Auswahl der wissenschaftlichen Literatur zum Thema „Photométrie de masse“
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Zeitschriftenartikel zum Thema "Photométrie de masse"
Samadi, Réza. „Microlensing photométrique et détermination des masses stellaires“. Comptes Rendus de l'Académie des Sciences - Series IIB - Mechanics-Physics-Astronomy 326, Nr. 12 (Januar 1998): 939–44. http://dx.doi.org/10.1016/s1251-8069(99)80052-0.
Der volle Inhalt der QuelleDissertationen zum Thema "Photométrie de masse"
Castel, Jérôme. „Developpements en spectrométrie de masse structurale pour la caratérisation de protéines d'intérêt thérapeutique“. Electronic Thesis or Diss., Strasbourg, 2024. http://www.theses.fr/2024STRAF003.
Der volle Inhalt der QuelleThis PhD work focuses on methodological developments in structural mass spectrometry (MS), especially by hydrogen/deuterium exchange coupled to MS (HDX-MS), by native MS coupled or not to ion mobility (IM-MS) and more recently mass photometry, for the characterization of various proteins of therapeutic interest. In particular, this work has demonstrated the contribution of a combination of structural MS approaches to the in-depth characterization of membrane proteins, from the analysis of intact proteins to their conformational dynamics. The implementation of new analytical strategies in IM-MS and HDX-MS has also been evaluated for the detailed structural characterization of therapeutic antibodies. Finally, the benefits of HDX-MS approach was illustrated for the conformational and dynamic screening of ligands in the context of the study of protein/ligand interactions involving nuclear receptors
Barret, Didier. „Modélisation de la réponse spectrale du télescope spatial SIGMA. Etude des propriétés spectrales des binaires X de faible masse dans la gamme d'énergie 35-500 keV : [thèse en partie soutenue sur un ensemble de travaux]“. Toulouse 3, 1993. http://www.theses.fr/1993TOU30260.
Der volle Inhalt der QuelleLamareille, Fabrice. „Évolution cosmologique des propriétés physiques des galaxies“. Phd thesis, Université Paul Sabatier - Toulouse III, 2006. http://tel.archives-ouvertes.fr/tel-00090655.
Der volle Inhalt der QuelleCe travail de thèse porte préférentiellement sur l'étude des relations masse-métallicité ou luminosité-métallicité qui permettent d'établir un lien entre les deux processus majeurs responsables de l'évolution des galaxies: l'assemblage de la masse stellaire (formation d'étoiles ou fusion de galaxies) et l'enrichissement chimique du milieu interstellaire par les générations d'étoiles successives. Nous montrons que la forme de cette relation est un très bon test des modèles de formation et d'évolution des galaxies. Nous étudions ensuite la relation luminosité-métallicité de référence obtenue à partir du relevé 2dFGRS dans l'Univers local. Puis nous étudions l'évolution en fonction de l'âge de l'univers de la relation luminosité-métallicité à l'aide d'un petit échantillon (LCL05), puis de la relation masse-métallicité à l'aide du grand relevé VVDS. Plusieurs résultats obtenus avec ces différents échantillons sont des indices en faveur du modèle hiérarchique: les galaxies les plus massives se formeraient par fusion progressive de galaxies plus petites.
Les propriétés physiques d'un grand nombre de galaxies sont estimées à l'aide d'outils d'analyse automatiques spécifiquement développés, ou adaptés à nos besoins, durant cette thèse. Comme résultats annexes, de nouvelles calibrations de la classification spectrale ou du taux de formation d'étoiles des galaxies sont obtenues à partir des grands relevés de l'univers local (respectivement 2dFGRS et SDSS). Ce travail offre de nombreuses perspectives de par le nombre et la diversité des données disponibles.
Moutard, Thibaud. „Redshifts photométriques et paramètres physiques des galaxies dans les sondages à grande échelle : contraintes sur l'évolution des galaxies massives“. Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4782.
Der volle Inhalt der QuelleThis thesis presents the measurement of the photometric redshifts and physical parameters in the framework of large scale surveys, and their constraint on galaxy evolution. The photometric redshift measurement allows us to study the entire photometric sample. For this reason, the weak lensing signal measurement used in the Euclid mission as a primary cosmological probe will rely on photometric redshift measurements. However, the method is strongly affected by the quality of the photometry. In particular, I show in this thesis how the photometric calibration impacts the photometric redshift precison, in order to constrain the photometric strategy to use in the Euclid mission.Aiming to take into account for observationnal problems, the analysis is done with observationnal data whose photometric configuration is close to the expected Euclid one. These data combine new near-infrared observations conduected to cover the VIPERS spectroscopic survey and the CFHTLS photometry.Using the conclusions of this analysis, I have producted the new photometric catalogue for VIPERS and the associated photometric redshift calalogue.Finally, I used the same photometry to compute the stellar masses of 760,000 galaxies covering 22 square degrees at the limiting magnitude Ks(AB) < 22. This enabled me to study the evolution of the stellar mass function between redshifts z= 0.2 and z = 1.5. We have then shown that the star formation of galaxies with stellar masses around log(M/Msol) = 10.66 is stopped in 2-4 Gyr, while in quiescent low-mass (log(M/Msol) < 9.5) galaxies, the star formation has been stopped 5-10 times faster (approximatelly in 0.4 Gyr)
Kronborg, Taia. „L' effet de lentilles gravitationnelles sur les supernovae du SNLS“. Paris 6, 2009. https://tel.archives-ouvertes.fr/tel-00562370.
Der volle Inhalt der QuelleType Ia supernovae have become an essential tool of modern observational cosmology. By studying the distance-redshift relation of a large number of supernovae, the nature of dark energy can be unveiled. Distances to Type Ia SNe are however affected by gravitational lensing which can induce systematic effects in the measurement of cosmology. The majority of the supernovae is slightly demagnified whereas a small fraction is significantly magnified due to the mass distribution along the line of sight. This causes naturally an additional dispersion in the observed magnitudes. There are two different ways to estimate the magnification of a supernova. A first method consists in comparing the supernova luminosity, which is measured to about 15% precision, to the mean SN luminosity at the same redshift. Another estimate can be obtained from predicting the magnification induced by the foreground matter density modeled from the measurements of the luminosity of the galaxies with an initial prior on the mass-luminosity relation of the galaxies A correlation between these 2 estimates will make it possible to tune the initially used mass-luminosity relation resulting in an independent measurement of the dark matter clustering based on the luminosity of SNe Ia. Evidently, this measurement depends crucially on the detection of this correlation also referred to as the lensing signal. This thesis is dedicated to the measurement of the lensing signal in the SNLS 3-year sample
Kronborg, Taia. „L'effet de lentilles gravitationnelles sur les supernovae du SNLS“. Phd thesis, Université Pierre et Marie Curie - Paris VI, 2009. http://tel.archives-ouvertes.fr/tel-00562370.
Der volle Inhalt der QuelleLachapelle, François-René. „Caractérisation photométrique et spectroscopique de compagnons sous-stellaires de faible masse autour d'étoiles de la région de formation Upper Scorpius“. Thèse, 2013. http://hdl.handle.net/1866/10721.
Der volle Inhalt der QuelleFollowing the discovery of about 2000 brown dwarfs over the past two decades, we begin to understand the physics of these objects of mass intermediate between stellar and planetary masses. Nevertheless, the atmosphere and evolution models for these low-mass objects are still struggling to reproduce their characteristics at young ages. This work presents the characterization of four sub-stellar mass (8-30 MJup) companions orbiting at large separation (300-900 AU) around young stars (5 Myr) in the Upper Scorpius formation region. New spectra (0,9-2,5 um) and new photometric measurements (YJHKsL') are presented and analyzed in order to determine the mass, effective temperature, luminosity and surface gravity of these companions, while assessing the fidelity with which the synthetic spectra from two recent atmosphere models reproduce the observed spectra.
Giammichele, Noemi. „Analyse des paramètres atmosphériques des étoiles naines blanches dans le voisinage solaire“. Thèse, 2010. http://hdl.handle.net/1866/4871.
Der volle Inhalt der QuelleWe present improved atmospheric parameters of nearby white dwarfs lying within 20 pc of the Sun. The aim of the current study is to obtain the best statistical model of the least-biased sample of the white dwarf population. A homogeneous analysis of the local population is performed combining detailed spectroscopic and photometric analyses based on improved model atmosphere calculations for various spectral types including DA, DB, DQ, and DZ stars. The spectroscopic technique is applied to all stars in our sample for which optical spectra are available. Photometric energy distributions, when available, are also combined to trigonometric parallax measurements to derive effective temperatures, stellar radii, as well as atmospheric compositions. A revised catalog of white dwarfs in the solar neighborhood is presented. We provide for the first time a comprehensive analysis of the mass distribution and the chemical distribution of white dwarf stars in a volume-limited sample.