Il y a de plus en plus d'indications que les trous noirs super-massifs ont joué un rôle important dans l'évolution des galaxies, en particulier au moment de la formation des galaxies les plus massives à haut décalage spectral vers le rouge (z ~ 2 - 3). Nous nous sommes attachés à quantifier les effets sur le milieu interstellaire des galaxies hôtes que peuvent avoir les jets des radio-galaxies, d'une part, et les importantes luminosités bolometriques des quasars, d'autre part. Pour cela, nous avons étudié la cinématique du gaz ionisé dans 12 radio-galaxies modérément puissantes et dans 11 quasars (6 avec une détection en radio et 5 sans jet détectable) à grand décalage spectral vers le rouge avec le spectro-imageur proche infra-rouge SINFONI du VLT, qui nous donnait accès aux raies d'émission normalement sitées dans le domaine visible. Afin d'évaluer la capacité du NAG à stopper la formation d'étoiles, nous avons cherché des traces de leur rétroaction dans ces galaxies, comme de vents de gaz s'échappant de la galaxie hôte. Dans notre échantillon de radio-galaxies modérément puissantes, nous observons des dispersions de vitesse presque aussi importantes que dans les plus puissantes (avec une FWHM ~ 1000 km/s), mais les quantités de gaz ionisé observées y sont inférieures d'un ordre de grandeur (Mion gas ~ 10^8 - 10^9 Msun) et les gradients de vitesse sont plus faibles (Δv < 400 km/s), quand ils sont observés. Dans notre échantillon de quasars, nous devions d'abord soustraire la composante large des raies d'émission avant de pouvoir étudier leur composante étroite, celle susceptible d'être étendue spatialement. Nous détectons des régions d'émission véritablement étendue autour de quatre des six sources avec une détection en radio et autour d'une seule des cinq sans détection radio. Nous estimons qu'il y a moins de gaz ionisé dans ces sources que dans notre échantillon de radio-galaxies (avec Mion gas ~ 10^7 - 10^8 Msun) et la cinématique de ce gaz est aussi plus calme, similaire à ce qui est observé autour de certains quasars proches. Enfin, de nouvelles observations de deux radio-galaxies particulières nous ont révélé que l'une d'entre elles est entourée de quatorze galaxies-companions et qu'elle se trouve donc dans une partie sur-dense de l'Univers. Nous expliquons donc la morphologie inhabituelle du gaz ionisé présent autour de ces deux radio-galaxies par des cycles répétés d'activité du NAG, en analogie à ce qui est observé dans les amas de galaxies proches, qui sont d'excellents exemples de rétroaction du NAG dans l'Univers local. / There is growing evidence that supermassive black holes may play a crucial role for galaxy evolution, in particular during the formation of massive galaxies at high redshift (z ~ 2 - 3). Our work focuses on quantifying the effects of jets of radiogalaxies and of large bolometric luminosities of quasars on the interstellar gas in their host galaxies. To this end, we studied the kinematics of the ionized gas in 12 moderately powerful radio galaxies and 11 quasars (6 radio-loud and 5 radio-quiet) at high redshifts with rest-frame optical imaging spectroscopy obtained at the VLT with SINFONI. We searched for outflows and other signatures of feedback from the supermassive black holes in the centers of these galaxies to evaluate if the AGN may plausibly quench star formation. In our sample of moderately powerful radiogalaxies, we observe velocity dispersions nearly as large as those observed in the most powerful ones (with FWHM ~ 1000 km/s), but the quantity of ionized gas is decreased by one order of magnitude (Mion gas ~ 10^8 - 10^9 Msun) and velocity gradients tend to be less dramatic (Δv < 400 km/s), when they are observed. In our sample of quasars, we had to carefully subtract the broad spectral component of emission lines to have access to its narrow, and spatially extended, component. We detect truly extended emission line regions in 4/6 sources of our radio-loud subsample and in 1/5 source of our radio-quiet subsample. We estimate that masses of ionized gas in these sources are smaller than in our sample of high-redshift radiogalaxies (with Mion gas ~ 10^7 - 10^8 Msun) and kinematics tend to be more quiescent, akin to what is observed in local quasars. Finally, detailed observations of two outliers among our sample of high-redshift radiogalaxies revealed that one of them is closely surrounded by 14 companions galaxies, hence lying in an overdensity. We therefore interpret the presence and morphology of ionized gas around these galaxies as evidence for repeated cycles ouf AGN outbursts, akin to what can be observed in local clusters of galaxies, which are prime examples of AGN feedback in the nearby Universe.

Forests can be considered as one of the most important Earth's ecosystems not only because of oxygen production and carbon sequestration via photosynthesis, but also as a source of many natural resources (such as wood) and as a habitat of many specific plants and animals. Monitoring of forest health status is thus crucial activity for keeping all production and ecosystem functions of forests. The main aim of the thesis is development of an alternative approach for forest health status based on airborne hyperspectral data (HyMap) analysis supported by field sampling. The proposed approach tries to use similar vegetation parameters which are used in case of the current methods of forest health status assessment based on field inspections. It is believed that importance of such new methods will significantly increase in the time when the planned satellite hyperspectral missions (e.g. EnMap) will move into operational phase. The developed forest health monitoring approach is practically demonstrated on mature Norway spruce (Picea abies L. Karst) forests of the Sokolov lignite basin which were affected by long-term coal mining and heavy industry and therefore high variability of forest health status was assumed in this case. Two leaf level radiative transfer models were used for simulating spectral...

Manipulating light by controlling surface plasmons on metals is being discussed as a means for bridging the size gap between micrometer-sized photonic circuits and nanometer-sized integrated electronics. Plasmonic waveguides based on metal nanoparticles are of particular interest for circumventing the diffraction limit, thereby enabling high-speed communication over short-range distances in miniaturized micro-components. However, scalable, inexpensive fine-tuning of particle assemblies remains a challenge and near-field probing is required to reveal plasmonic interactions. In this thesis, self-assembled waveguides should be produced on DNA scaffolds. DNA origami is an extremely versatile and robust self-assembly method which allows scalable production of nanostructures with a fine control of assemblies at the nanoscale. To form the plasmonic waveguides, six-helix bundle DNA origami nanotubes are used as templates for attachment of highly monodisperse and monocrystalline gold nanoparticles with an inter-particle distance of 1-2 nm. In the first part of this thesis, the effects of parameters which are involved in assembly reactions are systematically investigated. The assembly yield and binding occupancy of the gold nanoparticles are determined by an automated, high-throughput image analysis of electron micrographs of the formed complexes. As a result, unprecedented binding site occupancy and assembly yield are achieved with the optimized synthesis protocol. In addition, waveguides with different sizes of gold nanoparticles and different inter-particle distances, quantum dots attachments to the waveguides and multimerization of the waveguides are successfully realized. In the second part of this thesis, direct observation of energy transport through a self-assembled waveguide towards a fluorescent nanodiamond is demonstrated. High-resolution, near-field mapping of the waveguides are studied by electron energy loss spectroscopy and cathodoluminescence imaging spectroscopy. The experimental and simulation results reveal that energy propagation through the waveguides is enabled by coupled surface plasmon modes. These surface plasmon modes are probed at high spatial and spectral resolutions. The scalable self-assembly approach presented here will enable the construction of complex, sub diffraction plasmonic devices for applications in high-speed optical data transmission, quantum information technology, and sensing. / Die Manipulation des Lichts durch die Kontrolle von Oberflächenplasmonen auf metallischen Oberflächen und Nanopartikeln gilt als vielversprechende Methode zur Überbrückung der Größen-Lücke zwischen Mikrometer-großen photonischen und nanometer-großen elektronischen Schaltkreisen. Plasmonische Wellenleiter basierend auf metallischen Nanopartikeln sind vom besonderen Interesse, da sie die Umgehung des Beugungslimits und somit eine Hochgeschwindigkeitskommunikation über kurze Distanzen in immer kleiner werdenden Schaltkreisen ermöglichen könnten. Allerdings ist die skalierbare und kostengünstige Anordnung von Partikeln eine große Herausforderung und es werden Nahfelduntersuchungen benötigt um plasmonische Interaktionen detektieren zu können. Das Ziel dieser Arbeit ist die Selbstassemblierung von multi-partikel Wellenleitern auf DNA Gerüsten. Die Verwendung von DNA-Origami bietet eine äußerst vielseitige Plattform zur skalierbaren Herstellung von Nanostrukturen mittels Selbstassemblierung und ermöglicht eine präzise Kontrolle der Anordnungen im Nanobereich. Für den Aufbau der plasmonischen Wellenleiter werden DNA-Origami Nanoröhren, bestehend aus sechs Helices als Templat für die Anbindung von monodispersen und monokristallinen Goldnanopartikeln mit einem interpartikulären Abstand von 1-2 nm verwendet. Im ersten Abschnitt dieser Arbeit werden die beeinflussenden Faktoren dieser Assemblierungsreaktion systematisch untersucht. Die Ausbeute der assemblierten Strukturen und die Besetzung der Bindungsstellen werden durch eine automatisierte und effiziente Bildanalyse von Elektronenmikroskopieaufnahmen ausgewertet. Durch die Entwicklung eines optimierten Syntheseprotokolls werden bisher unerreichte Assemblierungsausbeuten ermöglicht. Zusätzlich erfolgen die experimentelle Realisierung von Strukturen mit verschieden großen Goldnanopartikeln und unterschiedlichen interpartikulären Abständen, sowie die Anbindung von Quantenpunkten an die Wellenleiter und eine Verknüpfung der assemblierten Strukturen. Der zweite Abschnitt dieser Dissertation befasst sich mit der Untersuchung des Energietransports in selbstassemblierten Wellenleitern über einen fluoreszierenden Nanodiamanten. Dazu erfolgen hochaufgelöste Nahfeldmessungen der Wellenleiter mittels Elektronenenergieverlustspektroskopie und Kathodolumineszenz-mikroskopie. Die experimentellen Ergebnisse und zusätzlich durchgeführte Simulationen bestätigen eine durch gekoppelte Oberflächenplasmonenmoden induzierte Weitergabe der Energie innerhalb des Wellenleiters. Diese Oberflächenplasmonenmoden werden bei hoher räumlicher und spektraler Auflösung untersucht. Das hier umgesetzte Konzept der Selbstassemblierung wird den Aufbau komplexer plasmonischer Geräte für Anwendungen im Bereich der optischen Hochgeschwindigkeitsdatenübertragung, der Quanteninformations-technolgie und der Sensorik ermöglichen.

There is growing evidence that supermassive black holes may play a crucial role for galaxy evolution, in particular during the formation of massive galaxies at high redshift (z ~ 2 - 3). Our work focuses on quantifying the effects of jets of radiogalaxies and of large bolometric luminosities of quasars on the interstellar gas in their host galaxies. To this end, we studied the kinematics of the ionized gas in 12 moderately powerful radio galaxies and 11 quasars (6 radio-loud and 5 radio-quiet) at high redshifts with rest-frame optical imaging spectroscopy obtained at the VLT with SINFONI. We searched for outflows and other signatures of feedback from the supermassive black holes in the centers of these galaxies to evaluate if the AGN may plausibly quench star formation. In our sample of moderately powerful radiogalaxies, we observe velocity dispersions nearly as large as those observed in the most powerful ones (with FWHM ~ 1000 km/s), but the quantity of ionized gas is decreased by one order of magnitude (Mion gas ~ 10^8 - 10^9 Msun) and velocity gradients tend to be less dramatic (Δv < 400 km/s), when they are observed. In our sample of quasars, we had to carefully subtract the broad spectral component of emission lines to have access to its narrow, and spatially extended, component. We detect truly extended emission line regions in 4/6 sources of our radio-loud subsample and in 1/5 source of our radio-quiet subsample. We estimate that masses of ionized gas in these sources are smaller than in our sample of high-redshift radiogalaxies (with Mion gas ~ 10^7 - 10^8 Msun) and kinematics tend to be more quiescent, akin to what is observed in local quasars. Finally, detailed observations of two outliers among our sample of high-redshift radiogalaxies revealed that one of them is closely surrounded by 14 companions galaxies, hence lying in an overdensity. We therefore interpret the presence and morphology of ionized gas around these galaxies as evidence for repeated cycles ouf AGN outbursts, akin to what can be observed in local clusters of galaxies, which are prime examples of AGN feedback in the nearby Universe.