Supermassive black holes, black holes with masses <106 Msun, are found at the centers of all massive galaxies. These massive black holes grew from smaller seed black holes through accretion events. Accreting black holes are very bright in the radio through very hard X-ray spectral regimes. Due to the location of these accreting black holes at the centers of galaxies, they are referred to as active galactic nuclei (AGN). It is understood that AGN are an important phase of galaxy evolution; however, the role of AGN in massive galaxy formation is very poorly constrained. Here, the unique tool of multi-wavelength population synthesis modeling is used to study the average properties of AGN and their host galaxies with a focus on host galaxy star formation and the role of black hole growth in galaxy evolution. Knowledge of the AGN population from deep X-ray surveys is combined with theoretical AGN spectral energy distributions to predict various observables of the AGN population in wavelength regions from the far infrared to very hard X-rays. Comparison of the model predictions to observations constrains the model input parameters and allows for the determination of average properties of the AGN population. Particular attention is paid to a special class of AGN known as Compton thick AGN. These AGN are deeply embedded in gas and dust such that the column density obscuring the line of sight to the central engine of the AGN exceeds 1/σT ~ 10²⁴ cm⁻², where σT is the Thomson cross-section of the electron---a column density comparable to that of the human chest. Theoretical and simulational evidence suggest that these Compton thick AGN may be recently triggered, rapidly accreting AGN, making them of special interest to researchers. I found that Compton thick AGN are likely to contribute ~20% of the peak of the cosmic X-ray background (XRB) at ~30 keV and demonstrated that a significant portion of Compton thick AGN may be accreting very rapidly. Moreover, Compton thick AGN do not appear to follow the orientation based unified model of AGN. According to the unified model, AGN exhibit a range of obscuration levels due to a dusty 'torus' which, depending on the orientation of the torus to the observer's line of sight, may obscure the central engine of the AGN. Upon further investigation into the stellar populations of AGN host galaxies, it appears that the unified model holds in general at z < 1, but not at z > 1. I found that this is likely due to the dominant triggering mechanism of AGN switching from major mergers at z > 1.5 to secular processes by z ~ 1.

A disponibilização de fontes ópticas multi-comprimento de onda de baixo custo certamente é um dos aspectos fundamentais para viabilizar a implantação de redes WDMPON (Wavelength Division Multiplexing-Passive Optical Network). Na literatura, são encontradas propostas de algumas tecnologias para a construção de tais dispositivos como a utilização de fontes ópticas sintonizáveis, uso de um vetor de lasers DFB (Distributed Feedback Laser) ou, até mesmo, o fatiamento espectral de uma fonte de banda larga. Contudo, essas propostas apresentam custo elevado, ou limitações de operação, tornando-se inapropriadas para a aplicação de interesse. Uma alternativa que vem sendo amplamente utilizada é o travamento óptico de diodos laser de Fabry-Pérot (FP-LD - Fabry-Pérot laser diode), realizado por meio da injeção de sinal óptico externo provindo do fatiamento espectral de uma fonte de banda larga. O travamento óptico possibilita o controle espectral do FP-LD, e o seu baixo custo torna essa fonte óptica atrativa na implantação de redes WDM. O entendimento do mecanismo de travamento torna-se, então, crucial na descrição da dinâmica de tais fontes ópticas. Desta forma, nesta dissertação, foi desenvolvido o estudo dos modelos matemáticos que descrevem a dinâmica de lasers travados, assim como foi investigado o desempenho de redes WDM-PON empregando estas fontes ópticas. / The availability of low cost multi-wavelength optical sources is certainly one of the fundamental aspects to allow the deployment of WDM-PON networks. Several technologies for the implementation of such optical sources are discussed in the literature, including tunable lasers, DFB arrays and spectral slicing of a broadband light source. However, those propositions suffer from high cost or operational limitations. One alternative is the optical injection locking of a Fabry Pérot laser diode (FPLD), in which the external optical injection signal is obtained from the spectral slicing of a broadband light source. This option has been widely investigated because the optical injection locking process allows for the FP-LD optical spectral control and wavelength selection. In addition, the low cost of such device makes this optical source an attractive solution for WDM-PON widespread deployment. In this context, the understanding of the locking mechanism becomes important in the optimization of such optical sources. Thus, in this dissertation, we conducted a study of mathematical models that describe the dynamics of locked lasers as well as investigated the performance of WDM-PON based on those optical sources.

Das IceCube Neutrino Teleskop hat einen diffusen Fluss hochenergetischen astrophysikalischen Neutrinos entdeckten. Allerdings sind die Quellen die für die Mehrzahl der nachgewiesenen Neutrinos verantwortlich sind, noch unbekannt. Diese Arbeit untersucht die Möglichkeit, dass der beobachtete Neutrino-Fluss im Zentrum von aktiven galaktischen Kernen (AGN) erzeugt wird. Eine Stacking-Analyse wird durchgeführt, um die Korrelation zwischen verschiedenen Subpopulationen von AGN und hochenergetischen Neutrinos unter Verwendung von IceCube-Daten aus acht Jahren zu testen. AGN werden anhand ihrer Radioemission, Infrarot-Farbeigenschaften und ihres Röntgenflusses. Die Leuchtkraft der Akkretionsscheibe wird verwendet, um den Beitrag ausgewählter Galaxien zum Neutrinosignal zu gewichten. Die leuchtende AGN-Population trägt zu ~52% des von IceCube gemessenen diffusen Flusses bei 100 TeV mit einem Best-Fit-Spektralindex von 2 bei mit 2.83 sigma post-trial Signifikanz. Für die AGN-Probe mit geringer Leuchtkraft wird eine Signifikanz nach dem Versuch von nur 0.66 sigma gefunden, daher werden Obergrenzen festgelegt. Unter Annahme des Spektralindex für den astrophysikalischen Fluss von 2 und einer gleichverteilten gleiche Zusammensetzung Neutrinoflavour-Zusammensetzung auf der Erde, wird eine obere Flussgrenze berechnet, die den maximalen Beitrag der Kerne von AGN mit geringer Leuchtkraft zum diffusen TeV-PeV-Neutrino-Fluss auf ~51% bei 100 TeV beschränkt. Für diese Arbeit wurde auch eine neue Rekonstruktionsmethode entwickelt. In IceCube werden hochenergetische Myon-neutrinos durch die sekundären Myonen identifiziert, die durch Wechselwirkungen über geladene Ströme mit dem Eis erzeugt werden. In dem hier vorgestellten Rekonstruktionsschema wird die erwartete Ankunftszeitverteilung durch ein vorbestimmtes stochastisches Myon-Energieverlustprofil parametrisiert. Diese realistischere Parametrisierung führt zu einer Verbesserung der Myon-Winkelauflösung in IceCube um etwa 20%. / The IceCube neutrino telescope has measured a diffuse flux of high-energy astrophysical neutrinos. However, the sources responsible for the emission of the majority of the detected neutrinos are still unknown. The goal of this thesis is to explore the possibility that the neutrino flux observed by IceCube is produced in the cores of Active Galactic Nuclei (AGN). A stacking analysis is conducted to test for a correlation between various sub-populations of AGN and high-energy neutrinos using eight years of IceCube data. AGN are selected based on their radio emission, infrared color properties, and X-ray flux using the NVSS, AllWISE, ROSAT and XMMSL2 catalogs. The accretion disk luminosity estimated by the observed soft X-ray flux is used as a proxy for the contribution of selected galaxies to the neutrino signal. Two of the three AGN samples tested in this analysis show over-fluctuations, with the highest significance being of 2.83 sigma after trial correction. The luminous AGN population is found to contribute to ~52% of the diffuse flux measured by IceCube at 100 TeV with a best-fit spectral index of 2. For the low-luminosity AGN sample a post-trial significance of only 0.66 sigma is found, therefore upper limits are set. Assuming the spectral index for the astrophysical flux to be 2 and an equal composition of neutrino flavours arriving at Earth, an upper flux limit is calculated which constrains the maximal contribution of the cores of low-luminosity AGN to the diffuse TeV-PeV neutrino flux to be ~51% at 100 TeV. A new reconstruction method has also been developed for this thesis. In IceCube high-energy muon neutrinos are identified through the secondary muons produced via charge current interactions with the ice. In the reconstruction scheme presented in this thesis, the expected arrival time distribution is parameterized by a predetermined stochastic muon energy loss pattern, leading to an improvement of about 20% to the muon angular resolution of IceCube.

In this dissertation we aim to perform a multi-wavelength analysis of galaxy clusters. We discuss various methods for clustering in order to determine physical parameters of galaxy clusters required for this type of study. A selection of galaxy clusters was chosen from 4 papers, (Popesso et al. 2007b, Yoon et al. 2008, Loubser et al. 2008, Brownstein & Mo at 2006) and restricted by redshift and galactic latitude to reveal a sample of 40 galaxy clusters with 0.0 < z < 0.15. Data mining using Virtual Observatory (VO) and a literature survey provided some background information about each of the galaxy clusters in our sample with respect to optical, radio and X-ray data. Using the Kayes Mixture Model (KMM) and the Gaussian Mixing Model (GMM), we determine the most likely cluster member candidates for each source in our sample. We compare the results obtained to SIMBADs method of hierarchy. We show that the GMM provides a very robust method to determine member candidates but in order to ensure that the right candidates are chosen we apply a select choice of outlier tests to our sources. We determine a method based on a combination of GMM, the QQ Plot and the Rosner test that provides a robust and consistent method for determining galaxy cluster members. Comparison between calculated physical parameters; velocity dispersion, radius, mass and temperature, and values obtained from literature show that for the majority of our galaxy clusters agree within 3 range. Inconsistencies are thought to be due to dynamically active clusters that have substructure or are undergoing mergers, making galaxy member identi cation di cult. Six correlations between di erent physical parameters in the optical and X-ray wavelength were consistent with published results. Comparing the velocity dispersion with the X-ray temperature, we found a relation of T0:43 as compared to T0:5 obtained from Bird et al. (1995). X-ray luminosity temperature and X-ray luminosity velocity dispersion relations gave the results LX T2:44 and LX 2:40 which lie within the uncertainty of results given by Rozgacheva & Kuvshinova (2010). These results all suggest that our method for determining galaxy cluster members is e cient and application to higher redshift sources can be considered. Further studies on galaxy clusters with substructure must be performed in order to improve this method. In future work, the physical parameters obtained here will be further compared to X-ray and radio properties in order to determine a link between bent radio sources and the galaxy cluster environment. / MSc (Space Physics), North-West University, Potchefstroom Campus, 2013

In this dissertation we aim to perform a multi-wavelength analysis of galaxy clusters. We discuss various methods for clustering in order to determine physical parameters of galaxy clusters required for this type of study. A selection of galaxy clusters was chosen from 4 papers, (Popesso et al. 2007b, Yoon et al. 2008, Loubser et al. 2008, Brownstein & Mo at 2006) and restricted by redshift and galactic latitude to reveal a sample of 40 galaxy clusters with 0.0 < z < 0.15. Data mining using Virtual Observatory (VO) and a literature survey provided some background information about each of the galaxy clusters in our sample with respect to optical, radio and X-ray data. Using the Kayes Mixture Model (KMM) and the Gaussian Mixing Model (GMM), we determine the most likely cluster member candidates for each source in our sample. We compare the results obtained to SIMBADs method of hierarchy. We show that the GMM provides a very robust method to determine member candidates but in order to ensure that the right candidates are chosen we apply a select choice of outlier tests to our sources. We determine a method based on a combination of GMM, the QQ Plot and the Rosner test that provides a robust and consistent method for determining galaxy cluster members. Comparison between calculated physical parameters; velocity dispersion, radius, mass and temperature, and values obtained from literature show that for the majority of our galaxy clusters agree within 3 range. Inconsistencies are thought to be due to dynamically active clusters that have substructure or are undergoing mergers, making galaxy member identi cation di cult. Six correlations between di erent physical parameters in the optical and X-ray wavelength were consistent with published results. Comparing the velocity dispersion with the X-ray temperature, we found a relation of T0:43 as compared to T0:5 obtained from Bird et al. (1995). X-ray luminosity temperature and X-ray luminosity velocity dispersion relations gave the results LX T2:44 and LX 2:40 which lie within the uncertainty of results given by Rozgacheva & Kuvshinova (2010). These results all suggest that our method for determining galaxy cluster members is e cient and application to higher redshift sources can be considered. Further studies on galaxy clusters with substructure must be performed in order to improve this method. In future work, the physical parameters obtained here will be further compared to X-ray and radio properties in order to determine a link between bent radio sources and the galaxy cluster environment. / MSc (Space Physics), North-West University, Potchefstroom Campus, 2013

HESS J1741−302 ist eine nicht identifizierte Quelle sehr hochenergetischer Gammastrahlen, welche circa 1,7 Grad vom Zentrum der Milchstraße entfernt liegt. Diese Quelle ist eines der schwächsten Objekte im TeV-Bereich mit einem Photonfluss von Φ(>1 TeV) = (1.65 ± 0.28stat ± 0.33sys) × 10^−13 cm^−2 s^−1, was ~1% des Krebsnebelflusses im gleichen Energiebereich entspricht. Die Analyse des aktuellen H.E.S.S. Datensatzes von 145 Stunden Beobachtungen mit hoher Qualität gibt Einblicke in die Morphologie von HESS J1741−302. Das Energiespektrum von HESS J1741−302 geht über 10 TeV hinaus, ohne dabei ein klares Anzeichen für einen spektralen Abbruch zu zeigen. Das Spektrum kann durch ein Potenzgesetz mit einem spektralen Index von Γ = 2.28 ± 0.16stat ± 0.20sys und einer Normierung bei 1 TeV von Φ0 = (2.12 ± 0.42stat ± 0.42sys) × 10^−13 cm^−2 s^−1 TeV^−1 beschrieben werden. In der vorliegenden Arbeit werden verschiedene Szenarien für die beobachtete Gammastrahlung und deren Entstehung in Betracht gezogen. Diese beinhalten die Wechselwirkung von Protonen der kosmischen Strahlung mit Molekülwolken entlang der Sichtlinie, IC Streuung an Infrarot-Photonen eines nahe gelegenen OH/IR Sterns und die Präsenz eines Pulsarwindnebels, welcher möglicherweise zu PSR B1737−30 gehört. / HESS J1741−302 is an unidentified very-high-energy (VHE) γ-ray source located in the Galactic Plane at about 1.7° away from the Galactic Center. It is one of the faintest TeV objects detected so far, with a flux Φ(>1 TeV) = (1.65 ± 0.28stat ± 0.33sys) × 10^−13 cm^−2 s^−1 corresponding to ~ 1% of the Crab Nebula flux at the same energies. The data analysis of an updated high-quality dataset of ~145 hours of VHE H.E.S.S. data taken between 2004 and 2013 has revealed the morphology of HESS J1741−302. The γ-ray spectrum of HESS J1741−302 extends beyond 10 TeV without showing any clear evidence of a cut-off. The source spectrum is well described by a power-law model with a spectral index of Γ = 2.28 ± 0.16stat ± 0.20sys and a normalization at 1 TeV of Φ0 = (2.12 ± 0.42stat ± 0.42sys) × 10^−13 cm^−2 s^−1 TeV^−1. Different scenarios will be considered in this thesis, including the interaction of cosmic-ray protons with molecular clouds found along the line of sight, inverse Compton scattering of infra-red photons provided by a nearby OH/IR star and the presence of a nearby pulsar wind nebula possibly related to PSR B1737−30, in order to explain the observed VHE gamma-ray emission.

Cette thèse s'intéresse aux mécanismes initiateurs de l'endommagement laser du KDP et du DKDP en régime nanoseconde. C'est un matériau non linéaire utilisé notamment dans les cristaux de conversion de fréquence du Laser MégaJoule, en cours de construction sur le centre du CEA-Cesta, en France. La tenue au flux de ces cristaux est une des clés de la réussite de cette installation et demeure actuellement une problématique à résoudre. C'est pourquoi, cette thèse propose différentes études permettant de répondre en partie à deux volets essentiels de l'endommagement laser du KDP en régime nanoseconde : les défauts précurseurs et les mécanismes initiateurs de l'endommagement. Tout d'abord, nous proposons une étude en longueur d'onde des dommages créés suite à un tir laser. Cette étude est basée à la fois sur l'observation de clichés de dommages obtenus en microscopie DIC ainsi que sur la comparaison à un code de calcul couplant dépôt d'énergie et hydrodynamique. Par la suite, nous étudions l'influence de la géométrie des défauts précurseurs par le biais d'une étude de l'effet de la polarisation du faisceau laser sur la tenue au flux d'un cristal de KDP. A l'aide d'un code interne au CEA, cette étude permet notamment d'introduire une nouvelle géométrie des défauts, de type ellipsoïdale et respectant les propriétés de la structure cristalline d'un tel cristal. Enfin, nous abordons plus largement les mécanismes d'initiation de l'endommagement à partir d'expériences pompe--pompe. Ces tests mettent en jeu le mélange de deux longueurs d'onde différentes -- impactant l'échantillon de manière concomitante ou désynchronisée l'une par rapport à l'autre -- et son influence sur la tenue au flux du KDP. Il est notamment montré qu'il peut y avoir un couplage entre les longueurs d'onde, donc par extension entre les mécanismes, en fonction de la combinaison des fluences qui sont employées. Au final, l'intérêt de ces études est d'acquérir de nouvelles données permettant d'améliorer la compréhension des mécanismes de l'endommagement du KDP en régime nanoseconde. A terme, elles permettront également de développer des modèles de prédiction de l'endommagement des cristaux de KDP et de DKDP montés sur les chaînes laser. / This thesis interests in the laser-induced damage mechanisms of KDP and DKDP crystals in the nanosecond regime. KDP is a non-linear material particularly used in the frequency converters of the Laser MegaJoule, which is under construction at the CEA-Cesta in France. For this facility, the KDP laser damage resistance is one of the keystones and is still under investigations to fix this problem. This is why this manuscript presents different studies which highlight the two main aspects of the nanosecond laser-induced damage of KDP frequency converters : the precursor defects and the mechanims to initiate damage. First, we propose a study based on the analysis of several photos obtained by DIC microscopy of damage initiated by different wavelengths. A comparison with a code coupling the energy deposition and hydrodynamic is also done. Then, we interest in the influence of the defects geometry through a study based on the laser polarization effet on the laser damage resistance. By the comparison with a CEA home-made code, this study particularly underlines the possibility to define a new geometry for the precursor defects. This geometry proposed has the shape of an ellipsoid and is supposed to keep the crystal structure properties. Finally, we enlarge on the physical mechanisms initiating laser damage with pump--pump experiments. These tests consist in combinating two radiations of different wavelengths which imping the crystal simultaneously or are delayed one by the other. We then observe the influence of this wavelengths mixing on the KDP laser damage resistance. In particular, a coupling effet between the wavelengths of the mixture may occur as a function of the fluences combination. Finally, the goal of these specific studies is to accumulate new data in order to improve the undertanding in the intiation of the laser damage in KDP and DKDP crystals in the nanosecond regime. In the end, these data will allow us to develop predictive models to simulate the laser damage of KDP and DKDP crystals on the LMJ laser chains.

Cette thèse traite un problème inverse en astronomie. L’objectif est de reconstruire un objet 2D+λ, ayant une distribution spatiale et spectrale, à partir d’un ensemble de données multispectrales de basse résolution fournies par l’imageur MIRI (Mid-InfraRed Instrument), qui est à bord du prochain télescope spatial James Webb Space Telescope (JWST). Les données multispectrales observées souffrent d’un flou spatial qui dépend de la longueur d’onde. Cet effet est dû à la convolution par la réponse optique (PSF). De plus, les données multi-spectrales souffrent également d’une sévère dégradation spectrale en raison du filtrage spectral et de l’intégration par le détecteur sur de larges bandes. La reconstruction de l’objet original est un problème mal posé en raison du manque important d’informations spectrales dans l’ensemble de données multispectrales. La difficulté se pose alors dans le choix d’une représentation de l’objet permettant la reconstruction de l’information spectrale. Un modèle classique utilisé jusqu’à présent considère une PSF invariante spectralement par bande, ce qui néglige la variation spectrale de la PSF. Cependant, ce modèle simpliste convient que dans le cas d’instrument à une bande spectrale très étroite, ce qui n’est pas le cas pour l’imageur de MIRI. Notre approche consiste à développer une méthode pour l’inversion qui se résume en quatre étapes : (1) concevoir un modèle de l’instrument reproduisant les données multispectrales observées, (2) proposer un modèle adapté pour représenter l’objet à reconstruire, (3) exploiter conjointement l’ensemble des données multispectrales, et enfin (4) développer une méthode de reconstruction basée sur la régularisation en introduisant des priori à la solution. Les résultats de reconstruction d’objets spatio-spectral à partir de neuf images multispectrales simulées de l’imageur de MIRI montrent une augmentation significative des résolutions spatiale et spectrale de l’objet par rapport à des méthodes conventionnelles. L’objet reconstruit montre l’effet de débruitage et de déconvolution des données multispectrales. Nous avons obtenu une erreur relative n’excédant pas 5% à 30 dB et un temps d’exécution de 1 seconde pour l’algorithme de norm-l₂ et 20 secondes avec 50 itérations pour l’algorithme norm-l₂/l₁. C’est 10 fois plus rapide que la solution itérative calculée par l’algorithme de gradient conjugué. / This thesis deals with an inverse problem in astronomy. The objective is to reconstruct a spatio-spectral object, having spatial and spectral distributions, from a set of low-resolution multispectral data taken by the imager MIRI (Mid-InfraRed Instrument), which is on board the next space telescope James Webb Space Telescope (JWST). The observed multispectral data suffers from a spatial blur that varies according to the wavelength due to the spatial convolution with a shift-variant optical response (PSF). In addition the multispectral data also suffers from severe spectral degradations because of the spectral filtering and the integration by the detector over broad bands. The reconstruction of the original object is an ill-posed problem because of the severe lack of spectral information in the multispectral dataset. The difficulty then arises in choosing a representation of the object that allows the reconstruction of this spectral information. A common model used so far considers a spectral shift-invariant PSF per band, which neglects the spectral variation of the PSF. This simplistic model is only suitable for instruments with a narrow spectral band, which is not the case for the imager of MIRI. Our approach consists of developing an inverse problem framework that is summarized in four steps: (1) designing an instrument model that reproduces the observed multispectral data, (2) proposing an adapted model to represent the sought object, (3) exploiting all multispectral dataset jointly, and finally (4) developing a reconstruction method based on regularization methods by enforcing prior information to the solution. The overall reconstruction results obtained on simulated data of the JWST/MIRI imager show a significant increase of spatial and spectral resolutions of the reconstructed object compared to conventional methods. The reconstructed object shows a clear denoising and deconvolution of the multispectral data. We obtained a relative error below 5% at 30 dB, and an execution time of 1 second for the l₂-norm algorithm and 20 seconds (with 50 iterations) for the l₂/l₁-norm algorithm. This is 10 times faster than the iterative solution computed by conjugate gradients.

Aerosols affect the global radiation budget which plays an important role in determining the state of the Earth's climate. The heterogeneous distribution of aerosols and the variety in their properties results in high uncertainty in the understanding of aerosols. Aerosols affect the radiation by scattering and absorption (direct effect) or by modifying the cloud properties which in turn affects the radiation (indirect effect). The current work focuses only on the direct radiative effect of aerosols. The change in the top-of-atmosphere (TOA) reflected flux due to the perturbation of aerosols and their properties is called direct aerosol radiative forcing (ARFTOA). Estimation of ARFTOA using aerosol properties is done by solving the radiative transfer equation using a radiative transfer model. However, before using the radiative transfer model, it has to be validated with observations for consistency. This is done to check if the model is able to replicate values close to actual observations. The current work uses the Santa Barbara DISORT Atmospheric Radiative Transfer (SBDART) model. The output radiative fluxes from SBDART are validated by comparing with the Clouds and the Earth's Radiant Energy System (CERES) satellite data. Under clear-skies SBDART agreed with observed fluxes at TOA well within the error limits of satellite observations. In the shortwave solar spectrum (0.25-4 µm) radiation is affected by change in various aerosol properties and also by water vapour and other gas molecules. To study the effect of each of these molecules separately on the aerosol forcing at TOA, SBDART is used. ARFTOA is found to depend on the aerosol loading (aerosol optical depth – AOD), aerosol type (SSA) and the angular distribution of scattered radiation (asymmetry parameter). The role of water vapour relative to the aerosol layer height was also investigated and for different aerosol types and aerosol layer heights, it was found that water vapour can induce a change of ~4 Wm-2 in TOA flux. The relative importance of aerosol scattering versus absorption is evaluated through a parameter called single scattering albedo (SSA) which can be estimated from satellites. SSA defined as the ratio of scattering efficiency to total extinction efficiency, depends on the aerosol composition and wavelength. Aerosols with SSA close to 1 (sea-salt, sulphates) scatter the radiation and cool the atmosphere. Aerosols with SSA < 0.9 (black carbon, dust) absorb radiation and warm the atmosphere. Over high reflective surfaces a small change in SSA can change forcing from negative (cooling) to positive (warming). This makes SSA one of the most important and uncertain aerosol parameters. Currently, the SSA retrievals from the Ozone Monitoring Instrument (OMI) are highly sensitive to sub-pixel cloud contamination and change in aerosol height. Using the sensitivity of OMI to aerosol absorption and the superior cloud masking technique and accurate AOD retrieval of Moderate Resolution Imaging Spectroradiometer (MODIS), an algorithm to retrieve SSA (OMI-MODIS) was developed. The algorithm was performed over global oceans (60S-60N) from 2008-2012. The difference in SSA estimated by OMI-MODIS and that of OMI depended on the aerosol type and aerosol layer height. Aerosol layer height plays an important role in the UV spectrum due to the dominance of Rayleigh scattering. This was verified using SBDART which otherwise would not have been possible using just satellite observations. Both the algorithms were validated with cruise measurements over Arabian Sea and Bay of Bengal. It was seen that when absorbing aerosols (low SSA values) were present closer to the surface, OMI overestimated the value of SSA. On the other hand OMI-MODIS algorithm, which made no assumption on the aerosol type or height, was better constrained than OMI and hence was closer to the cruise measurement The presence of clouds results in a more complex interaction between aerosols and radiation. Aerosols present above clouds are responsible to most of the direct radiative effect in cloudy regions. The ARFTOA depends not only on the aerosol properties but also on the relative position of aerosols with clouds. When absorbing aerosols are present above clouds, the ARFTOA is highly influenced by the albedo of the underlying surface. Recent studies, over regions influenced by biomass burning aerosol, have shown that it is possible to define a ‘critical cloud fraction’ (CCF) at which the aerosol direct radiative forcing switch from a cooling to a warming effect. Similar analysis was done over BoB (6.5-21.5N; 82.5-97.5E) for the years 2008-2011. Aerosol properties were taken from satellite observations. Satellites cannot provide for aerosols present at different heights and hence SBDART was used to calculate the forcing due to aerosols present only above clouds. Unlike previous studies which reported a single value of CCF, over BoB it was found that CCF varied from 0.28 to 0.13 from post-monsoon to winter as a result of shift from less absorbing to moderately absorbing aerosol. This implies that in winter, the absorbing aerosols present above clouds cause warming of the atmosphere even at low cloud fractions leading to lower CCF. The use of multiple satellites in improving the retrieval of SSA has been presented in this thesis. The effect of aerosols present above clouds on the radiative forcing at TOA is shown to be different between Bay of Bengal and Atlantic Ocean. This was due to the change in SSA of aerosols during different seasons. The effect of aerosol height, aerosol type and water vapour on the TOA flux estimation is also studied using a radiative transfer model.

This work relates to the remote sensing technologies to determine wind velocity and its related phenomena. Laser-based pulsed systems with heterodyne detection allow a very sensitive measurement of particles’ velocity in the atmosphere. The heterodyne detection theory and the essential principles and properties of this technology are presented. An all-fiber coherent Doppler lidar system in master-oscillator power-amplifier design with a novel multi-wavelength channel configuration was developed and introduced, characterized, and validated in this work. The fiber amplifier is a crucial component of multi-channel all-fiber systems and is therefore discussed with special emphasis on non-linear effects and pulse distortions. A novel feedback controlled pulse-shaping unit was developed to control pulse energy and the shape of the amplified pulses of each channel. Each and every wavelength-channel creates an independent speckle pattern, which is demonstrated by hard targets with diffuse character and atmospheric single-shot measurements, and compared with theoretical results. Utilizing four channels, the precision of the measured wind velocity can be improved and this feature is demonstrated with measured atmospheric return signals. A correlation technique is presented, which enables the enhancement of the SNR at higher backscattered powers by utilizing multiple channels. The multi-wavelength system was designed to work with four wavelength-channels, which also allow measurements along the same line-of-sight with different channel configurations. These channels can be different in pulse shape, pulse length, and pulse repetition frequency. In this work, the resulting benefits of using multiple channels are shown with atmospheric measurements and scientific discussion of these is presented.:1. Introduction to the subject 2. Introduction to pulsed coherent Doppler lidar 3. Methodology: Multi-channel coherent Doppler lidar system 4. Erbium-doped fiber amplifier in a multi-channel lidar 5. Correlation properties of a multi-channel lidar system 6. Benefits of a multi-channel coherent Doppler lidar 7. Conclusions A. Wind measurement examples B. Range gate weighting function for different pulse shapes / Diese Arbeit befasst sich mit der Fernerkundungstechnologie zur Erfassung der Windgeschwindigkeit und den damit verbundenen Phänomenen. Die heterodyne Detektion der laserbasierten gepulsten Systeme ermöglicht eine sehr sensitive Messung von Partikelgeschwindigkeiten in der Atmosphäre. Sowohl die Theorie der heterodynen Detektion als auch die wesentlichen Eigenschaften und Grundsätze werden in dieser Arbeit diskutiert. Ein neuartiges faserbasiertes kohärentes Doppler Mehrkanal-Lidarsystem wurde entwickelt, vorgestellt, charakterisiert und validiert. Dabei ist der faserbasierte Verstärker eine wesentliche Komponente in diesem System und wird somit in Bezug auf Nichtlinearitäten und Impulsverzerrungen besonders analysiert. Eine neuartige geregelte Impulsformung wurde entwickelt, um die Impulsenergie und die Impulsform unabhängig für jeden Kanal zu stabilisieren. Jeder einzelne Kanal erzeugt ein unabhängiges Specklebild, welches durch Messungen am festen Ziel und durch atmosphärische Messungen präsentiert und mit theoretischen Berechnungen verglichen wird. Somit wird unter der Verwendung aller vier Kanäle des Systems die Geschwindigkeitsgenauigkeit erhöht, welches durch atmosphärische Messungen dargelegt wird. Zudem wird eine Korrelationstechnik vorgestellt, die das SNR bei höherer Rückstreuintensität weiter erhöht. Das Mehr-Wellenlängensystem wurde für vier Kanäle ausgelegt, welches eine Beobachtung der Atmosphäre entlang der Sichtlinie unter sonst gleichen Bedingungen ermöglicht. Diese Kanäle können sich sowohl in der Impulsform, in der Impulslänge als auch in der Pulsfolgefrequenz unterscheiden. Diese Arbeit zeigt die wesentlichen Vorteile eines solchen Mehrkanal-Lidarsystems mit atmosphärischen Messungen und wissenschaftlichen Ausarbeitungen.:1. Introduction to the subject 2. Introduction to pulsed coherent Doppler lidar 3. Methodology: Multi-channel coherent Doppler lidar system 4. Erbium-doped fiber amplifier in a multi-channel lidar 5. Correlation properties of a multi-channel lidar system 6. Benefits of a multi-channel coherent Doppler lidar 7. Conclusions A. Wind measurement examples B. Range gate weighting function for different pulse shapes