La structure du milieu interstellaire est très hétérogène dans notre Galaxie. Les observations, ainsi que les lois d'échelle, suggèrent que sa structure pourrait être fractale. Les plus petites structures de gaz ou clumps auraient un rayon de quelques unités astronomiques et une température de quelques kelvins, les rendant très difficilement détectables. Ces nuages de gaz moléculaires froids et denses peuvent donc être des candidats peu lumineux à une matière noire baryonique.L'objectif de cette thèse est de trouver des indices observationnels de l'existence de ces sous-structures gazeuses. La méthodologie consiste à comparer les magnitudes apparentes d'étoiles à différents intervalles de temps et vers plusieurs directions dans la Galaxie; afin de détecter des variations photométriques temporelles compatibles avec un événement d'obscurcissement. En effet, si un nuage moléculaire se trouve en amont d'une étoile, celle-ci sera obscurcie ou occultée par les sous-structures composant le nuage moléculaire, pendant une certaine durée de temps (dépendant de la vitesse de chaque objet et du temps d'observation considéré). Dans un premier temps, nous avons effectué un traitement photométrique complet pour chercher de tels événements dans l'amas globulaire NGC 4833 en comparant des observations photométriques séparées de six mois. Cet amas fut observé par D. Puy et D. Pfenniger en janvier et juillet 2006. Puis, nous avons utilisé des observations de plusieurs amas globulaires observés par le télescope Hubble, dont la photométrie est connue et rendue publique.Finalement, nous avons développé des méthodes d'apprentissage automatique afin de détecter des événements d'obscurcissement dans le Sloan Digital Sky Survey, Stripe 82.Aucun événement d’obscurcissement d'étoiles n'a pu être détecté ni dans la direction des amas globulaires considérés ni dans la région de Stripe 82. Néanmoins, des simulations d'un nuage fractal ont été réalisées pour estimer la probabilité d’occurrence du phénomène d'obscurcissement d'étoiles. Elles montrent que l’événement est extrêmement rare, ce qui permet d'émettre une nouvelle stratégie d'observation pour augmenter les chances de détecter de tels événements. De plus, les méthodes d'apprentissage automatique utilisées pour cette étude sont appliquées à d'autres objets variables tel que les quasars, très nombreux dans Stripe 82, et peuvent être utilisées pour d'autres objets variables tels que les supernovae. / The scaling laws and the very appearance of the interstellar medium suggest that this medium might have a fractal structure. The smallest structure of gas called clumps might have a radius about few astronomical units and a very low temperature of few kelvins, making them very difficult to detect. That is why, cold, dense, molecular clouds could be ideal candidates for baryonic dark matter. Because of their low temperature, they do not radiate, and seem to be dark.The aim of this thesis is to highlight observational clues on the existence of clumps by comparing apparent magnitudes of stars at different times, and towards different directions in the Galaxy. If a molecular fractal cloud lies behind a star, it will be obscured or occulted within a certain time (depending on the velocity of each object and on observational time). Therefore the goal of this thesis is to detect magnitude-time variations of stars compatible with an obscuration event.First, we did a complete photometric data reduction of observations of a globular cluster, NGC 4833, carried out by D. Puy and D. Pfenniger in January and July 2006. We wanted to detect obscuration events of stars in NGC 4833, in a six-month period. Then, we used public data of several globular clusters observed by the Hubble Space telescope.Finally, we developed machine learning methods to detect obscuration events in the Sloan Digital Sky Survey, Stripe 82.No obscuration events were detected either in several globular clusters, or in the Stripe 82 survey. However, we performed simulations of a fractal cloud to estimate probabilities of obscuration events. They show that such events are very rare, allowing us to develop a new observational strategy for increasing the probability of detecting obscuration events. Moreover, machine learning methods used in this study are applied to other variable objects, such as quasars which are numerous inside Stripe 82 survey, and could be used to other variables objects such as supernovae for example.

The aim of this work has been to increase our understanding of the surface brightness distributions of late-type stars through Doppler imaging and eclipse mapping techniques. Combining spectroscopic and photometric observations with the technique of Doppler Imaging, I have reconstructed surface images of the G2V star He 699 (for 08 October 2000), which show high latitude and polar structures. In the case of the KOV star AB Dor, the Doppler images for January 1992 and November 1993 show a large polar cap with small dark features also present at intermediate to high latitudes. As the phase sampling of the observations was insufficient to apply the sheared-image method it was not possible to detect any differential rotation. In the second part of my thesis I determine the surface brightness distribution of the primary component of the RS CVn eclipsing binary SV Cam. I have used extrapolated size distributions of sunspots to an active star to synthesize images of stellar photospheres with high spot filling factors. The resulting surface images, reconstructed with the Maximum Entropy eclipse mapping technique, show large spurious spot features at the quadrature points. It is concluded that two-spot modelling or chi-squared minimisation techniques are more susceptible to spurious structures being generated by systematic errors, arising from incorrect assumptions about photospheric surface brightness, than simple Fourier analysis of the light-curves. Spectrophotometric data from 9 HST orbits, observed in November 2001, have been used to eclipse-map the primary component of SV Cam. In combination with its HIPPAR- COS parallax it is found that the surface flux in the eclipsed low-latitude region is about 30% lower than computed from the best fitting PHOENIX model atmosphere. This flux deficit can only be accounted for if about a third of the primary's surface is covered with unresolved spots. However, when the spottedness from the eclipsed region is applied to the entire surface of the primary star, there still remains an unaccounted flux deficit. The remaining flux deficit is explained by the presence of a large polar spot extending down to latitude 48+/-6 deg. When the Maximum Entropy eclipse mapping technique is used to fit SV Cam's lightcurve, the observed minus computed residuals show strong spurious peaks at the quadrature points. It is only possible to reduce these peaks with the addition of a polar cap and the reduction of the primary star's temperature, to account for the star being peppered with unresolvable spots. Motivated by this result we investigate the limb darkening of the primary component of SV Cam. The wavelength dependence of the limb darkening is analysed by sub-dividing the HST lightcurve into 10 bands of equal emission flux. Flux variations between the first and fourth contact of the primary eclipse indicate that the limb darkening decreases towards longer wavelengths, in accordance with published limb darkening laws. Comparing fits of ATLAS and PHOENIX model atmospheres we find a wavelength dependence of the best fitting model. Due to its smooth cutoff at the stellar limb, the spherical geometry of the PHOENIX model atmosphere gives the best fit during partial eclipse. Between the second and third contact the difference between spherical and plane-parallel geometry is less important.

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As galáxias espirais continuam desafiando as teorias que buscam explicar como o universo se tornou o que observamos hoje. Em especial, no contexto hierárquico de formação de estruturas, é difícil entender como as galáxias podem ser tão parecidas entre si, obedecendo a relações de escala tão estritas, apesar de suas diferentes histórias evolutivas. A fim de esclarecer algumas dessas perguntas, o projeto GHASP observou 203 galáxias na linha H-alfa, através de interferometria Fabry-Perot, construindo uma base de dados homogênea e de alta qualidade para estudos cinemáticos do universo local. Neste trabalho, buscamos complementar os resultados consolidados do GHASP, apresentando um estudo fotométrico para 173 destas galáxias na banda Rc. Os dados, provenientes de observações no telescópio de 1,2m do Observatório de Haute-Provence ou do projeto SDSS, foram cuidadosamente tratados com ferramentas de redução IRAF adaptados para a automação dos processos. Através do ajuste de elipses sobre as galáxias, foram obtidos perfis de brilho calibrados e magnitudes totais para as galáxias da amostra. A decomposição da luz destes perfis foi estudada através de um modelo exponencial para o disco e uma função de Sérsic para o bojo. Os resultados da decomposição bojo-disco foram utilizados para o estudo de relações de escala e correlações entre os diversos parâmetros medidos. Algumas das mais significativas correlações são detalhadas, como a relação entre os parâmetros de escala de bojo e disco, que reforçam o cenário de evolução secular das galáxias disco. Finalmente, com o auxílio dos resultados cinemáticos da literatura, apresentamos, pela primeira vez, a relação Tully-Fisher para a amostra do GHASP, na banda Rc. / The spiral galaxies still challenge the theories that try to explain how the universe has turned into what we see today. In particular, in the context of the hierarchical structure formation, it is difficult to understand how galaxies can be so similar, obeying such strict scaling relations, in spite of their distinct evolutionary histories. In order to clarify some of these questions, the GHASP project has observed 203 galaxies in the H-alpha line, through Fabry-Perot interferometry, and has built a homogeneous and high quality database for kinematical studies in the local universe. In the present work, we seek to supplement the GHASP project results, presenting a photometric study for 173 of those galaxies in the Rc band. The data, taken with the 1.2m telescope at Haute-Provence Observatory or extracted from the SDSS database, was carefully treated with customized IRAF routines for the automation of most of the jobs. By fitting ellipses over the galaxies, calibrated surface brightness profiles and total magnitudes were obtained for galaxies in the sample. Then, galaxy light decomposition techniques were employed using an exponential model for the disk and a Sérsic function for the bulge. The results of the bulge-disk decomposition were used for the study of scaling relations and correlations among the several measured parameters. A few of the most significant correlations were described, such as the relation between bulge and disc scale lengths, reinforcing the galaxy-disk secular evolutionary scenario. Finally, with the aid of kinematic results from the literature, we present, for the first time, the Tully-Fisher relation for the GHASP sample, in the Rc-band.

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Orientador: Matthieu Tubino / Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Química / Made available in DSpace on 2018-08-19T12:43:39Z (GMT). No. of bitstreams: 1 Caland_LiliaBasiliode_D.pdf: 2271472 bytes, checksum: b5d42f422be0f6983fc7ae4d28db0182 (MD5) Previous issue date: 2011 / Resumo: O trabalho reportou dois métodos alternativos para determinação de íons metálicos (Na, K, Ca e Mg) em amostras de biodiesel. Tais métodos foram aplicados em amostras de biodiesel sintetisados a partir de diferentes óleos vegetais e, também, de gordura animal. Os métodos propostos utilizam, no tratamento da amostra, extração líquido-líquido em meio aquoso ácido, com aquecimento e extração assistida por ultrassom. A quantificação dos íons metálicos é feita por cromatografia de íons (Na, K, Ca e Mg) e por fotometria de chama (Na, K). Uma melhor separação cromatográfica dos íons Na, K, Ca e Mg foi obtida quando se empregou como eluente uma solução mista de ácido dipicolínico 1,7 mmol L com HNO3 2,5 mmol L. Para o método empregando cromatografia de íons, os limites de detecção (LD) e os limites de quantificação (LQ) foram respectivamente: 0,28 e 0,83 mg kg (Na); 0,38 e 1,13 mg kg (K); 0,41 e 1,22 mg kg (Ca); 0,29 e 0,86 mg kg (Mg). Os desvios padrão relativos dos valores encontrados foram menores do que 18,6 %. A exatidão do método foi avaliada através de teste de recuperação, com resultados entre 88,45 e 109,8 %, e por comparação dos dados obtidos por ICP OES. O teste t-Student e o teste¿F mostraram que ambos os métodos apresentaram resultados equivalentes em termos de exatidão e precisão. Na fotometria de chama, os valores de LD e LQ, foram respectivamente: 0,6 e 1,8 mg kg (Na); 0,4 e 1,4 mg kg (K). A recuperação obtida foi de 92,1 % para Na e de 103,6 % para K. Na comparação dos teores dos íons Na e K fornecidos pelo procedimento que usa fotometria de chama com aqueles provindos da cromatografia de íons, não foi observada diferença significativa entre os resultados, ao nível de confiança de 95%, tanto no que se refere à exatidão como à precisão. A simplicidade, exatidão, precisão e custo relativamente baixo dos métodos propostos sugerem que podem ser boas alternativas para a determinação dos íons metálicos (Na, K, Mg e Ca) em amostras de biodiesel / Abstract: In this work reports two alternative methods for the quantitation of metallic ions (Na, K, Mg e Ca) in biodiesel samples. The proposed methods were applied to biodiesel that were synthesized from different vegetable oils and also animal fat. The proposed method uses water extraction, heating and ultrasound. The quantitation of the ions was performed using ion chromatography (Na, K, Mg e Ca) and flame photometry (Na, K).The best chromatographic separation of the cations (Na, K, Ca e Mg) was observed when a solution containing dipicolinic acid (1.7 mmol L) plus nitric acid was used (2.5 mmol L). For the method with ion chromatography, the limits of detection (LOD) and of quantitation (LOQ) were respectively: 0.28 and 0.83 mg kg (Na); 0.38 and 1.13 mg kg (K); 0.41 and 1.22 mg kg (Ca); 0.29 and 0.86 mg kg (Mg). The relative standard deviations of the obtained values were smaller than 18.6 %. The accuracy was determined through recovery procedures, with presented results between 88.45 and 109.8 %, and also by comparison with the data obtained from ICP-OES. The Student.s t-test and the F-test showed that both methods presented equivalent results in with respect to accuracy and precision. In the case of flame photometry the LD and LQ values were respectively: 0.6 and 1.8 mg kg (Na); 0.4 and 1.4 mg kg (K). The observed recoveries were 92.1 % for Na and 103.6 % for K. In the comparison between the set containing the results obtained for Na and K with flame photometry with that came from ion chromatography, it was not observed significant difference at the 95% confidence level, both with respect to accuracy as well to precision. The simplicity, accuracy, precision and relative low cost of the proposed methods suggest that they are interesting alternatives for the quantitation of metallic ions (Na, K, Mg and Ca) in biodiesel samples / Doutorado / Quimica Analitica / Doutor em Ciências

We present new spatially resolved surface photometry in the far-ultraviolet (FUV) and near-ultraviolet (NUV) from images obtained by the Galaxy Evolution Explorer (GALEX) and IRAC1 (3.6 mu m) photometry from the Spitzer Survey of Stellar Structure in Galaxies (S(4)G). We analyze the radial surface brightness profiles mu(FUV), mu(NUV), and mu[3.6], as well as the radial profiles of (FUV - NUV), (NUV -[3.6]), and (FUV -[3.6]) colors in 1931 nearby galaxies (z < 0.01). The analysis of the 3.6 mu m surface brightness profiles also allows us to separate the bulge and disk components in a quasi-automatic way and to compare their light and color distribution with those predicted by the chemo-spectrophotometric models for the evolution of galaxy disks of Boissier & Prantzos. The exponential disk component is best isolated by setting an inner radial cutoff and an upper surface brightness limit in stellar mass surface density. The best-fitting models to the measured scale length and central surface brightness values yield distributions of spin and circular velocity within a factor of two of those obtained via direct kinematic measurements. We find that at a surface brightness fainter than mu([3.6]) = 20.89 mag arcsec(-2), or below 3 x 10(8) M-circle dot kpc(-2) in stellar mass surface density, the average specific star formation rate (sSFR) for star-forming and quiescent galaxies remains relatively flat with radius. However, a large fraction of GALEX Green Valley galaxies show a radial decrease in sSFR. This behavior suggests that an outside-in damping mechanism, possibly related to environmental effects, could be testimony of an early evolution of galaxies from the blue sequence of star-forming galaxies toward the red sequence of quiescent galaxies.

We calculated the fraction of ‘clumpy’ galaxies (fclumpy) for three samples of nearby galaxies. These samples include interacting galaxies with strong tidal features, collisional ring galaxies, and normal spiral galaxies. We define a ‘clumpy’ galaxy as a galaxy that has luminous star-forming regions contributing more than 8% of the total flux for the galaxy. We calculate fclumpy for 16 different wavelengths. We find that fclumpy is highest in the ultraviolet, Hα, and 24μm, while fclumpy is the lowest in optical and near-infrared wavelengths. We also see a significant increase in fclumpy for the interacting samples compared to the normal spirals.

This thesis deals with an unconventional possibility of measuring photometric values and the work is based on analysis of luminance made by commercially available digital photo camera. In the first part is represent an overview of current methods for measuring the photometry. You also can see the basic photometric values and required instrumentation needed to measure them. The focus of the work is concentrated on the description of the problems associated with setting the correct luminance of digital photography. It describes the dependency and correction procedures for calculating fixed luminance ratios of the individual images. The last part of this thesis is devoted to the possible use in practice, especially in the analysis of luminance of objects, luminaires and light sources. It also deals with an alternative description of luminaire and light sources to replace the luminous intensity curve etc.

The diploma thesis deals with a design of illuminating system for tandem-scanning confocal microscope using a high-power LEDs.