Ce travail a comme objectif principal de vérifier s’il est possible de faire de la science avec les observations d’objets étendus qui seront réalisées par la mission spatiale Gaia. Cette mission, l’un des plus ambitieux projets de l’Astronomie moderne,observera plus d’un milliard d’objets dans tout le ciel avec des précisions inédites, fournissant des données astrométriques, photométriques et spectroscopiques. Naturellement, en fonction de sa priorité astrométrique, Gaia a été optimisé pour l’étude d’objets ponctuels. Néanmoins, diverses sources associées à des émissions étendues seront observées. Ces émissions peuvent avoir une origine intrinsèque, telles que les galaxies, ou extrinsèque, telles que les projections d’objets distincts sur la même ligne de visée, et présenteront probablement de solutions astrométriques moins bonnes.Pour étudier ces émissions, leurs images bidimensionnelles doivent être analysées.Néanmoins, comme Gaia ne produit pas de telles données, nous avons commencé ce travail en vérifiant si à partir de ses observations unidimensionnelles il serait possible de reconstruire des images 2D d’objets dans tout le ciel.Nous avons ainsi estimé la quantité de cas sujets à la présence d’émissions étendues extrinsèques, et nous avons présenté une méthode que nous avons développée pour analyser leurs images reconstruites. Nous avons montré que l’utilisation de cette méthode permettra d’étendre le catalogue final de façon fiable à des millions de sources ponctuelles dont beaucoup dépasseront la magnitude limite de l’instrument.D’un autre coté, dans le cas d’émissions intrinsèques, nous avons premièrement obtenu une estimation supérieure du nombre de cas que Gaia pourra observer. Nous avons alors vérifié qu’après les reconstructions d’images, les codes que nous avons développés permettront de classifier morphologiquement des millions de galaxies dans les types précoce/tardif et elliptique/spirale/irrégulière. Nous avons de plus présenté une méthode que nous avons développée pour réaliser la décomposition bulbe/disque directement à partir des observations unidimensionnelles de Gaia de façon complètement automatique.Finalement nous avons conclu qu’il est possible d’utiliser beaucoup de ces données qui pourraient être ignorées pour faire de la science. Et que le fait de les exploiter permettra aussi bien la détection de millions d’objets qui dépassent la limite de magnitude de Gaia, que de mener des études sur la morphologie de millions de galaxies dont les structures ne peuvent être révélées qu’à partir de l’espace ou au moyen d’optique adaptative, augmentant un peu plus les horizons de cette mission déjà immense. / The main objective of this work is to determine whether it is possible to do science from the observations of extended objects that will be performed by the Gaia space mission. One of the most ambitious projects of modern Astronomy, this mission will observe more than one billion objects through out the sky, thus providing astrometric, photometric and spectroscopic data with unprecedented precision. Naturally, Gaia has been optimized for the study of point-like sources due to its astrometrical priority. Nevertheless, many sources associated with extended emission will be observed. The origins of these extended sources can be either intrinsic, such as galaxies, or extrinsic, such as projections of objects in the same line of sight. In both cases, these sources will have less than optimal astrometric solutions.In order to study those emissions, their two-dimensional images will be analyzed. Nonetheless, since Gaia will not acquire such images, we begin this work by checking whether it will be possible to reconstruct images anywhere in the sky from the satellite’s one-dimensional observations.Consequently, we, on the one hand, estimate the number of cases which will be subjected to the extrinsic extended emissions, present a method which we developed to analyze the reconstructed images by segregating the different sources and show that the adoption of this method will allow extending the catalogue reliably by millions of point sources, many of which are beyond the limiting magnitude of the instrument. On the other hand, regarding intrinsic extended emissions, we first obtain an upper limit estimate for the number of cases which Gaia will be able to observe ; then,we verify that the combination of image reconstructions and the use of the codes introduced here in will allow performing the morphological classification of millions of galaxies in early/late types and elliptical/spiral/irregular classes. Afterward,we present a method which we developed to decompose those galaxies into their bulge/disk components directly from the one-dimensional Gaia data in a completely automatic way. Finally, we conclude that it is possible to harness the data of many of the observations that might other wise be ignored to do science. Saving these data will allow the detection of millions of objects beyond Gaia’s limiting magnitude and the study of the morphology of millions of galaxies whose structures can only be probed from space or through the adoption of adaptive optics, thus somewhat expanding the horizons of this already comprehensive mission.

Le travail présenté dans cette thèse porte sur l'estimation du flot optique par méthodes variationnelles en petits et en grands déplacements. Nous proposons un modèle basé sur la combinaison locale-globale à laquelle nous ajoutons la prise en compte des variations de la luminosité. La particularité de ce manuscrit réside dans l'utilisation de la méthode des éléments finis pour la résolution des équations. En effet, cette méthode se fait pour le moment très rare dans le domaine du flot optique. Grâce à ce choix de résolution, nous proposons d'implémenter un contrôle local de la régularisation ainsi qu'une adaptation de maillage permettant d'affiner la solution au niveau des arêtes de l'image. Afin de réduire les temps de calcul, nous parallélisons les programmes. La première méthode implémentée est la méthode parallèle en temps appelée pararéel. En couplant un solveur grossier et un solveur fin, cet algorithme permet d'accélérer les calculs. Pour pouvoir obtenir un gain de temps encore plus important et également traiter les séquences en haute définition, nous utilisons ensuite une méthode de décomposition de domaine. Combinée au solveur massivement parallèle MUMPS, cette méthode permet un gain de temps de calcul significatif. Enfin, nous proposons de coupler la méthode de décomposition de domaine et le pararéel afin de profiter des avantages de chacune. Dans une seconde partie, nous appliquons tous ces modèles dans le cas de l'estimation du flot optique en grands déplacements. Nous proposons de nous servir du pararéel afin de traiter la non-linéarité de ce problème. Nous terminons par un exemple concret d'application du flot optique en restauration de films. / The work presented in this thesis focuses on the estimation of the optical flow through variational methods in small and large displacements. We propose a model based on the combined local-global strategy to which we add the consideration of brightness intensity variations. The particularity of this manuscript is the use of the finite element method to solve the equations. Indeed, for now, this method is really rare in the field of the optical flow. Thanks to this choice of resolution, we implement an adaptive control of the regularization and a mesh adaptation to refine the solution on the edges of the image. To reduce computation times, we parallelize the programs. The first method implemented is a parallel in time method called parareal. By combining a coarse and a fine solver, this algorithm speeds up the computations. To save even more time and to also be able to handle high resolution sequences, we then use a domain decomposition method. Combined with the massively parallel solver MUMPS, this method allows a significant reduction of computation times. Finally, we propose to couple the domain decomposition method and the parareal to have the benefits of both methods. In the second part, we apply all these models to the case of the optical flow estimation in large displacements. We use the parareal method to cope with the non-linearity of the problem. We end by a concrete example of application of the optical flow in film restoration.

<p>The potential of using acid hydrogen peroxide under Fenton conditions to lower the electrical energy consumed during the production of Black spruce (Picea mariana) thermomechanical pulp (TMP) was investigated. The chemical system, which consisted of ferrous sulphate, hydrogen peroxide and optionally an enhancer (3,4-dimethoxybenzyl alcohol, ethylenediaminetetraacetic acid or oxalic acid/sodium oxalate), was evaluated as an inter-stage treatment where the primary refiner was used as a mixer. The produced TMPs were thoroughly characterised in order to explain the effect of the chemical system on fibre development and to be able to propose a mechanism for the impact on refining energy reduction. The possibility to improve the optical properties by washing, chelating and sodium dithionite or hydrogen peroxide bleaching the treated pulps was evaluated.</p><p> </p><p>The results obtained in a pilot plant trial show that it is possible to significantly reduce the comparative specific energy consumption by approximately 20% and 35% at a freeness value of 100 ml CSF or a tensile index of 45 Nm/g by using 1% and 2% hydrogen peroxide respectively. The energy reduction is obtained without any substantial change in the fractional composition of the pulp, though tear strength is slightly reduced, as are brightness and pulp yield. No major differences between the reference pulp and the chemically treated pulps were found with respect to fibre length, width or cross-sectional dimensions. However, the acid hydrogen peroxide-treated pulps tend to have more collapsed fibres, higher flexibility, a larger specific surface area and a lower coarseness value. The yield loss accompanying the treatment is mainly a consequence of degraded hemicelluloses. It was also found that the total charge of the chemically treated pulps is higher compared to the reference pulps, something that may have influenced the softening behaviour of the fibre wall.</p><p> </p><p>A washing or chelating procedure can reduce the metal ion content of the chemically treated TMPs considerably. The amount of iron can be further reduced to a level similar to that of untreated pulps by performing a reducing agent-assisted chelating stage (QY) with dithionite. The discoloration cannot, however, be completely eliminated. The brightness decrease of the treated pulps is thus not only caused by higher iron content in the pulp, but is also dependent on the type of iron compound and/or other coloured compounds connected with the acid hydrogen peroxide treatment. Oxidative bleaching with hydrogen peroxide (P) is more effective than reductive bleaching with sodium dithionite in regaining the brightness lost during the energy reductive treatment. Using a QY P sequence, a hydrogen peroxide charge of 3.8% was needed to reach an ISO brightness of 75% for the chemically treated pulps. The corresponding hydrogen peroxide charge for the untreated TMP reference was 2.5%.</p><p> </p><p>The radicals generated in the Fenton reaction will probably attack and weaken/soften the available outer fibre wall layers. This could facilitate fibre development and consequently lower the electrical energy demand for a certain degree of refinement.</p>

The potential of using acid hydrogen peroxide under Fenton conditions to lower the electrical energy consumed during the production of Black spruce (Picea mariana) thermomechanical pulp (TMP) was investigated. The chemical system, which consisted of ferrous sulphate, hydrogen peroxide and optionally an enhancer (3,4-dimethoxybenzyl alcohol, ethylenediaminetetraacetic acid or oxalic acid/sodium oxalate), was evaluated as an inter-stage treatment where the primary refiner was used as a mixer. The produced TMPs were thoroughly characterised in order to explain the effect of the chemical system on fibre development and to be able to propose a mechanism for the impact on refining energy reduction. The possibility to improve the optical properties by washing, chelating and sodium dithionite or hydrogen peroxide bleaching the treated pulps was evaluated.   The results obtained in a pilot plant trial show that it is possible to significantly reduce the comparative specific energy consumption by approximately 20% and 35% at a freeness value of 100 ml CSF or a tensile index of 45 Nm/g by using 1% and 2% hydrogen peroxide respectively. The energy reduction is obtained without any substantial change in the fractional composition of the pulp, though tear strength is slightly reduced, as are brightness and pulp yield. No major differences between the reference pulp and the chemically treated pulps were found with respect to fibre length, width or cross-sectional dimensions. However, the acid hydrogen peroxide-treated pulps tend to have more collapsed fibres, higher flexibility, a larger specific surface area and a lower coarseness value. The yield loss accompanying the treatment is mainly a consequence of degraded hemicelluloses. It was also found that the total charge of the chemically treated pulps is higher compared to the reference pulps, something that may have influenced the softening behaviour of the fibre wall.   A washing or chelating procedure can reduce the metal ion content of the chemically treated TMPs considerably. The amount of iron can be further reduced to a level similar to that of untreated pulps by performing a reducing agent-assisted chelating stage (QY) with dithionite. The discoloration cannot, however, be completely eliminated. The brightness decrease of the treated pulps is thus not only caused by higher iron content in the pulp, but is also dependent on the type of iron compound and/or other coloured compounds connected with the acid hydrogen peroxide treatment. Oxidative bleaching with hydrogen peroxide (P) is more effective than reductive bleaching with sodium dithionite in regaining the brightness lost during the energy reductive treatment. Using a QY P sequence, a hydrogen peroxide charge of 3.8% was needed to reach an ISO brightness of 75% for the chemically treated pulps. The corresponding hydrogen peroxide charge for the untreated TMP reference was 2.5%.   The radicals generated in the Fenton reaction will probably attack and weaken/soften the available outer fibre wall layers. This could facilitate fibre development and consequently lower the electrical energy demand for a certain degree of refinement.

This thesis presents studies of cosmic populations of extragalactic radio sources. The problems selected for this thesis are 1) the derivation of constraints on the emergence of new sub-mJy populations at flux density below about 1mJy (at1.4 GHz) paying careful attention to including sources with low surface brightness and counting sources rather than components 2) development of a new method to estimate the asymmetry in the large scale galaxy environment with respect to the axes of extended radio sources and use this to examine for evidence of impact of the environment on the morphology of radio sources. The studies presented herein have been carried out using the Australia Telescope Low Brightness Survey (ATLBS), which is a sensitive radio survey at 1.4 GHz, imaging 8.42 square degrees of the sky along with accompanying optical observations of the same region. There are multiple populations of extragalactic radio sources in the cosmos. These consist of populations of powerful radio-loud quasars and radio galaxies to populations of weaker radio sources such as star-forming galaxies. These populations of radio sources show evidence of evolution with cosmic epoch. Because the radio galaxy phenomenon and the AGNs at the centers of their host galaxies may influence the evolution of the galaxy via feedbacks, examinations of these source populations over cosmic time are a necessary complementary study to understanding the process of galaxy formation and in general, cosmology. Below we give brief introduction to the problems studied in this thesis. Sub-mJy Radio Source Counts Radio source counts, which have historically been a key probe of cosmology, now represent a measure of cosmological evolution in radio source populations. Currently, the estimation of source counts at sub-mJy flux density as well as the nature and evolution of these sources is undetermined. At flux densities ≤1.0 mJy a ‘flattening’ of normalized differential source counts has been widely reported in literature( Windhorst et al.(1985),Hopkins et al.(2003),Huynh et al.(2005) and references therein). The flattening is observed as an apparent change of slope for the normalized differential source counts from ∼0.7 at5.0 −100.0 mJy to about 0.4 in the 0.25 −5.0 mJy range. Attempts to understand the nature of the sub-mJy population have arrived at discordant results and identify the sub-mJy sources with different populations: starburst galaxies(Condon(1989), Benn et al. (1993), Huynhet al. (2005)), early type galaxies (Gruppioniet al., 1999),low(radio) luminosity activegalactic nuclei(AGNs)(Huynh et al.,2008) or a mixture of these. Due to unavailability of spectroscopically complete samples of hosts of sub-mJy sources, the exact nature of the sub-mJy radio source population is currently uncertain. However, the presence of a population which emerges at sub-mJy flux density and is different from the AGN-dominated radio source population is not in doubt. The studies in the literature are inconsistent in identifying the precise location of the emergence of flattening in counts at sub-mJy flux density. Several studies show that the source counts are consistent with a continuation in the slope of the differential counts below mJy flux density (Prandoniet al.(2001) and Subrahmanyan et al.(2010)). The scatter in the sub-mJy counts from different studies may be because of the relatively small areas covered by deep surveys(in many cases, a single pointing of an interferometric array) which may have relatively large errors arising from large scale clustering in the spatial distribution of cosmic radio sources(however the study by Condon (2007) concludes that the scatter in the source counts stems from variations in corrections and sensitivity in different studies)In contrast, wide-field surveys may not reach the depth to probe sub-mJy counts. Another reason is the correction applicable to the observed source counts necessary to estimate the true source counts; these are especially pertinent at low flux densities. To resolve these is-sues, a survey which combines the attributes of wide spatial coverage as well as excellent sensitivity and a procedure which accounts for the biases in estimation of the sub-mJy source counts is needed. In conclusion, accurate measurements of the source counts at sub-mJy flux densities are needed to correctly estimate the cosmic evolution of radio sources. Environments of Extended Radio Sources Another issue of importance in the study of extragalactic radio sources is their interaction with their environments. The gas environments in which radio sources reside and evolve ought to have an influence on the morphology of the radio sources. This has been shown in many case studies where the radio structures have been compared with the X-ray gas environments (Blanton et al. (2011); Boehringer et al.(1993)). Studies of the optical environments of radio galaxies have also been carried out previously (Longair & Seldner, 1979; Yee & Green, 1984; Hill & Lilly, 1991; Zirbel, 1997). The motivation behind these studies has been to examine differences between different classes of radio sources, the evolution of environments with cosmic epoch as well as the possibility of identifying clusters/groups of galaxies using radio sources as a tracer(Wing &Blanton, 2011). Many previous studies have found that the environments of FRI/FRII sources are different and are dependent on the cosmic epoch. FRI sources, typically, are found in rich environments. FRII sources in the local universe are generally hosted by field galaxies, but at higher red shifts are found in richer environments(Hatch et al.,2011;Best et al.,2003;Overzier et al.,2008). However, there have been fewer studies that relate the richness of the environments and morphological asymmetries of radio galaxies. Earlier investigations by Subrahmanyan et al. (2008) and Safouris et al.(2009) are noteworthy in this regard where the radio structures of two giant radio galaxies were examined in the context of the large-scale galaxy distributions in their vicinity(also see Chen et al.(2012) and references therein). The study was also used to infer properties of the ambient thermal gas medium in which the structures evolved. Clear correlations between structural asymmetries and associated extended emission-line gas were also found for radio galaxies that have relatively smaller sizes of a few hundred kpc(McCarthy et al., 1991). Thesis Work To progress the field in the problems highlighted above, the following work has been done in this thesis. Radio Imaging of ATLBS Survey To characterize the cosmic evolution of radio sources and their properties, observations and imaging of faint radio sources is essential. The Australia Telescope Low Brightness Survey(ATLBS), which has been used in the studies presented in this thesis, has been designed specifically to image diffuse radio emission to relatively high red shifts(z ∼1−1.5). Therefore obtaining good surface brightness sensitivity was a prime objective in planning the radio observations and in imaging the data obtained from these observations. This requires a nearly complete synthesized aperture and observations of a representative patch of the extra galactic sky. These requirements have been fulfilled in ATLBS survey, which has excellent uv coverage, especially at short spacings, and images a region off the galactic plane that is devoid of strong radio sources. The observations were carried out for two adjacent fields, designated as A and B with their centers at RA:00h 35m 00s,DEC:−67◦00 00 and RA:00h 59m 17s,DEC:−67◦00 00 ,in the 20 cm band, with a center frequency of1388MHz,infullpolarization mode. The radio data was imaged by using techniques such as multi-frequency deconvolution and self-calibration to make two mosaics of region A and B which are free of artefacts. These high-resolution radio images(with beamFWHM of 6 “)of the ATLBS survey regions cover 8.42 square degrees sky area with rms noise 72 µJy beam−1 and are of exceptional quality in that there are no imaging errors or artifacts above the thermal noise over the entire field of view. The images have excellent surface brightness sensitivity and hence provide good representation of extended emission components associated with radio sources. Optical Imaging of ATLBS Survey The ATLBS survey region has been also observed in SDSS r band, specifically for providing information about the galaxies hosting radio sources observed in ATLBS survey as well as galaxies in the neighbourhood of the radio sources. The optical observations were carried out using the CTIO 4 meter Blanco Telescope in Chile and using theMOSAICIIimager,whichisamosaicof8CCDs. In total, 28 optical images were created from the optical data. Each image was formed from a set of 5 dithers, using which spurious sources in the images were rejected. The final images are complete down to a magnitude of 22.75. Radio Source Counts Using the sensitive radio and optical images, a study of radio source counts was carried out. This study made use of some novel strategies and algorithms to generate a source list and correct it for various biases to obtain the radio source counts. More specifically, care was taken to identify sources with low surface brightness by making use of low resolution images for initial identification, and using multiple indicators (including optical images) to identify components of sources. The blending issues inherent in using low resolution images has been avoided using higher resolution images to identify blended sources. Thus, use of low resolution images( beam FWHM =50”′) almost completely removes effects of resolution bias and the use of high resolution images avoids blending issues. These strategies, together with use of optical images to locate candidate galaxy hosts and a careful visual examination of resolved and complex sources instead of automated classification ensures that the ATLBS catalog is a ‘source catalog’ as opposed to a ‘component catalog’. The distinction between ‘sources’ (which are single sources) as opposed to components(parts of a single source appearing separate) is crucial in estimating the true source counts. The source list was used toestimatetheradiosourcecountsdownto0.4 mJy. Comparing the counts with previous work shows that the ATLBS counts are systematically lower and the upturn in sub-mJy source counts has not been found down to the noise limited flux densities probed. The systematically low counts for ATLBS relative to most previous studies are attributed to the ATLBS counts representing sources as opposed to components, as well as corrections for noise bias as well as clustering effects that may affect source counts derived from the small sky coverage typical of deep surveys. This study also demonstrates the substantial difference in counts that result from using component catalogs as opposed to source catalogs: at 1 mJy flux density component counts may be as much as 50% above true source counts. This implies that automated image analysis for counts may be dependent on the ability of the imaging to reproduce connecting emission with low surface brightness as well as the ability of the algorithm to recognize sources, which require that source finding algorithms effectively work with multi-resolution and multi-wavelength data. Galaxy Environments of Extended Radio Sources in ATLBS Survey A study of the galaxy environments of the extended sources in the ATLBS survey was carried out using the optical images. This study of the environments of radio sources from the ATLBS survey is restricted to those that are extended and hence to a subset of the ATLBS-ESS(Extended Source Sample) sources. Briefly, the ATLBS-ESS subsample consists of 119 radio sources that have angular size ex-ceeding0’.5. Applying a red shift cut(to exclude sources with high red shifts whose optical environment may be beyond the depth of the optical images) as well as other constraints(such as availability of optical magnitudes of the host galaxy), a sub-sample of 43 sources was formed, including sources of diverse radio morphologies(FRI/FRII, WATs and HTs)as well as7 radio sources which are highly asymmetric in their radio morphology. For these sources, where no spectroscopic data was available, a red shift estimate was obtained from a magnitude-red shift relation derived from other sources in the ATLBS survey. Using the optical images convolved with a matched filter(following the prescription from Postman et al. (1996))consisting of a radial and magnitude filter, smoothed maps were formed for each source in the sample. These give the likelihood of a cluster being present in a given position in the map (in this case the location of interest being the position of the radio source in the map). Further, five parameters were defined in this study, which give estimates of the angular anisotropy of galaxy density around the axis of the radio source. This method used to quantify environmental asymmetry for the study presented in the thesis is new. The parameters defined thus were used to examine the environments of radio sources in the sample over a wide range in red shift. Specifically a comparison of FRI/FRII environments was made in two different red shift regimes(above and below z = 0.5) and it was found that the FRI and FRII sources inhabit environments of similar richness at low and high red shifts, with no evidence for red shift evolution. The WAT and HT sources were(as expected from earlier studies in literature)found in the most dense environments. Examination of the anisotropy parameters for the asymmetric radio sources clearly showed the influence environment has on radio source morphology, specifically in that the higher density of galaxies was found on the shorter side of the radio sources in almost all cases. Images and Other Resources The radio and optical images are an excellent resource for examining with auto-mated algorithms for source finding, parameter fitting, and morphological classification, and as a resource for testing such algorithms that would be used on upcoming all-sky continuum surveys with the LOFAR and ASKAP/SKA. The techniques and methods developed and presented in the thesis may be used in future studies of radio source populations.

Dizertační práce se zabývá problematikou výpočtu vlivu coulombovských interakcí částic na parametry emitovaného elektronového svazku v blízkosti Schottkyho a studené katody. Práce poskytuje základní předhled o problematice, popisuje vytvořené modely emisních zdrojů a metodu simulace Monte Carlo. Představuje novou metodu generování vstupních dat, která klade větší důraz na přesnou simulaci emisního procesu. Pozornost je zde věnována zejména vlivu interakcí na energiovou šířku, velikost virtuálního zdroje a jas katody v závislosti na velikosti poloměru hrotu a emisním proudu. Sledováním vývoje energiové šířky bylo zjištěno, že naprostá většina interakcí se odehrává v prostoru do několika mikrometrů od hrotu katody. Závislost spočtené celkové energiové šířky na úhlové intenzitě je ve shodě s dostupnými experimentálními daty. Spočtené energiové rozšíření vlivem coulombovských interakcí bylo srovnáno s hodnotami vypočtenými pomocí vzorců založených na analytických přiblíženích. Bylo zjištěno, že některé z nich přijatelně předpovídají trendy ale nemohou být použity pro kvantitativní odhad.

Ce travail de thèse est consacré au développement de sources lasers femtosecondes à haute cadence, de forte puissancemoyenne (>10 W) avec des énergies supérieures à 100 μJ. Ce type de sources est primordial pour le développementd’applications industrielles variées (micro-usinage athermique, chirurgie oculaire, …) ainsi qu’en recherchefondamentale pour l’étude de l’interaction laser matière.Après un chapitre d’introduction sur l’état de l’art des chaînes lasers de forte puissance moyenne à base de matériauxdopés ytterbium, la réalisation d’une chaîne laser de forte puissance moyenne compacte à base de fibre photoniquemicrostructurée à large aire modale sera présentée. Il sera notamment démontré les principales limitations en termed’énergie et de puissance moyenne. D’une part, le fort confinement de l’impulsion lumineuse dans le coeur de la fibrefavorise l’accumulation d’effets non-linéaires lors de l’amplification et détériore la qualité de l’impulsion. D’autrepart, en raison du diamètre de coeur important (> 70 μm) choisit pour lutter contre l’effet précèdent, le guidage dumode fondamental TEM00 de ces fibres est très critique et devient sensible à la charge thermique interne à la fibre.Cette source laser a été utilisée dans le cas de deux applications bien spécifiques : le perçage de plaques d’acierépaisses pour une finalité de déminage (relatif au cadre du financement de cette thèse par la Direction Générale del’Armement) et à la génération d’harmoniques d’ordres élevées à très haute cadence (relatif au domaine d’expertisedu CELIA). Ces deux applications sont traitées au cours du troisième chapitre.A la vue des limitations observées et afin de disposer de chaînes lasers plus énergétiques et offrant des duréesd’impulsions encore plus courtes, une nouvelles architecture d’amplification a été proposée : le pompage fortebrillance de matériaux dopés Ytterbium. Ce concept présenté dans le dernier chapitre utilise le développement desources fibrées monomodes continues émettant à 976 nm. Cette architecture d’amplification a été utilisée afin deréaliser d’une part un oscillateur sub-70 fs et de forte puissance moyenne (>2,3 W) à une cadence de 73 MHz etd’autre part : un amplificateur type « booster » à fort gain. Deux expériences qui ont été réalisées avec des cristauxd’Yb:CaF2. Ce matériaux présente en effet l’avantage d’avoir un très large spectre d’émission (>60 nm) propice à lagénération et amplification d’impulsions femtosecondes mais aussi d’être « compatible » avec les chaînes de trèsforte puissance grâce à sa très bonne conductivité thermique. / This work concerns the development of high repetition rate femtosecond lasers with high average power (>10 W)and energies in excess of 100 μJ. Such lasers are paramount for the development of new industrial applications(athermal micro-drilling, eye surgery, ...) and for fundamental research on high repetition rate laser matter interactionstudies.After a brief introduction and the state of the art summary on high-average power femtosecond laser with ytterbiumdoped materials, a compact high-average power femtosecond laser with a large mode area microstructured rod typeamplifier will be presented. It will browse the main limitations in terms of energy and average power. Limitationsare mainly due to the strong confinement of the electric field propagating in the fibre core leading to non-linear effectsaccumulated during the amplification. On the other hand, for larger core diameter (> 70 μm), the fundamental modeguiding (TEM00) is very weak and thus very sensitive to the internal thermal load of the fibre.This laser source has been used in two specific applications: athermal drilling of thick stainless steel plate for mineclearing(an application of interest for the Direction Générale de l’Armement) and High order Harmonics Generationat high repetition rate (related to CELIA activities). These two applications are presented in the third chapter.In order to stretch the limits and generate more energetic and a shorter pulse, a new amplification scheme has beenproposed, namely high brightness optical pumping of ytterbium doped materials. This concept presented in the lastchapter benefits from the development of high average power single-mode fibre lasers source emitting at 976 nm.This amplification scheme allowed us to realize a high average power Kerr-lens oscillator delivering pulses with apulse duration below than 70 fs and an average power of 2.3W at a repetition rate of 73 MHz. In a second phase, wealso developed a « booster » amplifier with a high single- pass-gain. These two results have been obtained by usingYb-doped CaF2 crystals. This material presents the advantage to have a very broad emission bandwidth (> 60nm)suitable to generate and amplify femtosecond pulses and to be compatible with high average power laser due to hisvery good thermal conductivity.

<p>I papperstillverkning ställs det krav inte bara på kvalité och kvantitet utan också att stickprov från produktion utförs och tas hand om på ett korrekt sätt. Från det att ett stickprov tas ut och undersöks på brukets laboratorium kan en del källor till förändringar på provresultatet uppstå. Sådana förändringar kan uppstå för det första vid hanteringen av stickprov från pappersmaskin och provens transportering till laboratoriet och för det andra vid laboratoriets hantering och uppföljning av kvalitén. En annan faktor som kan påverka stickproven är klimatet. Årstiderna vår och höst är de tider som proverna kan påverkas mest. Prover undersöks med jämna mellanrum från färdigt papper och används till kalibrering av on-line mätning på pappersmaskin. Vissa av provresultaten skickas direkt till kunden i form av ett analyscertifikat.</p><p>I detta examensarbete var syftet att analysera vissa felkällor i provhanteringen och vad klimatet hade för påverkan på provresultatet. Det undersöktes hur varierande klimatförhållanden på pappersmaskin kunde påverka provresultaten för prov som undersöktes direkt på laboratoriet. Resultat från de proven har sen jämförts med prov som konditionerades en tid på laboratoriet i ett fast klimat (23°C, 50 % RH). Prov konditionerades både efter att provet tagits ut direkt och efter att provet hade legat uppe i maskinhallen under en längre tid. I arbetet ingick det att årstider skulle simuleras och det utfördes på Stora Enso Research Center i Falun i ett speciellt klimatrum. Klimaten som papper undersöktes i då var extremt torrt och extremt fuktigt och dessa resultat jämfördes med resultat från normalt provtagningsklimat.</p><p>Papperskvalitéerna som undersöktes var 45 g/m2 standard tidningspapper från PM 11 och 52 g/m2 SC-papper (obestruket journalpapper) från Kvarnsvedens nya maskin PM 12. Det som undersöktes var de kritiska parametrarna där det föreligger risk för att papper måste kasseras. De kritiska egenskaperna som har kassaktionsgräns är ytvikt, ljushet, nyans och i även vissa fall ytråhet och rivstyrka.</p><p>Resultaten visade att vid extrema klimatförhållanden från undersökningen på Stora Enso Research Center hade många prover påverkats till den grad att de hade lett till kassaktion. För SC-papper var ytråheten den egenskap som var mest kritisk vid extremt torrt klimat och vid fuktigt klimat var ytvikt den mest känsliga egenskapen. För standard tidningspapper var ytvikt och rivstyrka de egenskaper som påverkades mest av extremt klimat och pappret hade fått kasseras vid både extremt torrt och fuktigt klimat.</p><p>Vid undersökningen på Kvarnsveden visade resultaten att fukthalten i pappret påverkades mer än vad papprets övriga egenskaper gjorde. Förändringarna i papprets övriga egenskaper var endast marginella och höll sig inom respektive gränsvärde för kassaktion. Nyans och de andra optiska egenskaperna hade marginella förändringar för både varierande och extrema klimatförhållanden och förändringarna kan i de flesta fall anses försumbara för produktionen.</p><p>I de fall där det råder extrema klimatförhållanden som det kan göra vid vissa årstider är det mycket viktigt att operatörens hantering av stickprov sker på ett korrekt sätt. Då gäller det att stickproverna skickas ner till laboratoriet så snabbt som möjligt där påverkan är mindre än vad den kan vara inne i maskinhallen.</p> / <p>In paper production demands are set not only on quality and quantity, but it is also required that samples from the production are taken out and handled in a correct way. From the moment when a sample is taken out and up to the point when it is examined in the laboratory of the mill, a number of factors may affect the sample and thus the test result. Such changes can arise from the handling of samples from the paper machine and the transport of the samples to the laboratory and also from the handling of the samples in the laboratory. Another factor that can influence the samples is the climate and the seasons spring and autumn is the times when the samples are influenced most. Samples are examined with even intervals from finished papers and is used for calibration of on-line measurement on the paper machine and some of the sample results are sent directly to the costumer in the form of an analysis certificate.</p><p>The purpose of this project was to analyze certain error sources in the sample handling and the impact of the climate on the sample result. It was examined how varying climates on the paper machine could influence the sample results for samples that were examined directly and compared with samples that were conditioned for one hour on the laboratory in a permanent climate (23°C, 50% RH). Samples that were conditioned were either taken directly to the lab or left by the paper machine for an extended period of time. In the work, it was included that seasons would be simulated and it was carried out on Stora Enso Research centre in Falun in a climate room. The climates that papers were examined in then were extreme dry and extreme damp and these results were compared with results from normal climate for testing paper.</p><p>The paper qualities that were examined where 45 g/m2 standard newspaper from papermachine 11 and 52 g/m2 SC-paper (uncoated journal papers) from the new papermachine 12 in Kvarnsveden. What were examined were the critical parameters were it exists risk to rejection of papers. The critical properties that have a limit when the papers are rejected are grammage, ISO-brightness and nuance and in certain cases also roughness and tear strength.</p><p>The results showed that at extreme climate relations from the studies on Stora Enso Research centre samples had been influenced to that degree that many of the samples had to be rejected. For SC-paper roughness was the property that was most critical at extremely dry climate and at damp climate the grammage was the most sensitive property. Standard newspaper was very sensitive at both extremely damp and dry climates for grammage and tearing strength.</p><p>The study on Kvarnsveden showed that the moisture content in the paper was influenced more than the other properties but its changes were only marginal and within the respective limit for rejection. Nuance and the other optic properties had only marginal changes for both varying and extreme climates and the changes can in most cases be considered negligible for the production.</p><p>In those cases when there are extreme climates, like during certain seasons, it is very important that the operator handles the samples correctly. Then, it is important that the samples are sent down to the laboratory as fast as possible where the impact is smaller than if the samples stay in the machine room.</p>

I papperstillverkning ställs det krav inte bara på kvalité och kvantitet utan också att stickprov från produktion utförs och tas hand om på ett korrekt sätt. Från det att ett stickprov tas ut och undersöks på brukets laboratorium kan en del källor till förändringar på provresultatet uppstå. Sådana förändringar kan uppstå för det första vid hanteringen av stickprov från pappersmaskin och provens transportering till laboratoriet och för det andra vid laboratoriets hantering och uppföljning av kvalitén. En annan faktor som kan påverka stickproven är klimatet. Årstiderna vår och höst är de tider som proverna kan påverkas mest. Prover undersöks med jämna mellanrum från färdigt papper och används till kalibrering av on-line mätning på pappersmaskin. Vissa av provresultaten skickas direkt till kunden i form av ett analyscertifikat. I detta examensarbete var syftet att analysera vissa felkällor i provhanteringen och vad klimatet hade för påverkan på provresultatet. Det undersöktes hur varierande klimatförhållanden på pappersmaskin kunde påverka provresultaten för prov som undersöktes direkt på laboratoriet. Resultat från de proven har sen jämförts med prov som konditionerades en tid på laboratoriet i ett fast klimat (23°C, 50 % RH). Prov konditionerades både efter att provet tagits ut direkt och efter att provet hade legat uppe i maskinhallen under en längre tid. I arbetet ingick det att årstider skulle simuleras och det utfördes på Stora Enso Research Center i Falun i ett speciellt klimatrum. Klimaten som papper undersöktes i då var extremt torrt och extremt fuktigt och dessa resultat jämfördes med resultat från normalt provtagningsklimat. Papperskvalitéerna som undersöktes var 45 g/m2 standard tidningspapper från PM 11 och 52 g/m2 SC-papper (obestruket journalpapper) från Kvarnsvedens nya maskin PM 12. Det som undersöktes var de kritiska parametrarna där det föreligger risk för att papper måste kasseras. De kritiska egenskaperna som har kassaktionsgräns är ytvikt, ljushet, nyans och i även vissa fall ytråhet och rivstyrka. Resultaten visade att vid extrema klimatförhållanden från undersökningen på Stora Enso Research Center hade många prover påverkats till den grad att de hade lett till kassaktion. För SC-papper var ytråheten den egenskap som var mest kritisk vid extremt torrt klimat och vid fuktigt klimat var ytvikt den mest känsliga egenskapen. För standard tidningspapper var ytvikt och rivstyrka de egenskaper som påverkades mest av extremt klimat och pappret hade fått kasseras vid både extremt torrt och fuktigt klimat. Vid undersökningen på Kvarnsveden visade resultaten att fukthalten i pappret påverkades mer än vad papprets övriga egenskaper gjorde. Förändringarna i papprets övriga egenskaper var endast marginella och höll sig inom respektive gränsvärde för kassaktion. Nyans och de andra optiska egenskaperna hade marginella förändringar för både varierande och extrema klimatförhållanden och förändringarna kan i de flesta fall anses försumbara för produktionen. I de fall där det råder extrema klimatförhållanden som det kan göra vid vissa årstider är det mycket viktigt att operatörens hantering av stickprov sker på ett korrekt sätt. Då gäller det att stickproverna skickas ner till laboratoriet så snabbt som möjligt där påverkan är mindre än vad den kan vara inne i maskinhallen. / In paper production demands are set not only on quality and quantity, but it is also required that samples from the production are taken out and handled in a correct way. From the moment when a sample is taken out and up to the point when it is examined in the laboratory of the mill, a number of factors may affect the sample and thus the test result. Such changes can arise from the handling of samples from the paper machine and the transport of the samples to the laboratory and also from the handling of the samples in the laboratory. Another factor that can influence the samples is the climate and the seasons spring and autumn is the times when the samples are influenced most. Samples are examined with even intervals from finished papers and is used for calibration of on-line measurement on the paper machine and some of the sample results are sent directly to the costumer in the form of an analysis certificate. The purpose of this project was to analyze certain error sources in the sample handling and the impact of the climate on the sample result. It was examined how varying climates on the paper machine could influence the sample results for samples that were examined directly and compared with samples that were conditioned for one hour on the laboratory in a permanent climate (23°C, 50% RH). Samples that were conditioned were either taken directly to the lab or left by the paper machine for an extended period of time. In the work, it was included that seasons would be simulated and it was carried out on Stora Enso Research centre in Falun in a climate room. The climates that papers were examined in then were extreme dry and extreme damp and these results were compared with results from normal climate for testing paper. The paper qualities that were examined where 45 g/m2 standard newspaper from papermachine 11 and 52 g/m2 SC-paper (uncoated journal papers) from the new papermachine 12 in Kvarnsveden. What were examined were the critical parameters were it exists risk to rejection of papers. The critical properties that have a limit when the papers are rejected are grammage, ISO-brightness and nuance and in certain cases also roughness and tear strength. The results showed that at extreme climate relations from the studies on Stora Enso Research centre samples had been influenced to that degree that many of the samples had to be rejected. For SC-paper roughness was the property that was most critical at extremely dry climate and at damp climate the grammage was the most sensitive property. Standard newspaper was very sensitive at both extremely damp and dry climates for grammage and tearing strength. The study on Kvarnsveden showed that the moisture content in the paper was influenced more than the other properties but its changes were only marginal and within the respective limit for rejection. Nuance and the other optic properties had only marginal changes for both varying and extreme climates and the changes can in most cases be considered negligible for the production. In those cases when there are extreme climates, like during certain seasons, it is very important that the operator handles the samples correctly. Then, it is important that the samples are sent down to the laboratory as fast as possible where the impact is smaller than if the samples stay in the machine room.

The intermontane Ipswich Basin, which is situated 30km south-west of Brisbane, contains coal measures formed in the Late Triassic Epoch following a barren non-depositional period. Coal, tuff, and basalt were deposited along with fluvial dominated sediments. The Ipswich Coal Measures mark the resumption of deposition in eastern Australia after the coal hiatus associated with a series of intense tectonic activity in Gondwanaland during the Permo-Triassic interval. A transtensional tectonic movement at the end of the Middle Triassic deformed the Toogalawah Group before extension led to the formation of the Carnian Ipswich Coal Measures in the east. The Ipswich Coal Measures comprise the Brassall and Kholo Subgroups. The Blackstone Formation, which forms the upper unit of the Brassall Subgroup, contains seven major coal seams. The lower unit of the Brassall Subgroup, the Tivoli Formation, consists of sixteen stratigraphically significant coal seams. The typical thickness of the Blackstone Formation is 240m and the Tivoli Formation is about 500m. The coal seams of the Ipswich Basin differ considerably from those of other continental Triassic basins. However, the coal geology has previously attracted little academic attention and the remaining exposures of the Ipswich coalfield are rapidly disappearing now that mining has ceased. The primary aim of this project was to study the patterns of coal sedimentation and the response of coal seam characteristics to changing depositional environments. The coal accumulated as a peat-mire in an alluvial plain with meandering channel systems. Two types of peat-mire expansion occurred in the basin. Peat-mire aggradation, which is a replacement of water body by the peatmire, was initiated by tectonic subsidence. This type of peat-mire expansion is known as terrestrialisation. It formed thick but laterally limited coal seams in the basin. Whereas, peat-mire progradation was related to paludification and produced widespread coal accumulation in the basin. The coal seams were separated into three main groups based on the mean seam thickness and aerial distribution of one-meter and four-meter thickness contour intervals. Group 1 seams within the one-meter thickness interval are up to 15,000m2 in area, and seams within the four-meter interval have an aerial extent of up to 10,000m2. Group 1A contains the oldest seam with numerous intraseam clastic bands and shows a very high thickness to area ratio, which indicates high subsidence rates. Group 1B seams have moderately high thickness to area ratios. The lower clastic influx and slower subsidence rates favoured peat-mire aggradation. The Group 1A seam is relatively more widespread in aerial extent than seams from Group 1B. Group 1C seams have low mean thicknesses and small areas, suggesting short-lived peat-mires as a result of high clastic influx. Group 2 seams arebetween 15,000 and 35,000m2 in area within the one-meter interval, and between 5,000 and 10,000m2 within the four-meter interval. They have moderately high area to thickness ratios, indicating that peat-mire expansion occurred due to progressively shallower accommodation and a rising groundwater table. Group 3 seams, which have aerial extents from 35,000 to 45,000m2 within the one-meter thickness contour interval and from 10,000 to 25,000m2 within the four-meter interval, show high aerial extent to thickness ratios. They were deposited in quiet depositional environments that favoured prolonged existence of peat-mires. Group 3 seams are all relatively young whereas most Group 1 seams are relatively old seams. All the major fault systems, F1, F2 and F3, trend northwest-southeast. Apart from the West Ipswich Fault (F3), the F1 and F2 systems are broad Palaeozoic basement structures and thus they may not have had a direct influence on the formation of the much younger coal measures. However, the sedimentation patterns appear to relate to these major fault systems. Depocentres of earlier seams in the Tivoli Formation were restricted to the northern part of the basin, marked by the F1 system. A major depocentre shift occurred before the end of the deposition of the Tivoli Formation as a result of subsidence in the south that conformed to the F2 system configuration. The Blackstone Formation depocentres shifted to the east (Depocentre 1) and west (Depocentre 2) simultaneously. This depocentre shift was associated with the flexural subsidence produced by the rejuvenation of the West Ipswich Fault. Coal accumulation mainly occurred in Depocentre 1. Two types of seam splitting occurred in the Ipswich Basin. Sedimentary splitting or autosedimentation was produced by frequent influx of clastic sediments. The fluvial dominant depositional environments created the random distribution of small seam splits. However, the coincidence of seam splits and depocentres found in some of the seams suggests tectonic splitting. Furthermore, the progressive splitting pattern, which displays seam splits overlapping, was associated with continued basin subsidence. The tectonic splitting pattern is more dominant in the Ipswich Basin. Alternating bright bands shown in the brightness profiles are a result of oscillating water cover in the peat-mire. Moderate groundwater level, which was maintained during the development of the peat, reduced the possibility of salinisation and drowning of the peat swamp. On the other hand, a slow continuous rise of the groundwater table, that kept pace with the vertical growth of peat, prevented excessive oxidation of peat. Ipswich coal is bright due to its high vitrinite content. The cutinite content is also high because the dominant flora was pteridosperms of Dicroidium assemblage containing waxy and thick cuticles. Petrographic study revealed that the depositional environment was telmatic with bog forest formed under ombrotrophic to mesotrophic hydrological conditions. The high preservation of woody or structured macerals such as telovitrinite and semifusinite indicates that coal is autochthonous. The high mineral matter content in coal is possibly due to the frequent influx of clastic and volcanic sediments. The Ipswich Basin is part of a much larger Triassic basin extending to Nymboida in New South Wales. Little is known of the coal as it lacks exposures. It is apparently thin to absent except in places like Ipswich and Nymboida. This study suggests that the dominant control on depocentres of thick coal at Ipswich has been the tectonism. Fluvial incursions and volcanism were superimposed on this.