuum. While the first one maintained its historical average of 1 x 10(21) cm(-2), the second was very large and doubled to 7.4 x 10(23) cm(-2) during our X-ray observations. Although we found no clear relation between this column density and orbital phase, it correlates well with the disk brightening and reddening both in the 2010 and earlier observations. Thus, the inference from this study is that much (perhaps all?) of the X-ray emission from this source originates behind matter ejected by gamma Cas into our line of sight.

High precision astrometry mission for the detection and characterization of nearby habitable planetary systems with the Nearby Earth Astrometric Telescope (NEAT)

A complete census of planetary systems around a volume-limited sample of solar-type stars (FGK dwarfs) in the Solar neighborhood (d a parts per thousand currency signaEuro parts per thousand 15 pc) with uniform sensitivity down to Earth-mass planets within their Habitable Zones out to several AUs would be a major milestone in extrasolar planets astrophysics. This fundamental goal can be achieved with a mission concept such as NEAT-the Nearby Earth Astrometric Telescope. NEAT is designed to carry out space-borne extremely-high-precision astrometric measurements at the 0.05 mu as (1 sigma) accuracy level, sufficient to detect dynamical effects due to orbiting planets of mass even lower than Earth's around the nearest stars. Such a survey mission would provide the actual planetary masses and the full orbital geometry for all the components of the detected planetary systems down to the Earth-mass limit. The NEAT performance limits can be achieved by carrying out differential astrometry between the targets and a set of suitable reference stars in the field. The NEAT instrument design consists of an off-axis parabola single-mirror telescope (D = 1 m), a detector with a large field of view located 40 m away from the telescope and made of 8 small movable CCDs located around a fixed central CCD, and an interferometric calibration system monitoring dynamical Young's fringes originating from metrology fibers located at the primary mirror. The mission profile is driven by the fact that the two main modules of the payload, the telescope and the focal plane, must be located 40 m away leading to the choice of a formation flying option as the reference mission, and of a deployable boom option as an alternative choice. The proposed mission architecture relies on the use of two satellites, of about 700 kg each, operating at L2 for 5 years, flying in formation and offering a capability of more than 20,000 reconfigurations. The two satellites will be launched in a stacked configuration using a Soyuz ST launch vehicle. The NEAT primary science program will encompass an astrometric survey of our 200 closest F-, G- and K-type stellar neighbors, with an average of 50 visits each distributed over the nominal mission duration. The main survey operation will use approximately 70% of the mission lifetime. The remaining 30% of NEAT observing time might be allocated, for example, to improve the characterization of the architecture of selected planetary systems around nearby targets of specific interest (low-mass stars, young stars, etc.) discovered by Gaia, ground-based high-precision radial-velocity surveys, and other programs. With its exquisite, surgical astrometric precision, NEAT holds the promise to provide the first thorough census for Earth-mass planets around stars in the immediate vicinity of our Sun.

THE SLOAN DIGITAL SKY SURVEY CO-ADD: A GALAXY PHOTOMETRIC REDSHIFT CATALOG

We present and describe a catalog of galaxy photometric redshifts (photo-z) for the Sloan Digital Sky Survey (SDSS) Co-add Data. We use the artificial neural network (ANN) technique to calculate the photo-z and the nearest neighbor error method to estimate photo-z errors for similar to 13 million objects classified as galaxies in the co-add with r < 24.5. The photo-z and photo-z error estimators are trained and validated on a sample of similar to 83,000 galaxies that have SDSS photometry and spectroscopic redshifts measured by the SDSS Data Release 7 (DR7), the Canadian Network for Observational Cosmology Field Galaxy Survey, the Deep Extragalactic Evolutionary Probe Data Release 3, the VIsible imaging Multi-Object Spectrograph-Very Large Telescope Deep Survey, and the WiggleZ Dark Energy Survey. For the best ANN methods we have tried, we find that 68% of the galaxies in the validation set have a photo-z error smaller than sigma(68) = 0.031. After presenting our results and quality tests, we provide a short guide for users accessing the public data.

The peculiar isolated neutron star in the Carina Nebula Deep XMM-Newton and ESO-VLT observations of 2XMM J104608.7-594306

While fewer in number than the dominant rotation-powered radio pulsar population, peculiar classes of isolated neutron stars (INSs) which include magnetars, the ROSAT-discovered "Magnificent Seven" (M7), rotating radio transients (RRATs), and central compact objects in supernova remnants (CCOs) - represent a key element in understanding the neutron star phenomenology. We report the results of an observational campaign to study the properties of the source 2XMM J104608.7-594306, a newly discovered thermally emitting INS. The evolutionary state of the neutron star is investigated by means of deep dedicated observations obtained with the XMM-Newton Observatory, the ESO Very Large Telescope, as well as publicly available gamma-ray data from the Fermi Space Telescope and the AGILE Mission. The observations confirm previous expectations and reveal a unique type of object. The source, which is likely within the Carina Nebula (N-H = 2.6x10(21) cm(-2)), has a spectrum that is both thermal and soft, with kT(infinity) = 135 eV. Non-thermal (magnetospheric) emission is not detected down to 1% (3 sigma, 0.1-12 keV) of the source luminosity. Significant deviations (absorption features) from a simple blackbody model are identified in the spectrum of the source around energies 0.6 keV and 1.35 keV. While the former deviation is likely related to a local oxygen overabundance in the Carina Nebula, the latter can only be accounted for by an additional spectral component, which is modelled as a Gaussian line in absorption with EW = 91 eV and sigma = 0.14 keV (1 sigma). Furthermore, the optical counterpart is fainter than m(V) = 27 (2 sigma) and no gamma-ray emission is significantly detected by either the Fermi or AGILE missions. Very interestingly, while these characteristics are remarkably similar to those of the M7 or the only RRAT so far detected in X-rays, which all have spin periods of a few seconds, we found intriguing evidence of very rapid rotation, P = 18.6ms, at the 4 sigma confidence level. We interpret these new results in the light of the observed properties of the currently known neutron star population, in particular those of standard rotation-powered pulsars, recycled objects, and CCOs. We find that none of these scenarios can satisfactorily explain the collective properties of 2XMM J104608.7-594306, although it may be related to the still poorly known class of Galactic anti-magnetars. Future XMM-Newton data, granted for the next cycle of observations (AO11), will help us to improve our current observational interpretation of the source, enabling us to significantly constrain the rate of pulsar spin down.

A new enrichment space for the treatment of discontinuous pressures in multi-fluid flows

In this work, a new enrichment space to accommodate jumps in the pressure field at immersed interfaces in finite element formulations, is proposed. The new enrichment adds two degrees of freedom per element that can be eliminated by means of static condensation. The new space is tested and compared with the classical P1 space and to the space proposed by Ausas et al (Comp. Meth. Appl. Mech. Eng., Vol. 199, 10191031, 2010) in several problems involving jumps in the viscosity and/or the presence of singular forces at interfaces not conforming with the element edges. The combination of this enrichment space with another enrichment that accommodates discontinuities in the pressure gradient has also been explored, exhibiting excellent results in problems involving jumps in the density or the volume forces. Copyright (c) 2011 John Wiley & Sons, Ltd.

Overview of semi-sinusoidal stellar variability with the CoRoT satellite

Context. To date, the CoRoT space mission has produced more than 124 471 light curves. Classifying these curves in terms of unambiguous variab ility behavior is mandatory for obtaining an unbi ased statistical view on th eir controlling root-causes. Aims. The present study provides an overview of semi-sinusoidal light curves observed by the CoRoT exo-field CCDs. Methods. We selected a sample of 4206 light curves presenting well-defined semi-si nusoidal signatures. Th e variability periods were computed based on Lomb-Scargle periodograms, harmonic fits, and visual inspection. Results. Color–period diagrams for the present sample show the trend of an increase of the variability periods as long as the stars evolve. This evolutionary behavior is also noticed when comparing the period distribution in the Galactic center and anti-center directions. These aspect s indicate a compatibility with stellar rotation, although more inform ation is needed to confirm their root- causes. Considering this possi bility, we identified a subset of th ree Sun-like candidates by their photometric peri od. Finally, the variability period versus color diagr am behavior was found to be highly depe ndent on the reddening correction.

Identifying clouds over the Pierre Auger Observatory using infrared satellite data

We describe a new method of identifying night-time clouds over the Pierre Auger Observatory using infrared data from the Imager instruments on the GOES-12 and GOES-13 satellites. We compare cloud identifications resulting from our method to those obtained by the Central Laser Facility of the Auger Observatory. Using our new method we can now develop cloud probability maps for the 3000 km2 of the Pierre Auger Observatory twice per hour with a spatial resolution of ∼2.4 km by ∼5.5 km. Our method could also be applied to monitor cloud cover for other ground-based observatories and for space-based observatories.

Utilizzo metrico di immagini panoramiche satellitari CORONA

CAPITOLO 1 INTRODUZIONE Il lavoro presentato è relativo all’utilizzo a fini metrici di immagini satellitari storiche a geometria panoramica; in particolare sono state elaborate immagini satellitari acquisite dalla piattaforma statunitense CORONA, progettata ed impiegata essenzialmente a scopi militari tra gli anni ’60 e ’70 del secolo scorso, e recentemente soggette ad una declassificazione che ne ha consentito l’accesso anche a scopi ed utenti non militari. Il tema del recupero di immagini aeree e satellitari del passato è di grande interesse per un ampio spettro di applicazioni sul territorio, dall’analisi dello sviluppo urbano o in ambito regionale fino ad indagini specifiche locali relative a siti di interesse archeologico, industriale, ambientale. Esiste infatti un grandissimo patrimonio informativo che potrebbe colmare le lacune della documentazione cartografica, di per sé, per ovvi motivi tecnici ed economici, limitata a rappresentare l’evoluzione territoriale in modo asincrono e sporadico, e con “forzature” e limitazioni nel contenuto informativo legate agli scopi ed alle modalità di rappresentazione delle carte nel corso del tempo e per diversi tipi di applicazioni. L’immagine di tipo fotografico offre una rappresentazione completa, ancorché non soggettiva, dell’esistente e può complementare molto efficacemente il dato cartografico o farne le veci laddove questo non esista. La maggior parte del patrimonio di immagini storiche è certamente legata a voli fotogrammetrici che, a partire dai primi decenni del ‘900, hanno interessato vaste aree dei paesi più avanzati, o regioni di interesse a fini bellici. Accanto a queste, ed ovviamente su periodi più vicini a noi, si collocano le immagini acquisite da piattaforma satellitare, tra le quali rivestono un grande interesse quelle realizzate a scopo di spionaggio militare, essendo ad alta risoluzione geometrica e di ottimo dettaglio. Purtroppo, questo ricco patrimonio è ancora oggi in gran parte inaccessibile, anche se recentemente sono state avviate iniziative per permetterne l’accesso a fini civili, in considerazione anche dell’obsolescenza del dato e della disponibilità di altre e migliori fonti di informazione che il moderno telerilevamento ci propone. L’impiego di immagini storiche, siano esse aeree o satellitari, è nella gran parte dei casi di carattere qualitativo, inteso ad investigare sulla presenza o assenza di oggetti o fenomeni, e di rado assume un carattere metrico ed oggettivo, che richiederebbe tra l’altro la conoscenza di dati tecnici (per esempio il certificato di calibrazione nel caso delle camere aerofotogrammetriche) che sono andati perduti o sono inaccessibili. Va ricordato anche che i mezzi di presa dell’epoca erano spesso soggetti a fenomeni di distorsione ottica o altro tipo di degrado delle immagini che ne rendevano difficile un uso metrico. D’altra parte, un utilizzo metrico di queste immagini consentirebbe di conferire all’analisi del territorio e delle modifiche in esso intercorse anche un significato oggettivo che sarebbe essenziale per diversi scopi: per esempio, per potere effettuare misure su oggetti non più esistenti o per potere confrontare con precisione o co-registrare le immagini storiche con quelle attuali opportunamente georeferenziate. Il caso delle immagini Corona è molto interessante, per una serie di specificità che esse presentano: in primo luogo esse associano ad una alta risoluzione (dimensione del pixel a terra fino a 1.80 metri) una ampia copertura a terra (i fotogrammi di alcune missioni coprono strisce lunghe fino a 250 chilometri). Queste due caratteristiche “derivano” dal principio adottato in fase di acquisizione delle immagini stesse, vale a dire la geometria panoramica scelta appunto perché l’unica che consente di associare le due caratteristiche predette e quindi molto indicata ai fini spionaggio. Inoltre, data la numerosità e la frequenza delle missioni all’interno dell’omonimo programma, le serie storiche di questi fotogrammi permettono una ricostruzione “ricca” e “minuziosa” degli assetti territoriali pregressi, data appunto la maggior quantità di informazioni e l’imparzialità associabili ai prodotti fotografici. Va precisato sin dall’inizio come queste immagini, seppur rappresentino una risorsa “storica” notevole (sono datate fra il 1959 ed il 1972 e coprono regioni moto ampie e di grandissimo interesse per analisi territoriali), siano state molto raramente impiegate a scopi metrici. Ciò è probabilmente imputabile al fatto che il loro trattamento a fini metrici non è affatto semplice per tutta una serie di motivi che saranno evidenziati nei capitoli successivi. La sperimentazione condotta nell’ambito della tesi ha avuto due obiettivi primari, uno generale ed uno più particolare: da un lato il tentativo di valutare in senso lato le potenzialità dell’enorme patrimonio rappresentato da tali immagini (reperibili ad un costo basso in confronto a prodotti simili) e dall’altro l’opportunità di indagare la situazione territoriale locale per una zona della Turchia sud orientale (intorno al sito archeologico di Tilmen Höyük) sulla quale è attivo un progetto condotto dall’Università di Bologna (responsabile scientifico il Prof. Nicolò Marchetti del Dipartimento di Archeologia), a cui il DISTART collabora attivamente dal 2005. L’attività è condotta in collaborazione con l’Università di Istanbul ed il Museo Archeologico di Gaziantep. Questo lavoro si inserisce, inoltre, in un’ottica più ampia di quelle esposta, dello studio cioè a carattere regionale della zona in cui si trovano gli scavi archeologici di Tilmen Höyük; la disponibilità di immagini multitemporali su un ampio intervallo temporale, nonché di tipo multi sensore, con dati multispettrali, doterebbe questo studio di strumenti di conoscenza di altissimo interesse per la caratterizzazione dei cambiamenti intercorsi. Per quanto riguarda l’aspetto più generale, mettere a punto una procedura per il trattamento metrico delle immagini CORONA può rivelarsi utile all’intera comunità che ruota attorno al “mondo” dei GIS e del telerilevamento; come prima ricordato tali immagini (che coprono una superficie di quasi due milioni di chilometri quadrati) rappresentano un patrimonio storico fotografico immenso che potrebbe (e dovrebbe) essere utilizzato sia a scopi archeologici, sia come supporto per lo studio, in ambiente GIS, delle dinamiche territoriali di sviluppo di quelle zone in cui sono scarse o addirittura assenti immagini satellitari dati cartografici pregressi. Il lavoro è stato suddiviso in 6 capitoli, di cui il presente costituisce il primo. Il secondo capitolo è stato dedicato alla descrizione sommaria del progetto spaziale CORONA (progetto statunitense condotto a scopo di fotoricognizione del territorio dell’ex Unione Sovietica e delle aree Mediorientali politicamente correlate ad essa); in questa fase vengono riportate notizie in merito alla nascita e all’evoluzione di tale programma, vengono descritti piuttosto dettagliatamente gli aspetti concernenti le ottiche impiegate e le modalità di acquisizione delle immagini, vengono riportati tutti i riferimenti (storici e non) utili a chi volesse approfondire la conoscenza di questo straordinario programma spaziale. Nel terzo capitolo viene presentata una breve discussione in merito alle immagini panoramiche in generale, vale a dire le modalità di acquisizione, gli aspetti geometrici e prospettici alla base del principio panoramico, i pregi ed i difetti di questo tipo di immagini. Vengono inoltre presentati i diversi metodi rintracciabili in bibliografia per la correzione delle immagini panoramiche e quelli impiegati dai diversi autori (pochi per la verità) che hanno scelto di conferire un significato metrico (quindi quantitativo e non solo qualitativo come è accaduto per lungo tempo) alle immagini CORONA. Il quarto capitolo rappresenta una breve descrizione del sito archeologico di Tilmen Höyuk; collocazione geografica, cronologia delle varie campagne di studio che l’hanno riguardato, monumenti e suppellettili rinvenute nell’area e che hanno reso possibili una ricostruzione virtuale dell’aspetto originario della città ed una più profonda comprensione della situazione delle capitali del Mediterraneo durante il periodo del Bronzo Medio. Il quinto capitolo è dedicato allo “scopo” principe del lavoro affrontato, vale a dire la generazione dell’ortofotomosaico relativo alla zona di cui sopra. Dopo un’introduzione teorica in merito alla produzione di questo tipo di prodotto (procedure e trasformazioni utilizzabili, metodi di interpolazione dei pixel, qualità del DEM utilizzato), vengono presentati e commentati i risultati ottenuti, cercando di evidenziare le correlazioni fra gli stessi e le problematiche di diversa natura incontrate nella redazione di questo lavoro di tesi. Nel sesto ed ultimo capitolo sono contenute le conclusioni in merito al lavoro in questa sede presentato. Nell’appendice A vengono riportate le tabelle dei punti di controllo utilizzati in fase di orientamento esterno dei fotogrammi.

Each one teaches one: characterizing active forms of proteins by single molecule force spectroscopy

This Ph.D. candidate thesis collects the research work I conducted under the supervision of Prof.Bruno Samor´ı in 2005,2006 and 2007. Some parts of this work included in the Part III have been begun by myself during my undergraduate thesis in the same laboratory and then completed during the initial part of my Ph.D. thesis: the whole results have been included for the sake of understanding and completeness. During my graduate studies I worked on two very different protein systems. The theorical trait d’union between these studies, at the biological level, is the acknowledgement that protein biophysical and structural studies must, in many cases, take into account the dynamical states of protein conformational equilibria and of local physico-chemical conditions where the system studied actually performs its function. This is introducted in the introductory part in Chapter 2. Two different examples of this are presented: the structural significance deriving from the action of mechanical forces in vivo (Chapter 3) and the complexity of conformational equilibria in intrinsically unstructured proteins and amyloid formation (Chapter 4). My experimental work investigated both these examples by using in both cases the single molecule force spectroscopy technique (described in Chapter 5 and Chapter 6). The work conducted on angiostatin focused on the characterization of the relationships between the mechanochemical properties and the mechanism of action of the angiostatin protein, and most importantly their intertwining with the further layer of complexity due to disulfide redox equilibria (Part III). These studies were accompanied concurrently by the elaboration of a theorical model for a novel signalling pathway that may be relevant in the extracellular space, detailed in Chapter 7.2. The work conducted on -synuclein (Part IV) instead brought a whole new twist to the single molecule force spectroscopy methodology, applying it as a structural technique to elucidate the conformational equilibria present in intrinsically unstructured proteins. These equilibria are of utmost interest from a biophysical point of view, but most importantly because of their direct relationship with amyloid aggregation and, consequently, the aetiology of relevant pathologies like Parkinson’s disease. The work characterized, for the first time, conformational equilibria in an intrinsically unstructured protein at the single molecule level and, again for the first time, identified a monomeric folded conformation that is correlated with conditions leading to -synuclein and, ultimately, Parkinson’s disease. Also, during the research work, I found myself in the need of a generalpurpose data analysis application for single molecule force spectroscopy data analysis that could solve some common logistic and data analysis problems that are common in this technique. I developed an application that addresses some of these problems, herein presented (Part V), and that aims to be publicly released soon.

Design methodologies of microwawe integrated circuits for satellite telecommunications

The running innovation processes of the microwave transistor technologies, used in the implementation of microwave circuits, have to be supported by the study and development of proper design methodologies which, depending on the applications, will fully exploit the technology potentialities. After the choice of the technology to be used in the particular application, the circuit designer has few degrees of freedom when carrying out his design; in the most cases, due to the technological constrains, all the foundries develop and provide customized processes optimized for a specific performance such as power, low-noise, linearity, broadband etc. For these reasons circuit design is always a “compromise”, an investigation for the best solution to reach a trade off between the desired performances. This approach becomes crucial in the design of microwave systems to be used in satellite applications; the tight space constraints impose to reach the best performances under proper electrical and thermal de-rated conditions, respect to the maximum ratings provided by the used technology, in order to ensure adequate levels of reliability. In particular this work is about one of the most critical components in the front-end of a satellite antenna, the High Power Amplifier (HPA). The HPA is the main power dissipation source and so the element which mostly engrave on space, weight and cost of telecommunication apparatus; it is clear from the above reasons that design strategies addressing optimization of power density, efficiency and reliability are of major concern. Many transactions and publications demonstrate different methods for the design of power amplifiers, highlighting the availability to obtain very good levels of output power, efficiency and gain. Starting from existing knowledge, the target of the research activities summarized in this dissertation was to develop a design methodology capable optimize power amplifier performances complying all the constraints imposed by the space applications, tacking into account the thermal behaviour in the same manner of the power and the efficiency. After a reminder of the existing theories about the power amplifier design, in the first section of this work, the effectiveness of the methodology based on the accurate control of the dynamic Load Line and her shaping will be described, explaining all steps in the design of two different kinds of high power amplifiers. Considering the trade-off between the main performances and reliability issues as the target of the design activity, we will demonstrate that the expected results could be obtained working on the characteristics of the Load Line at the intrinsic terminals of the selected active device. The methodology proposed in this first part is based on the assumption that designer has the availability of an accurate electrical model of the device; the variety of publications about this argument demonstrates that it is so difficult to carry out a CAD model capable to taking into account all the non-ideal phenomena which occur when the amplifier operates at such high frequency and power levels. For that, especially for the emerging technology of Gallium Nitride (GaN), in the second section a new approach for power amplifier design will be described, basing on the experimental characterization of the intrinsic Load Line by means of a low frequency high power measurements bench. Thanks to the possibility to develop my Ph.D. in an academic spin-off, MEC – Microwave Electronics for Communications, the results of this activity has been applied to important research programs requested by space agencies, with the aim support the technological transfer from universities to industrial world and to promote a science-based entrepreneurship. For these reasons the proposed design methodology will be explained basing on many experimental results.

Extraterrestrial and terrestrial outdoor applications of Mössbauer spectroscopy

„Extraterrestrische und terrestrische Anwendungen eines miniaturisierten Mössbauer-Spektrometers“ Die vorliegende Arbeit befasst sich mit Anwendungen eines miniaturisierten Mössbauer- Spektrometers (MIMOS II), dessen Entwicklung in den frühen neunziger Jahren am Institut für Kernphysik der Technischen Universität Darmstadt unter Professor Egbert Kankeleit und seinen Mitarbeitern begann. Seit 1998 sind die Entwicklungsarbeiten im Arbeitskreis von Prof. Gütlich am Institut für Anorganische und Analytische Chemie der Johannes Gutenberg- Universität Mainz von Dr. Göstar Klingelhöfer und Mitarbeitern fortgesetzt worden. Vorrangiges Ziel war dabei der geplante Einsatz des Spektrometers zu mineralogischen Untersuchungen im Weltall. Entsprechend ist das Projekt mit erheblichen finanziellen Mitteln des Forschungsinstituts der Deutschen Luft- und Raumfahrt (DLR) in Bonn unterstützt worden. Bei den beiden Missionen, die im Jahre 2003 von der NASA zum Mars gesandt wurden und im Januar dieses Jahres die beiden „Mars Exploration Rover“ (MER) "Spirit" und "Opportunity" erfolgreich auf der Marsoberfläche abgesetzt haben, ist jeweils ein MIMOS II-Gerät zur Charakterisierung eisenhaltiger Minerale und Böden während der laufenden Mission im Einsatz. Einige Ergebnisse von MIMOS II an Gestein und Böden der Marsoberfläche werden in der vorliegenden Arbeit präsentiert und diskutiert. Diese Ergebnisse wurden vom MIMOS II-Consortium unter Führung von Dr. Göstar Klingelhöfer, mit Unterstützung des Ingenieurs- und Wissenschaftsteams von MER am Jet Propulsion Laboratory in Kalifornien, erlangt. Erste Spektren, die von Proben im Gusev-Krater (Landestelle von „Spirit“) aufgenommen wurden und in dieser Arbeit vorgestellt werden, weisen auf das Vorkommen von forsteritischem Olivin, Pyroxen, Magnetit hin; daneben zeigt sich ein von Eisen(III) herrührendes Quadrupoldublett, das (noch) nicht eindeutig zugeordnet werden konnte. Aus den gewonnenen Daten wurde geschlossen, dass physikalische Verwitterung der vorherrschende Veränderungsprozess in den Ebenen des Gusev-Kraters ist. Um die Fähigkeiten von MIMOS II in der Charakteriserung extraterrestrischen Materials vor dem Start zum Mars zu demonstrieren, wurde eine Auswahl von chondritischen, Eisenund Marsmeteoriten gemessen. Ein Datenanalysepaket, basierend auf künstlichen neuronalen Netzwerken, genetischen Algorithmen und "fuzzy" Logik, wurde erstellt, erfolgreich getestet und während der Echtzeit-Operation der MER benutzt. Eine Datenbasis von Mössbauer-Parametern und Referenzen von veröffentlichten Studien über den Temperaturbereich des Mars wurde zusammengestellt. Die Werkzeuge zur Datenanalyse eröffnen neue Einsatzmöglichkeiten des miniaturisierten Mössbauer-Spektrometers in vielen Bereichen ausserhalb des Physikllabors. Einige davon werden in dieser Arbeit vorgestellt, wie z.B.die Pigmentcharakterisierung, die Echtheit archäologischer Artefakte oder in-situ Luftverschmutzungsmessungen. Datum: 20.07.2004 1. Betreuer: Professor Dr. P. Gütlich Paulo A. de Souza Jr. GAFEP/GETEP Departamento de Pelotização - DIPE Companhia Vale do Rio Doce - CVRD Tel.: (27) 3333-4609 - Carrier (835)

Background minimization issues for next generation hard X-ray focusing telescopes

The hard X-ray band (10 - 100 keV) has been only observed so far by collimated and coded aperture mask instruments, with a sensitivity and an angular resolution lower than two orders of magnitude as respects the current X-ray focusing telescopes operating below 10 - 15 keV. The technological advance in X-ray mirrors and detection systems is now able to extend the X-ray focusing technique to the hard X-ray domain, filling the gap in terms of observational performances and providing a totally new deep view on some of the most energetic phenomena of the Universe. In order to reach a sensitivity of 1 muCrab in the 10 - 40 keV energy range, a great care in the background minimization is required, a common issue for all the hard X-ray focusing telescopes. In the present PhD thesis, a comprehensive analysis of the space radiation environment, the payload design and the resulting prompt X-ray background level is presented, with the aim of driving the feasibility study of the shielding system and assessing the scientific requirements of the future hard X-ray missions. A Geant4 based multi-mission background simulator, BoGEMMS, is developed to be applied to any high energy mission for which the shielding and instruments performances are required. It allows to interactively create a virtual model of the telescope and expose it to the space radiation environment, tracking the particles along their path and filtering the simulated background counts as a real observation in space. Its flexibility is exploited to evaluate the background spectra of the Simbol-X and NHXM mission, as well as the soft proton scattering by the X-ray optics and the selection of the best shielding configuration. Altough the Simbol-X and NHXM missions are the case studies of the background analysis, the obtained results can be generalized to any future hard X-ray telescope. For this reason, a simplified, ideal payload model is also used to select the major sources of background in LEO. All the results are original contributions to the assessment studies of the cited missions, as part of the background groups activities.