A method is set forth which makes use of a commercially available, non-metric, solid-state matrix camera to capture spatial and spectral data from an individual tree bole that can be used to measure characteristics about the stem. In this study diameters and heights were measured and used to estimate the volume of 20 red oak (Quercus spp.) stems ranging in diameter at breast height from 16 to over 60 cm and height from 12 to 20 meters. Images were taken from four orthogonal directions around the each stem. Diameter estimates from matching camera to stem distances (3 to 15 meters) of opposite sides were arithmetically averaged. Two arithmetic averages from perpendicular directions were then geometrically averaged. It was found that locating the camera farther from the tree led to more consistent results over the entire stem while locating it closer to the tree provided the most precise estimates provided the inclination angle did not exceed 45 degrees. This method resulted in geometric mean diameter estimates within ± 4 cm for all heights combined when obtained at a distance of 12 m or greater using a 95 % chi-square maximum anticipated error statistic. Error increases with increased stem height from ± 3 cm to ± 7 cm for heights from 1 to 20 meters. In general, the error is equivalent to 3 times the instrument precision, which varies with distance. Two-thirds of the time volume estimates were within 8 percent, which is quite an improvement over the 30 percent interval afforded by an appropriate volume equation. / Master of Science

Nowadays, CCD observations are widely used to determine astrometric positions of minor planets differentially. Especially, follow-up observational programs require to produce and analyse a large number of CCD frames. This dissertation discusses the methods which are used to process such astrometrical CCD frames and extract scientific information from them. These methods are then combined into a complete astrometric software package. Among all corrections which have to be taken into consideration, special attention is given to the effects of differential chromatic refraction (DCR). It is demonstrated how the influence of DCR can be reduced using the photometric data of reference stars taken from the UCAC2 catalogue. In this way, for several test frames a gain in positional accuracy of about 15 percent has been achieved at a zenith distance of 65 degrees. Furthermore, different measurement algorithms of the image positions as well as the properties of several transformation models for the conversion between measured and tangential coordinates are analysed. In addition, the algorithm for automatic identification of reference stars is improved. With respect to the analysis of frames taken through follow-up observations of minor planets, software requirements are formulated. Considering these aspects the automatic universal computer program MpCCD has been developed and is presented and tested here. Particularly, it is compared to other astrometric applications, which are advised to be employed for the determination of minor planet positions by the IAU's Minor Planet Center. The developed software is able to measure positions of minor planets with high accuracy. For a series of test frames an average uncertainty of 62mas in the positions was achieved. This uncertainty is similar to the accuracy level of the UCAC2 catalogue used for the analysis. / Für Zwecke der differentiellen astrometrischen Positionsbestimmung von Kleinplaneten werden heutzutage verbreitet CCD-Beobachtungen eingesetzt. Insbesondere im Rahmen von Follow-up-Beobachtungsprogrammen sind eine Vielzahl von Aufnahmen herzustellen und auszuwerten. In dieser Arbeit werden Verfahren zur Auswertung solcher astrometrischer CCD-Aufnahmen diskutiert und später zu einem kompletten Messsystem für Kleinplaneten zusammengefügt. Unter den zu berücksichtigenden Korrekturen erhalten die Effekte der differentiellen chromatischen Refraktion (DCR) besondere Aufmerksamkeit. Es wird demonstriert, wie sich der Einfluss der DCR verringern lässt, indem die fotometrischen Angaben des Referenzsternkataloges UCAC2 hinzugezogen werden. Für Testaufnahmen ergaben sich so Verbesserungen der Lagegenauigkeit von 15 Prozent bei einer Zenitdistanz von 65 Grad. Des Weiteren werden verschiedene Messalgorithmen für Bildpositionen sowie die Eigenschaften diverser Transformationsmodelle für die Überführung von gemessenen in Tangentialkoordinaten untersucht. Außerdem erfolgt eine Weiterentwicklung des Algorithmus zur automatischen Identifikation von Referenzsternen. In Hinblick auf die Auswertung von Follow-up-Beobachtungen von Kleinplaneten werden Anforderungen an Software formuliert. Das nach diesen Gesichtspunkten entwickelte automatische universelle Computerprogramm MpCCD wird vorgestellt und getestet. Insbesondere findet ein Vergleich mit anderen astrometrischen Programmen statt, die vom Minor Planet Center der IAU zur Positionsbestimmung von Kleinplaneten empfohlen werden. Die entwickelte Software ist in der Lage, Positionen von Kleinplaneten mit hoher Genauigkeit zu ermitteln. Die für eine Reihe von Testaufnahmen verbliebenen Positionsunsicherheiten der Neupunkte von durchschnittlich 62mas liegen im Bereich der Koordinaten-Unsicherheiten des zur Auswertung verwendeten Referenzsternkataloges UCAC2.

Suivi de notre développement ou encore la compréhension de l’Univers. Deux technologies de capteurs d’image sont actuellement utilisées dans les missions d’imagerie de la Terre et de l’espace : les imageurs CCD (Charge Coupled Device) et CMOS. L’environnement radiatif spatial est constitué de particules énergétiques qui dégradent les performances des imageurs. Et il s’avère que les dégradations réelles observées en vol dépendent fortement des conditions orbitales et de fonctionnement et sont donc très difficiles à prédire. L’étude menée dans le cadre de cette thèse a pour objet la compréhension des dégradations subies par les capteurs CCD et CMOS lorsqu’ils sont soumis à l’environnement radiatif spatial et la proposition de méthodes d’évaluation mieux adaptées pour obtenir une meilleure prédiction de la dégradation réelle d’un imageur en orbite à partir de tests d’irradiation réalisés au sol. La démarche entreprise a tout d’abord consisté à identifier les paramètres d’essais au sol pouvant potentiellement être à l'origine des différences observées entre les résultats sol et vol. Un plan d’essai d’irradiation aux rayons y et aux protons a ainsi été défini afin d’évaluer la dégradation des imageurs CCD et CMOS dans des conditions de fonctionnement et d’irradiation proches de celles en vol. Nous avons étudié l’impact des conditions de mise en opération du composant durant l’irradiation (polarisation, rapport cyclique, etc.) mais aussi l’impact des conditions d’irradiation (débit de dose, énergies des protons, etc.). Le périmètre de cette thèse se limite à l’étude des effets sur le courant d’obscurité, sur la dispersion pixel-à-pixel du courant d’obscurité et sur l’apparition des pixels chauds, qui sont, au premier ordre, les principaux critères de performances dégradés d’un imageur par les radiations. L’étude de l’influence du débit de dose de l’irradiation a montré un phénomène ELDRS (Enhanced Low Dose Rate Sensitivity) pour la première fois sur un capteur CCD polarisé dynamiquement avec un rapport cyclique ON/OFF. Les conditions de polarisation dynamique évaluées sur les APS ont démontré que la dégradation est d’autant plus importante que la fréquence d’activation et le rapport cyclique sont grands. Les irradiations aux protons sur les imageurs CMOS ont aussi montré l’apparition et la guérison de pixels chauds après irradiation à température ambiante ainsi que l'apparition du bruit de signal aléatoire télégraphique (RTS). Ces deux modes de dégradation ont été analysés plus en détail afin d'évaluer leur comportement en guérison pour le premier et extraire les statistiques d'apparition sur l'autre, sur un grand nombre de pixels. En parallèle, un code de simulation de l’effet de dose dans les oxydes de structures élémentaires MOS, ACDC (Accumulation des Charges en Dose Cumulée), a été adapté et utilisé. Ce code a permis de mettre en évidence les constantes de temps impliquées dans la dégradation par effets ionisants dans ces structures. Ces constantes de temps sont utilisées pour l'interprétation des effets de la polarisation dynamique. Les résultats expérimentaux obtenus sur les capteurs d’image CCD et CMOS ont un impact sur l’assurance durcissement. Les irradiations aux protons des imageurs CMOS ont notamment montré un phénomène de guérison des pixels chauds plus marqué que sur les autres pixels, montrant l'intérêt d'une caractérisation de plusieurs semaines après irradiation. Pour les irradiations au Co60 des imageurs CMOS, il est recommandé de ne pas utiliser des temps de polarisation ON trop courts (périodes de cycle petites) car cela peut conduire à une sous-estimation de la dégradation (charge piégée et états d'interface). / Two imaging sensor technologies are presently used in Earth and space imagery missions: Charge Couple Devices (CCD) and CMOS detectors. The space radiation environment is composed of energetic particles that degrade imaging sensor’s performances. It has been shown that real in-orbit degradation of imaging sensors are strongly dependent of orbital and operating conditions and are, as a consequence, difficult to predict. The work performed in this thesis has for purpose an understanding of space radiation-induced degradations for both CCD and CMOS technologies and the proposal of better suited assessment methods for these specific devices in order to better prediction of real in-orbit detector’s degradation from on-ground irradiation tests. The first step of the work focused on the identification of on-ground test parameters that could possibly explain the differences observed between inorbit and on-ground data. Thus an irradiation test plan to y-rays and proton particles has been defined in order to assess the imaging sensor’s degradation for both CCD and CMOS technologies in operating and irradiation conditions close to in-orbit ones. The effects of detector’s operation conditions during irradiation (bias, duty cycle, etc.) but also the irradiation conditions (dose rate, proton energy, etc.) have been studied. The present work focuses on effects on dark current, on its pixel to pixel dispersion and on the presence of hot pixels, which are, at first order, the main performance parameters of an imaging sensor that is degraded by space radiations. The study of the irradiation dose rate influence has shown an Enhanced Low Dose Rate Sensitivity (ELDRS) phenomenon observed for the first time on a CCD imager under dynamic bias condition with a ON/OFF duty cycle. The tested bias conditions CMOS image sensors have demonstrated that the higher the activation frequency and duty cycle, the higher is the degradation. Besides, the proton irradiations performed on CMOS detectors have induced hot pixels that anneal just after irradiation at room temperature. A random telegraphic signal (RTS) behaviour of the dark current has also been shown on CMOS sensors. In parallel to the irradiation tests, a simulation code of ionizing dose effects on oxides of MOS elementary structures has been adapted and used. This program, called ACDC (Accumulation des Charges en Dose Cumulée), has allowed to assess the quantification time constants of physical mechanisms that induce ionizing dose degradation on these structures. These time constants are used for the interpretation of dynamic bias effects.

Nowadays, CCD observations are widely used to determine astrometric positions of minor planets differentially. Especially, follow-up observational programs require to produce and analyse a large number of CCD frames. This dissertation discusses the methods which are used to process such astrometrical CCD frames and extract scientific information from them. These methods are then combined into a complete astrometric software package. Among all corrections which have to be taken into consideration, special attention is given to the effects of differential chromatic refraction (DCR). It is demonstrated how the influence of DCR can be reduced using the photometric data of reference stars taken from the UCAC2 catalogue. In this way, for several test frames a gain in positional accuracy of about 15 percent has been achieved at a zenith distance of 65 degrees. Furthermore, different measurement algorithms of the image positions as well as the properties of several transformation models for the conversion between measured and tangential coordinates are analysed. In addition, the algorithm for automatic identification of reference stars is improved. With respect to the analysis of frames taken through follow-up observations of minor planets, software requirements are formulated. Considering these aspects the automatic universal computer program MpCCD has been developed and is presented and tested here. Particularly, it is compared to other astrometric applications, which are advised to be employed for the determination of minor planet positions by the IAU's Minor Planet Center. The developed software is able to measure positions of minor planets with high accuracy. For a series of test frames an average uncertainty of 62mas in the positions was achieved. This uncertainty is similar to the accuracy level of the UCAC2 catalogue used for the analysis. / Für Zwecke der differentiellen astrometrischen Positionsbestimmung von Kleinplaneten werden heutzutage verbreitet CCD-Beobachtungen eingesetzt. Insbesondere im Rahmen von Follow-up-Beobachtungsprogrammen sind eine Vielzahl von Aufnahmen herzustellen und auszuwerten. In dieser Arbeit werden Verfahren zur Auswertung solcher astrometrischer CCD-Aufnahmen diskutiert und später zu einem kompletten Messsystem für Kleinplaneten zusammengefügt. Unter den zu berücksichtigenden Korrekturen erhalten die Effekte der differentiellen chromatischen Refraktion (DCR) besondere Aufmerksamkeit. Es wird demonstriert, wie sich der Einfluss der DCR verringern lässt, indem die fotometrischen Angaben des Referenzsternkataloges UCAC2 hinzugezogen werden. Für Testaufnahmen ergaben sich so Verbesserungen der Lagegenauigkeit von 15 Prozent bei einer Zenitdistanz von 65 Grad. Des Weiteren werden verschiedene Messalgorithmen für Bildpositionen sowie die Eigenschaften diverser Transformationsmodelle für die Überführung von gemessenen in Tangentialkoordinaten untersucht. Außerdem erfolgt eine Weiterentwicklung des Algorithmus zur automatischen Identifikation von Referenzsternen. In Hinblick auf die Auswertung von Follow-up-Beobachtungen von Kleinplaneten werden Anforderungen an Software formuliert. Das nach diesen Gesichtspunkten entwickelte automatische universelle Computerprogramm MpCCD wird vorgestellt und getestet. Insbesondere findet ein Vergleich mit anderen astrometrischen Programmen statt, die vom Minor Planet Center der IAU zur Positionsbestimmung von Kleinplaneten empfohlen werden. Die entwickelte Software ist in der Lage, Positionen von Kleinplaneten mit hoher Genauigkeit zu ermitteln. Die für eine Reihe von Testaufnahmen verbliebenen Positionsunsicherheiten der Neupunkte von durchschnittlich 62mas liegen im Bereich der Koordinaten-Unsicherheiten des zur Auswertung verwendeten Referenzsternkataloges UCAC2.

This master’s work deals with types of digital cameras used in industry. Furthermore, there are mentioned application areas of cameras in the automotive industry. There was created searches industrial cameras on the market. In the next part is described hardware interconnection of Basler acA 1300-60gc camera and measuring platform cDAQ 9178. Part of this work is to create a system for synchronization of camera and measured data. In the last part is developed program for image processing and determine the angle of rotation of the steering wheel.

L'approche développée par l'équipe imXgam du CPPM a consisté à adapter la technologie des pixels hybrides XPAD à l'imagerie biomédicale. C'est dans cette optique qu'un micro-tomodensitomètre PIXSCAN II basé sur la nouvelle génération de détecteurs à pixels hybrides appelés XPAD3 a été développé. Ce travail de thèse décrit la démarche engagée pour évaluer l'apport de la technologie à pixels hybrides en tomodensitométrie par rayons X en termes de contraste et de dose et pour explorer de nouvelles possibilités d'imagerie biomédicale à faible dose. L'évaluation des performances ainsi que la validation des résultats obtenus avec les données acquises avec le détecteur XPAD3 ont été comparées aux résultats obtenus avec la caméra CCD DALSA XR-4 similaire aux détecteurs utilisés dans la plupart des micro-TDM usuels. Le détecteur XPAD3 permet d'obtenir des images reconstruites d'une qualité satisfaisante et proche de celle des images de la caméra DALSA XR-4, mais avec une meilleure résolution spatiale. A faible dose, les images du détecteur XPAD3 sont de meilleure qualité que celles de la caméra CCD. Du point de vue de l'instrumentation, ce projet a prouvé le bon fonctionnement du dispositif PIXSCAN II pour la souris. Nous avons pu reproduire une qualité d'image semblable à celle obtenue avec un détecteur à intégration de charges de type caméra CCD. Pour améliorer les performances du détecteur XPAD3, il va falloir optimiser la stabilité des seuils et avoir des courbes de réponses des pixels en fonction de l'énergie assez homogènes en utilisant un capteur plus dense comme le CdTe par exemple. / The pathway that has been followed by the imXgam team at CPPM was to adapt the hybrid pixel technology XPAD to biomedical imaging. It is in this context that the micro-CT PIXSCAN II based on the new generation of hybrid pixel detectors called XPAD3 has been developed. This thesis describes the process undertaken to assess the contribution of the hybrid pixel technology in X-ray computed tomography in terms of contrast and dose and to explore new opportunities for biomedical imaging at low doses. Performance evaluation as well as the validation of the results obtained with data acquired with the detector XPAD3 were compared to results obtained with the CCD camera DALSA XR-4 similar to detectors used in most conventional micro-CT systems. The detector XPAD3 allows to obtain reconstruced images of satisfactory quality close to that of images from the DALSA XR-4 camera, but with a better spatial resolution. At low doses, the images from the detector XPAD3 have a better quality that is those from CCD camera. From an instrumentation point of view, this project demonstrated the proper erations of the device PIXSCAN II for mouse imaging. We were able to reproduce an image quality similar to that obtained with a charge integration detector such as a CCD camera. To improve the performance of the detector XPAD3, we will have to optimize the stability of the thresholds and in order to obtain more homogeneous response curves of the pixels as a function as energy by using a denser sensor such as CdTe.

A análise da retina permite o diagnostico de muitas patologias relacionadas ao olho humano. A qualidade da imagem e um fator importante já que o médico normalmente examina os pequenos vasos da retina e a sua coloração. O equipamento normalmente utilizado para a visualização da retina e o retinógrafo digital, que utiliza sensor colorido com filtro de Bayer e luz (flash) branca. No entanto, esse filtro causa perda na resolução espacial, uma vez que e necessário um processo de interpolação matemática para a formação da imagem. Com o objetivo de melhorar a qualidade da imagem da retina, um retinógrafo com câmera CCD monocromática de alta resolução foi desenvolvido. Nele, as imagens coloridas são geradas pela combinação dos canais monocromáticos R (vermelho), G (verde) e B (azul), adquiridos com o chaveamento da iluminação do olho com LED vermelho, verde e azul, respectivamente. Entretanto, o pequeno período entre os flashes pode causar desalinhamento entre os canais devido a pequenos movimentos do olho. Assim, este trabalho apresenta uma técnica de registro de imagens, baseado em correlação de fase no domínio da frequência, para realizar precisamente o alinhamento dos canais RGB no processo de geração de imagens coloridas da retina. A validação do método foi realizada com um olho mecânico (phantom) para a geração de 50 imagens desalinhadas que foram corrigidas pelo método proposto e comparadas com as imagens alinhadas obtidas como referência (ground-truth). Os resultados mostraram que retinógrafo com câmera monocromática e o método de registro proposto nesse trabalho podem produzir imagens coloridas da retina com alta resolução espacial, sem a perda de qualidade intrínseca às câmeras CCD coloridas que utilizam o filtro de Bayer. / The analysis of retina allows the diagnostics of several pathologies related to the human eye. Image quality is an important factor since the physician often examines the small vessels of the retina and its color. The device usually used to observe the retina is the fundus camera, which uses color sensor with Bayer filter and white light. However, this filter causes loss of spatial resolution, since it is necessary a mathematical interpolation process to create the final image. Aiming at improving the retina image quality, a fundus camera with monochromatic CCD camera was developed. In this device, color images are generated by combining the monochromatic channels R (red), G (green) and B (blue), which were acquired by switching the eye illumination with red, green and blue light, respectively. However, the short period between the flashes may cause misalignment among the channels because of the small movements of the eye. Thus, this work presents an image registration technique based on phase correlation in the frequency domain, for accurately aligning the RGB channels on the process of generating retina color images. Validation of the method was performed by using a mechanical eye (phantom) for generating 50 misaligned images, which were aligned by the proposed method and compared to the aligned images obtained as references (ground-truth). Results showed that the fundus camera with monochromatic camera and the method proposed in this work can produce high spatial resolution images without the loss of quality intrinsic to color CCD cameras that uses Bayer filter.

The interstellar matter in the Galaxy is concentrated in a thin layer close to the galactic plane, mostly in spiral arms. Most of the interstellar matter is in a form of atomic and molecular gas and only 1% of its mass is in a form of small (0.01 – 0.1 µm) dust grains which absorb and scatter the light of stars and cause the interstellar extinction. A part of interstellar gas and dust are in a diffuse form and fill the space with density which exponentially decreases with the distance from the galactic plane. However, in the spiral arms gigantic molecular clouds are present which play an outstanding role in the evolution of the Galaxy, since in them star forming processes take place. Molecular and dust clouds, young star clusters and associations and other star forming regions are concentrated in the Milky Way plane. However, due to gravitational and radiation interactions between the molecular clouds and the young massive stars, some fragments of spiral arms deviate from the galactic plane. One of such deviating branches from the Local (Orion) spiral arm is a huge elongated system of molecular and dust clouds located in the Cepheus constellation which is known as the Cepheus Flare. Most of the objects investigated in this dissertation belong to this branch of the Local spiral arm. The objects selected for the investigation are star forming regions in the vicinity of the reflection nebula NGC 7023, a group of dark clouds TGU 619, the young open cluster NGC 7129 and the... [to full text] / Paukščių tako Galaktikoje didžioji dalis tarpžvaigždinės medžiagos yra susitelkusi į ploną sluoksnį Galaktikos plokštumoje, daugiausiai spiralinėse vijose. Didžiąją dalį tarpžvaigždinės medžiagos sudaro atominės ir molekulinės dujos ir tik maždaug 1% masės yra mažos (0.01 – 0.1 µm) dydžio dulkelės, kurios sugeria ir išsklaido šviesą ir sukelia tarpžvaigždinės ekstinkcijos reiškinį. Spiralinėse vijose esantys molekuliniai debesys yra svarbūs Galaktikos evoliucijos procese, nes juose vyksta aktyvūs žvaigždžių formavimosi procesai. Molekuliniai ir dulkių debesys, jaunų žvaigždžių spiečiai ir asociacijos bei kitos žvaigždžių susidarymo sritys dažniausiai yra Galaktikos plokštumoje. Tačiau dėl gravitacinės ir radiacinės sąveikos tarp jaunų didelės masės žvaigždžių ir molekulinių debesų kai kuriose Paukščių Tako srityse žvaigždėdaros rajonai nukrypsta nuo Galaktikos plokštumos. Viename iš tokių rajonų Cefėjo žvaigždyno kryptimi dalis tarpžvaigždinių debesų ir žvaigždėdaros rajonų yra nukrypę nuo Galaktikos plokštumos link šiaurinio dangaus poliaus ir sudaro Paukščių Tako atšaką, literatūroje žinomą kaip Cepheus Flare. Dauguma šioje disertacijoje tyrinėjamų objektų priklauso šiai Cefėjo atšakai. Šio darbo tikslas yra Cefėjo žvaigždėdaros rajonų, žinomų kaip atspindžio ūkas NGC 7023, tamsiųjų debesų kompleksas TGU 619 ir jaunas spiečius NGC 7129 fotometrinis tyrimas, siekiant nustatyti šių objektų nuotolį ir tarpžvaigždinę ekstinkciją, jauno spiečiaus NGC 7129 ir... [toliau žr. visą tekstą]

Paukščių Tako Galaktikoje didžioji dalis tarpžvaigždinės medžiagos yra susitelkusi į ploną sluoksnį Galaktikos plokštumoje, daugiausiai spiralinėse vijose. Didžiąją dalį tarpžvaigždinės medžiagos sudaro atominės ir molekulinės dujos ir tik maždaug 1% masės yra mažos (0.01 – 0.1 µm) dydžio dulkelės, kurios sugeria ir išsklaido šviesą ir sukelia tarpžvaigždinės ekstinkcijos reiškinį. Spiralinėse vijose esantys molekuliniai debesys yra svarbūs Galaktikos evoliucijos procese, nes juose vyksta aktyvūs žvaigždžių formavimosi procesai. Molekuliniai ir dulkių debesys, jaunų žvaigždžių spiečiai ir asociacijos bei kitos žvaigždžių susidarymo sritys dažniausiai yra Galaktikos plokštumoje. Tačiau dėl gravitacinės ir radiacinės sąveikos tarp jaunų didelės masės žvaigždžių ir molekulinių debesų kai kuriose Paukščių Tako srityse žvaigždėdaros rajonai nukrypsta nuo Galaktikos plokštumos. Viename iš tokių rajonų Cefėjo žvaigždyno kryptimi dalis tarpžvaigždinių debesų ir žvaigždėdaros rajonų yra nukrypę nuo Galaktikos plokštumos link šiaurinio dangaus poliaus ir sudaro Paukščių Tako atšaką, literatūroje žinomą kaip Cepheus Flare. Dauguma šioje disertacijoje tyrinėjamų objektų priklauso šiai Cefėjo atšakai. Šio darbo tikslas yra Cefėjo žvaigždėdaros rajonų, žinomų kaip atspindžio ūkas NGC 7023, tamsiųjų debesų kompleksas TGU 619 ir jaunas spiečius NGC 7129 fotometrinis tyrimas, siekiant nustatyti šių objektų nuotolį ir tarpžvaigždinę ekstinkciją, jauno spiečiaus NGC 7129 ir... [toliau žr. visą tekstą] / The interstellar matter in the Galaxy is concentrated in a thin layer close to the galactic plane, mostly in spiral arms. Most of the interstellar matter is in a form of atomic and molecular gas and only 1% of its mass is in a form of small (0.01 – 0.1 µm) dust grains which absorb and scatter the light of stars and cause the interstellar extinction. A part of interstellar gas and dust are in a diffuse form and fill the space with density which exponentially decreases with the distance from the galactic plane. However, in the spiral arms gigantic molecular clouds are present which play an outstanding role in the evolution of the Galaxy, since in them star forming processes take place. Molecular and dust clouds, young star clusters and associations and other star forming regions are concentrated in the Milky Way plane. However, due to gravitational and radiation interactions between the molecular clouds and the young massive stars, some fragments of spiral arms deviate from the galactic plane. One of such deviating branches from the Local (Orion) spiral arm is a huge elongated system of molecular and dust clouds located in the Cepheus constellation which is known as the Cepheus Flare. Most of the objects investigated in this dissertation belong to this branch of the Local spiral arm. The objects selected for the investigation are star forming regions in the vicinity of the reflection nebula NGC 7023, a group of dark clouds TGU 619, the young open cluster NGC 7129 and the... [to full text]

In general, natural and synthetic phenazines have attracted much attention because of their biological activities, like antitumour agents antimalarials, antibiotics, among others. The natural phenazines are isolated as secondary metabolites of terrestrial and marine microorganisms, mainly of Pseudomonas spp. and Streptomyces spp. This work aiming the structural determination of phenazinics compounds, derivatives that present bioactivity for the treatment of malaria and tuberculosis, using the X-ray diffraction method. The phenazinics compounds had been: (Fena-3244): 14b-Chloro-4amethoxy- 3,3-dimethyl-2,3,4a,14b-tetrahydro-1H-benzo[a]-pyrano[2,3-c]phenazine, (Fena-3243): 1,5-Dioxa-3-dimethyl-benzo[g ]oxanane[e -b]quinoxaline (Fena- 3279): 2,5,5-Trimethyl-benzo[c]-cyclohexan[c ]pyran[e ,a]phenazine (Fena- 3245): 1-allyl2-oxa-10-hydro-2H, 10H-benzo[c]phenazine. All the data collection had been obtained in one automatic KappaCCD, diffractometer using monocromatizada radiation for a graphite crystal, of wave length of 0.71073 Å (molybdenum). The compound Fena-3244 crystallize in the Monoclinic system and belongs to space group P121/n1, with cell parameters a =15.5498 (6) Å, b = 6.97000 (10) Å, c = 17.4872 (7) Å, β = 92.488 (2) Å, with a volume, V = 1893.51 (11) Å3. The compound Fena-3243, crystallize in the Monoclinic system and belongs to the space group P121/C1, with cell parameters of a = 8.3700 (5) Å, b = 11.5120 (9) Å, c = 18.5370 (10) Å, β = 110.223 (4)°, with a volume, V= 1676.03 (19) Å 3. The compound Fena-3279, crystallize in the crystalline system Triclinic, belongs to the space group P - 1, with parameters of a = 10.9810 (4), b = 12.6080 (7), c =16.0080 (6) Å, α = 88.449 (3)°, β = 71.118 (2)°, γ = 87.203 (2)°, V = 1047.18 (8) Å3 . The compound Fena-3245, crystallize in the Triclinic system and belongs to the space group P - 1, with cell parameters of a = 9.4880 (5) Å, b= 17.7650 (13) Å , c= 18.0760 (12) Å , V= 2818.4 (3) Å3 . The results for the compound Fena-3244 and Fena-3243 confirmed their proposed structures for different spectroscopic techniques (NMR, Utraviolet). The results for Fena-3279 show the existing doubts about the aromaticity of ring C. For Fena-3245 revealed the discrepancy structural model of the proposed model as compared to the functional binder group in C5. There were also certain all possible interactions of hydrogen in the bundling of crystalline molecules, allowing them to be established their respective arrangements. / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / Em geral, fenazinas naturais e sintéticas têm atraído muita atenção devido às suas atividades biológicas interessantes, como agentes antitumorais antimaláricos, antibióticos entre outros. As fenazinas naturais são isoladas como metabólitos secundários de microorganismos terrestres e marinhos, principalmente de Pseudomonas spp. e Streptomyces spp. O presente trabalho tem por objetivo a determinação das estruturas cristalinas e moleculares de 4 compostos fenazínicos derivados do Lapachol, que apresentam bioatividade para o tratamento da tuberculose e da malária, empregando o método de difração de raios X. Os compostos fenazínicos estudados neste trabalho foram: (Fena-3244): 14b-Cloro-4a-metoxi-3,3-dimetil-2,3,4a,14b-tetrahidro-1H-benzo[a]-pirano [2,3- c]fenazina (Fena-3243): 1,5-Dioxa-3-dimetil-benzo[g ]oxanana[e -b]quinoxalina (Fena-3279): 2,5,5-Trimetil-benzo[c]-ciclohexano[c ]piran[e ,a]fenazina (Fena- 3245): 1-allil-2-oxa-10-hidro-2H, 10H-benzo[c]fenazina.Todos os dados das intensidades difratadas foram obtidos num difratômetro automático KappaCCD, utilizando radiação monocromatizada por um cristal de grafite, de comprimento de onda igual a 0,71073 Å (molibdênio). O composto (Fena-3244) cristaliza no sistema monoclínico e grupo espacial P121/n1, tendo como parâmetros de rede: a = 15,5498(6) Å, b = 6,9700(10) Å, c = 17,4872(7) Å, β = 92,488(2)° e um volume, V= 1893,51(11) Å 3. O composto (Fena-3243) cristaliza no sistema monoclínico e grupo espacial P121/c1, tendo como parâmetros de rede: a = 8,3700(5) Å, b = 11,5120(9) Å, c = 18,5370(10) Å, β = 110,223(4)°, com um volume, V= 1676,03(19) Å 3. O composto (Fena-3279) cristaliza no sistema triclínico e grupo espacial P-1, tendo como parâmetros de rede: a = 10,9810(4) Å, b = 12,6080(7) Å, c = 16,0080(6) Å, α= 88,45(3)°, β = 71,118(2)°, γ = 87,203(2)° com um volume, V= 1047,18(8) Å 3. O composto (Fena-3245) cristaliza no sistema triclínico e grupo espacial P-1, tendo como parâmetros de rede: a = 9,4880(5) Å, b = 17,7650(13) Å, c = 18,0760(12) Å, α= 112,321(3)°, β = 90,267(4)°, γ = 90,077(4)° com um volume, V= 2818,4(3) Å 3. Os resultados obtidos para os compostos Fena-3244, Fena-3243 confirmaram as respectivas estruturas propostas por diferentes técnicas espectroscópicas (RMN, Utravioleta). Os resultados para Fena-3279 elucidaram a duvida existente quanto à aromaticidade do anel C. Para Fena-3245 evidenciaram a discordância do modelo estrutural comparado ao modelo proposto quanto ao grupo funcional ligante em C5. Foram determinadas também todas as possíveis interações de hidrogênio nos empacotamentos cristalinos das moléculas, permitindo que fossem estabelecidos os seus respectivos arranjos.