Dissertations / Theses on the topic 'Galaxy'
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Linke, Laila Maria [Verfasser]. "Testing models of galaxy formation and evolution with galaxy-galaxy-galaxy lensing / Laila Maria Linke." Bonn : Universitäts- und Landesbibliothek Bonn, 2021. http://d-nb.info/1235524469/34.
Full textHarker, Geraint John Alan. "Connecting galaxy formation and galaxy clustering." Thesis, Durham University, 2007. http://etheses.dur.ac.uk/2375/.
Full textSaghiha, Hananeh [Verfasser]. "Comparing galaxy-galaxy(-galaxy) lensing in semi-analytic models and observations to study galaxy evolution / Hananeh Saghiha." Bonn : Universitäts- und Landesbibliothek Bonn, 2017. http://d-nb.info/113070467X/34.
Full textDavoli, Guido. "Galaxy-galaxy strong lensing as a probe of the inner structure of galaxy clusters." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2017. http://amslaurea.unibo.it/13969/.
Full textBrimioulle, Fabrice. "Dark matter halo properties from galaxy-galaxy lensing." Diss., Ludwig-Maximilians-Universität München, 2013. http://nbn-resolving.de/urn:nbn:de:bvb:19-159994.
Full textThe scientific results over the past years have shown that the Universe is by far not only composed of baryonic matter. In fact the major energy content of 72% of the Universe appears to be represented by so-called dark energy, while even from the remaining components only about one fifth is of baryonic origin, whereas 80% have to be attributed to dark matter. Originally appearing in observations of spiral galaxy rotation curves, the need for dark matter has also been verified investigating elliptical galaxies and galaxy clusters. In fact, it appears that dark matter played a major role during structure formation in the early Universe. Shortly after the Big Bang, when the matter distribution was almost homogeneous, initially very small inhomogeneities in the matter distribution formed the seeds for the gravitational collapse of the matter structures. Numerical n-body simulations, for instance, clearly indicate that the presently observable evolutionary state and complexity of the matter structure in the Universe would not have been possible without dark matter, which significantly accelerated the structure collapse due to its gravitational interaction. As dark matter does not interact electromagnetically and therefore is non-luminous but only interacts gravitationally, the gravitational lens effect provides an excellent opportunity for its detection and estimation of its amount. Weak gravitational lensing is a technique that makes use of the random orientation of the intrinsic galaxy ellipticities and thus their uniform distribution. Gravitational tidal forces introduce a coherent distortion of the background object shapes, leading to a deviation from the uniform distribution which depends on the lens galaxy properties and therefore can be used to study them. This thesis describes the galaxy-galaxy lensing analysis of 89 deg^2 of optical data, observed within the CFHTLS-WIDE survey. In the framework of this thesis the data were used in order to create photometric redshift and galaxy shape catalogs. The complete galaxy sample consists of a total number of 5×10^6 lens galaxies within a redshift range of 0.05 < z_phot ≤ 1 and 1.7×10^6 corresponding source galaxies with redshifts of 0.05 < z_phot ≤ 2 and successfully extracted shapes. Assuming that the galaxy halos can be described by analytic profiles, the scaling relations with absolute luminosity for the galaxy masses, their mass-to-light ratios and the corresponding halo parameters have been extracted. Based on the obtained scaling relations, the average values for the corresponding halo parameters and the mean galaxy masses for a given luminosity were derived as a function of considered halo model, the galaxy SED and the local environment density. We obtain a total mass of M_total = 23.2+2.8−2.5 ×10^11 h{−1} M_⊙ for an average galaxy with chosen reference luminosity of L∗ = 1.6×10^10 h{−2} L_⊙. In contrast, the mean total masses for red galaxies of same luminosity exceed the value of the average galaxy about 130%, while the mass of a blue galaxy is about 65% below the value of an average fiducial galaxy. Investigating the influence of the environmental density on the galaxy properties we observe a significant increase of the total integrated masses with galaxy density, however the velocity dispersions are not affected. This indicates that the central galaxy matter density mostly depends on the galaxy luminosity but not on the environment. Simulations based on the extracted scientific results were built, verifying the robustness of the scientific results. They give a clear hint that multiple deflections on different lens galaxies have to be properly accounted for in order to avoid systematically biased results.
Goddard, Daniel Stephen. "Mapping galaxy properties with large-scale galaxy surveys." Thesis, University of Portsmouth, 2018. https://researchportal.port.ac.uk/portal/en/theses/mapping-galaxy-properties-with-largescale-galaxy-surveys(43eec926-30d1-44bc-8270-86222d389bff).html.
Full textAcreman, D. M. "Galaxy wakes." Thesis, University of Birmingham, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.403583.
Full textRychlík, Adam. "Casino Galaxy." Master's thesis, Vysoké učení technické v Brně. Fakulta stavební, 2017. http://www.nusl.cz/ntk/nusl-265370.
Full textWang, Pin-Wei. "Star formation rate and the assembly of galaxies in the early universe." Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4713/document.
Full textThe main purpose of this THESIS is to identify and study the population of high redshift galaxies in the redshift range (4.5 < z < 6.5). I use the near infrared data from the UltraVista survey conducted with the Vista telescope in combination with multi-wavelength data available in the COSMOS field and use The VIMOS Ultra Deep spectroscopic redshift survey (VUDS) as a control sample for the selection of high redshift candidates. I made a analysis leads me to select galaxies at z ≥ 4.5 using photometric redshifts computed from the full spectral energy distribution (SED) combined with well tuned magnitude limits based on the depth of the data in each band. At the end of this process I produce a unique catalogue of 2036 galaxies with 4.5 ≤ z ≤ 5.5 and 330 galaxies with 5.5 ≤ z ≤ 6.5, the largest and most complete catalogue of sources at these redshifts existing today. I find that the LF at z ∼ 5 is well fit by a Schechter function. At z ∼ 6 I find that the bright end might be more populated than expected from a Schechter function, in line with results from other authors, an indication that the mass assembly processes have evolved quickly in a short 0.5-1 Gyr timescale. Finally I integrate the luminosity functions to compute the luminosity density and derive the star formation rate density (SFRD) in 4.5 ≤ z ≤ 6.5. My results show a high SFRD comparable to the latest results derived from the HST data, with an improved accuracy linked to the better constraints at the bright end of the LF
Madgwick, Darren Stewart. "The 2dF galaxy redshift survey : galaxy spectra and cosmology." Thesis, University of Cambridge, 2002. https://www.repository.cam.ac.uk/handle/1810/251844.
Full textMartinet, Nicolas. "Galaxy clusters : a probe to galaxy evolution and cosmology." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066348/document.
Full textThis thesis presents some recent results concerning galaxy evolution and cosmology,based on the observation of galaxy clusters at optical wavelengths. We first introduce the main properties of galaxy clusters (Sect. 1.1) and how they can be used for cosmology within the standard cosmological model (Sect. 1.2). A large fraction of the presented results comes from the study of the DAFT/FADA galaxy cluster survey at redshifts 0.4 < z < 0.9 (Sect. 1.3). We divide our study in two parts according to the observable that is considered: galaxy luminosity or galaxy shape. The distribution of galaxy luminosities is called the galaxy luminosity function (GLF), which can be used to probe the evolution of cluster galaxies (Sect. 2.1). Computing the GLFs for a sub sample of 25 DAFT/FADA clusters, we find that faint blue star forming galaxies are quenched into red quiescent galaxies from high redshift until today. Comparing to the field shows that this transformation is more efficient in high density environments.We also study the fraction of baryons in galaxy groups and clusters (Sect. 2.2). Wefind that in groups, the stars contained in galaxies can reach masses of the same order as those of the intra-cluster gas, while in clusters they are usually negligible relatively to the gas. Taking both stars and gas into account we constrain the matter density parameter Galaxy shapes are distorted by foreground objects that bend light in their vicinity. This lensing signal can be exploited to measure the mass distribution of a foreground cluster. We review the basic theory of weak lensing and shear measurement (Sect. 3.1), and then apply it to a subsample of 16 DAFT/FADA clusters, with Subaru/SuprimeCam or CFHT/MegaCam imaging (Sect. 3.2). We estimate the masses of these clusters, and take advantage of the large fields of view of our images to detect filaments and structures in the cluster vicinity, observationally supporting the hierarchical scenario of cluster growth. Finally, we detect shear peaks in Euclid-like simulations, and use their statistics as a cosmological probe, similarly to cluster counts (Sect. 3.3). We forecast the cosmological constraints that this technique will achieve when applied to the Euclid space mission, and develop a tomographic analysis that adds information from redshifts. We conclude with a discussion of our perspectives on future studies in all the fieldsinvestigated in the present thesis
Kim, Jae Woo. "Galaxy clustering and galaxy clusters from the UKIDSS DXS." Thesis, Durham University, 2011. http://etheses.dur.ac.uk/3270/.
Full textZheng, Zheng. "Constraining galaxy bias and cosmology using galaxy clustering data." Connect to this title online, 2004. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1092257217.
Full textTitle from first page of PDF file. Document formatted into pages; contains xix, 302 p. : ill. (some col.). Advisor: David H. Weinberg, Department of Astronomy. Includes bibliographical references (p. 291-302).
Cool, Richard Jacob. "Empirical Measurements of Massive Galaxy and Active Galaxy Evolution." Diss., The University of Arizona, 2008. http://hdl.handle.net/10150/195540.
Full textPark, Y., E. Krause, S. Dodelson, B. Jain, A. Amara, M. R. Becker, S. L. Bridle, et al. "Joint analysis of galaxy-galaxy lensing and galaxy clustering: Methodology and forecasts for Dark Energy Survey." AMER PHYSICAL SOC, 2016. http://hdl.handle.net/10150/621963.
Full textMachado, murtinheiras martins Andre. "Statistical analysis of large scale surveys for constraining the Galaxy evolution." Thesis, Besançon, 2014. http://www.theses.fr/2014BESA2026/document.
Full textThe formation and evolution of the thick disc of the Milky Way remain controversial. We made use of a population synthesis model of the Galaxy, the Besançon Galaxy Model (Robin et al. 2003), which can be used for data interpretation, study the Galactic structure and test different scenarios of Galaxy formation and evolution. We examined these questions by studying the shape and the metallicity distribution of the thin and thick disc using the population synthesis approach. We imposed on simulations observational errors and biases to make them directly comparable to observations. We corrected magnitudes and colors of stars, from the simulation, using an extinction model. The available extinction models do not always reproduce the exact quantity of extinction along the line of sight. A code to correct the distribution of extinction in distance along these lines have been developed and the corrected extinctions have been applied on model simulations. We studied the shape of the thin disc using photometric data at low latitudes from the SDSS-SEGUE survey. We compared qualitatively and quantitatively observations and simulations and try to constrain the Initial Mass Function. Using the spectroscopic survey SEGUE we selected Main Sequence Turnoff (MSTO) stars (Cheng et al 2012) and K giants to study the metallicity distribution of the thin and thick discs. We computed a distance for each star from the relation between effective temperatures and absolute magnitudes for the observed and simulated catalogs. These two catalogues have the same biases in distances, therefore are comparable. We developed a tool based on a MCMC-ABC method to determine the metallicity distribution and study the correlations between the fitted parameters. We confirmed a radial metallicity gradient of -0.079 ± 0.015 dex kpc−1 for the thin disc. We obtained a solar neighborhood metallicity of the thick disc of -0.47 ± 0.03 dex similar to previous studies and the thick disc shows no gradient but the data are compatible with an inner positive gradient followed by a outer negative one. Furthermore, we have applied the developed tools to the Gaia-ESO spectroscopic survey and computed the metallicity distribution of F/G/K stars in the thin and thick disc assuming a two epoch formation for the thick disc of the Milky Way. We obtained a local metallicity in the thick disc of -0.23 ± 0.04 dex slightly higher than the one obtained with SEGUE but in agreement with Adibekyan et al. (2013) and a radial metallicity gradient for the thick disc in agreement with our previous analysis of SEGUE data and the literature. The local metallicity is in fair agreement with literature at the 3σ level but because the GES data is an internal release under testing further analysis with more data and better calibrations have to be done. The existence of a flat gradient in the thick disc can be a consequence of an early formation from a highly turbulent homogeneous well mixed gas, unless it has suffered heavy radial mixing later on
Kwan, J., C. Sánchez, J. Clampitt, J. Blazek, M. Crocce, B. Jain, J. Zuntz, et al. "Cosmology from large-scale galaxy clustering and galaxy–galaxy lensing with Dark Energy Survey Science Verification data." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623270.
Full textMerson, Alexander Ian. "Mock galaxy catalogues and their application to future galaxy surveys." Thesis, Durham University, 2013. http://etheses.dur.ac.uk/6382/.
Full textThomas, Nicole. "Galaxy Clustering as a Probe for Galaxy Evolution in Simulations." University of the Western Cape, 2017. http://hdl.handle.net/11394/6206.
Full textStudying clustering on small scales (<10Mpc) over a large span of red- shifts allows us to connect galaxies to underlying cosmic large-scale structure, and thereby provide constraints on the physical processes that drive galaxy evolution. Relatedly, studying the relative bias of galaxies and their halo occupancy quanti es how the underlying dark matter distribution is traced by baryons in galaxies. Comparing model predictions to current and future multi-wavelength galaxy surveys, en- ables a greater understanding of how galaxy formation processes impact the relationship between galaxies and dark matter
Braglia, Filiberto Giorgio. "Study of optical properties and galaxy populations of galaxy clusters." Diss., kostenfrei, 2008. http://edoc.ub.uni-muenchen.de/9179/.
Full textWijesinghe, Dinuka. "Galaxy star formation rates and their relation to galaxy environments." Thesis, The University of Sydney, 2012. https://hdl.handle.net/2123/28926.
Full textHau, George Kin Tak. "Elliptical galaxy cores." Thesis, University of Cambridge, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.624785.
Full textBocquet, Sebastian. "Galaxy cluster cosmology." Diss., Ludwig-Maximilians-Universität München, 2015. http://nbn-resolving.de/urn:nbn:de:bvb:19-183812.
Full textKennedy, Rebecca. "Unravelling galaxy components." Thesis, University of Nottingham, 2017. http://eprints.nottingham.ac.uk/44091/.
Full textBonamigo, Mario. "Triaxial galaxy clusters." Thesis, Aix-Marseille, 2016. http://www.theses.fr/2016AIXM4717/document.
Full textIt is well established both theoretically and observationally that galaxy clusters are not spherical objects and that they are much better approximated as triaxial objects. This thesis focusses on the three dimencional shape of galaxy clusters. The originality of my approach is to tackle the problem both theoretically and observationally. First, I have measured the shape of dark matter haloes in the Millenium XXL and Sbarbine simulations, providing predictions for dark matter halo shape over 5 order in magnitude in mass. Then, I have developed an algorithm aimed at fitting simultaneously lensing and X-ray data in order to constrain a triaxial mass distribution. The algorithm is tested and characterized on mock data sets. It is found to be able to recover the input parameters. Finally, I present the X-ray analysis of galaxy cluster Abell 1703, which will be combined with the existing lensing analysis in order to investigate its shape
Steele, Oliver. "Galaxy spectral analysis in the era of large-scale galaxy surveys." Thesis, University of Portsmouth, 2015. https://researchportal.port.ac.uk/portal/en/theses/galaxy-spectral-analysis-in-the-era-of-largescale-galaxy-surveys(6631e476-60ec-4de3-a536-d8a9e1f8cbc4).html.
Full textZenteno, Alfredo. "Galaxy populations in galaxy clusters selected by the Sunyaev-Zeldovich Effect." Diss., Ludwig-Maximilians-Universität München, 2014. http://nbn-resolving.de/urn:nbn:de:bvb:19-170507.
Full textImpey, C. D., and G. D. Bothun. "MALIN: A Quiescent Disk Galaxy|MALIN 1: A Quiescent Disk Galaxy." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623912.
Full textLONI, ALESSANDRO. "The low HI-mass galaxy population in the Fornax galaxy cluster." Doctoral thesis, Università degli Studi di Cagliari, 2022. http://hdl.handle.net/11584/327519.
Full textSoumagnac, M. T. "Tipping scales in galaxy surveys : star/galaxy separation and scale-dependent bias." Thesis, University College London (University of London), 2015. http://discovery.ucl.ac.uk/1460581/.
Full textMajewski, Steven R., Ricardo P. Schiavon, Peter M. Frinchaboy, Carlos Allende Prieto, Robert Barkhouser, Dmitry Bizyaev, Basil Blank, et al. "The Apache Point Observatory Galactic Evolution Experiment (APOGEE)." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625493.
Full textHoffmann, Kai Delf. "Cosmology with galaxy clustering." Doctoral thesis, Universitat Autònoma de Barcelona, 2015. http://hdl.handle.net/10803/297700.
Full textFor constraining cosmological models via the growth of large-scale matter fluctuations it is important to understand how the observed galaxies trace the full matter density field. The relation between the density fields of matter and galaxies is often approximated by a second- order expansion of a so-called bias function. The freedom of the parameters in the bias function weakens cosmological constraints from observations. In this thesis we study two methods for determining the bias parameters independently from the growth. Our analysis is based on the matter field from the large MICE Grand Challenge simulation. Haloes, identified in this simulation, are associated with galaxies. The first method is to measure the bias parameters directly from third-order statistics of the halo and matter distributions. The second method is to predict them from the abundance of haloes as a function of halo mass (hereafter referred to as mass function). Our bias estimations from third-order statistics are based on three-point auto- and cross- correlations of halo and matter density fields in three dimensional configuration space. Using three-point auto-correlations and a local quadratic bias model we find a ∼ 20% overestimation of the linear bias parameter with respect to the reference from two-point correlations. This deviation can originate from ignoring non-local and higher-order contributions to the bias function, as well as from systematics in the measurements. The effect of such inaccuracies in the bias estimations on growth measurements are comparable with errors in our measurements, coming from sampling variance and noise. We also present a new method for measuring the growth which does not require a model for the dark matter three-point correlation. Results from both approaches are in good agreement with predictions. By combining three-point auto- and cross-correlations one can either measure the linear bias without being affected by quadratic (local or non-local) terms in the bias functions or one can isolate such terms and compare them to predictions. Our linear bias measurements from such combinations are in very good agreement with the reference linear bias. The comparison of the non-local contributions with predictions reveals a strong scale dependence of the measurements with significant deviations from the predictions, even at very large scales. Our second approach for obtaining the bias parameters are predictions derived from the mass function via the peak-background split approach. We find significant 5−10% deviations between these predictions and the reference from two-point clustering. These deviations can only partly be explained with systematics affecting the bias predictions, coming from the halo mass function binning, the mass function error estimation and the mass function parameterisation from which the bias predictions are derived. Studying the mass function we find unifying relations between different mass function parameterisation. Furthermore, we find that the standard Jack-Knife method overestimates the mass function error covariance in the low mass range. We explain these deviations and present a new improved covariance estimator.
Croton, Darren. "Galaxy Formation and Evolution." Diss., lmu, 2005. http://nbn-resolving.de/urn:nbn:de:bvb:19-44059.
Full textRimes, Christopher D. "Modelling the galaxy population." Thesis, University of Edinburgh, 2003. http://hdl.handle.net/1842/27270.
Full textBielby, Richard. "Galaxy clustering and feedback." Thesis, Durham University, 2008. http://etheses.dur.ac.uk/2344/.
Full textEke, Vincent R. "Cosmology with galaxy clusters." Thesis, Durham University, 1996. http://etheses.dur.ac.uk/5195/.
Full textMaddox, Stephen John. "The APM galaxy survey." Thesis, University of Cambridge, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.304353.
Full textRuggiero, Rafael. "Galaxy Evolution in Clusters." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-14022019-140755/.
Full textNesta tese, nós visamos a contribuir para o entendimento do fenômeno da evolução de galáxias no ambiente de aglomerados de galáxias usando a metodologia de simulações numéricas. Para isso, desenvolvemos modelos hidrodinâmicos nos quais galáxias idealizadas ricas em gás movem-se em meio ao gás difuso de aglomerados de galáxias idealizados, permitindo um estudo detalhado e controlado da evolução destas galáxias neste ambiente extremo. O principal código usado em nossas simulações é o RAMSES, e nossos resultados tratam das mudanças em composição do gás, taxa de formação estelar, luminosidade e cor de galáxias caindo em aglomerados. Adicionalmente a processos acontecendo dentro das próprias galáxias, nós também descrevemos a dinâmica do gás que é varrido dessas galáxias com resolução sem precedentes para simulações dessa natureza (122 pc em uma caixa incluindo um aglomerado de 1e14 Msun inteiro), encontrando que aglomerados de gás molecular são formados nas caudas de galáxias que passaram por varrimento de gás por pressão de arraste, aglomerados estes que procedem a viver em isolamento em meio ao gás difuso de um aglomerado de galáxias por até 300 Myr. Esses aglomerados moleculares possivelmente representam uma nova classe de objetos; objetos similares foram previamente observados tanto em aglomerados quanto em grupos de galáxias, mas um tratamento compreensivo deles não foi apresentado até agora. Nós adicionalmente criamos um modelo hidrodinâmico para o sistema multi-aglomerado A901/2, e correlacionamos as condições do gás nesse modelo com a localização de uma amostra de galáxias jellyfish nesse sistema; isso nos permitiu inferir um possível mecanismo para a geração de morfologias jellyfish em colisões de aglomerados de galáxias em geral.
Curtis, Lake Emma. "Galaxy evolution with FMOS." Thesis, University of Oxford, 2010. http://ora.ox.ac.uk/objects/uuid:866b8ba5-5353-43a7-9898-a4b767ab0f6d.
Full textBrimioulle, Fabrice [Verfasser], and Ralf [Akademischer Betreuer] Bender. "Dark matter halo properties from galaxy-galaxy lensing / Fabrice Brimioulle. Betreuer: Ralf Bender." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2013. http://d-nb.info/1038152550/34.
Full textLaporte, Chervin F. P., Facundo A. Gómez, Gurtina Besla, Kathryn V. Johnston, and Nicolas Garavito-Camargo. "Response of the Milky Way's disc to the Large Magellanic Cloud in a first infall scenario." OXFORD UNIV PRESS, 2018. http://hdl.handle.net/10150/626276.
Full textHayes, Christian R., Steven R. Majewski, Matthew Shetrone, Emma Fernández-Alvar, Carlos Allende Prieto, William J. Schuster, Leticia Carigi, et al. "Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626539.
Full textCzekaj, Maria A. "Galaxy evolution: A new version of the Besançon Galaxy Model constrained with Tycho data." Doctoral thesis, Universitat de Barcelona, 2012. http://hdl.handle.net/10803/123978.
Full textLa misión Gaia (ESA, 2013) revolucionará el conocimiento sobre el origen y la evolución de nuestra Galaxia. Una óptima explotación científica de sus datos requiere disponer de modelos que permitan contrastar hipótesis y escenarios sobre estos procesos de formación. En esta tesis hemos optimizado el modelo de síntesis de poblaciones estelares de Besançon, ampliamente utilizado por la comunidad internacional, centrándonos en la componente del disco delgado. Hemos diseñado, desarrollado, implementado y testeado una nueva estructura de generación de las estrellas que permite encontrar la mejor combinación de función inicial de masa (IMF) y ritmo de formación estelar (SFR) que ajusta a las observaciones. El código permite imponer la autoconsistencia dinámica, recalculando el potencial galáctico para cada nuevo escenario de evolución. También, por primera vez, se generan sistemas binarios bajo esta consistencia dinámica, marcada por la función de luminosidad observada en el entorno solar. Esta, junto con el catálogo Tycho, han sido los dos ingredientes observacionales clave para el ajuste entre modelo y observación. También, por primera vez, hemos conseguido un ajuste aceptable a los recuentos estelares de todo el cielo hasta V=11. Se han evaluado con rigor los efectos en los recuentos estelares derivados del uso de los modelos de atmosfera, de evolución estelar y de extinción interestelar así como de parámetros tan críticos como la masa dinámica del sistema galáctico. El ajuste de estos ingredientes usando el catálogo Tycho nos ha permitido confirmar, de una vez por todas, que la SFR en el disco galáctico no ha sido constante sino decreciente desde los inicios de la formación de esta estructura. En conclusión, esta tesis proporciona un nuevo código, optimizado y flexible en el uso de los ingredientes básicos, en el que se ha realizado una rigurosa evaluación y actualización de los ingredientes que lo componen.
Leuzzi, Laura. "Characterization of convolutional neural networks for the identification of galaxy-galaxy strong lensing events." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2021. http://amslaurea.unibo.it/22516/.
Full textThomas, Daniel. "Chemical evolution and galaxy formation." Diss., lmu, 2000. http://nbn-resolving.de/urn:nbn:de:bvb:19-4637.
Full textSawala, Till. "Simulations of Dwarf Galaxy Formation." Diss., lmu, 2011. http://nbn-resolving.de/urn:nbn:de:bvb:19-132531.
Full textKampakoglou, Marios. "Analytical models of galaxy formation." Thesis, University of Oxford, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.487269.
Full textBothwell, Matthew Stuart. "Galaxy evolution : near and far." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/265602.
Full textMoustakas, John. "Spectral Diagnostics of Galaxy Evolution." Diss., The University of Arizona, 2006. http://hdl.handle.net/10150/305142.
Full textThomas, Peter Andrew. "Cooling flows and galaxy formation." Thesis, University of Cambridge, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.329135.
Full text