Gotowe bibliografie tematyczne / Structure and evolution of the Galaxy

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Gotowa bibliografia na temat „Structure and evolution of the Galaxy”

Autor: Grafiati

Data publikacji: 8 czerwca 2024

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Artykuły w czasopismach na temat "Structure and evolution of the Galaxy"

White, Simon. "The influence of halo evolution on galaxy structure." Proceedings of the International Astronomical Union 10, H16 (2012): 371. http://dx.doi.org/10.1017/s1743921314011430.

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AbstractIf Einstein-Newton gravity holds on galactic and larger scales, then current observations demonstrate that the stars and interstellar gas of a typical bright galaxy account for only a few percent of its total nonlinear mass. Dark matter makes up the rest and cannot be faint stars or any other baryonic form because it was already present and decoupled from the radiation plasma at z = 1000, long before any nonlinear object formed. The weak gravito-sonic waves so precisely measured by CMB observations are detected again at z = 4 as order unity fluctuations in intergalactic matter. These subsequently collapse to form today's galaxy/halo systems, whose mean mass profiles can be accurately determined through gravitational lensing. High-resolution simulations link the observed dark matter structures seen at all these epochs, demonstrating that they are consistent and providing detailed predictions for all aspects of halo structure and growth. Requiring consistency with the abundance and clustering of real galaxies strongly constrains the galaxy-halo relation, both today and at high redshift. This results in detailed predictions for galaxy assembly histories and for the gravitational arena in which galaxies live. Dark halos are not expected to be passive or symmetric but to have a rich and continually evolving structure which will drive evolution in the central galaxy over its full life, exciting warps, spiral patterns and tidal arms, thickening disks, producing rings, bars and bulges. Their growth is closely related to the provision of new gas for galaxy building.

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Yee, H. K. C., M. J. Sawicki, R. G. Carlberg, et al. "The CNOC2 Field Galaxy Redshipt Survey." Highlights of Astronomy 11, no. 1 (1998): 460–63. http://dx.doi.org/10.1017/s153929960002178x.

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Fundamental to our understanding of the universe is the evolution of structures, from galaxies to clusters of galaxies to large-scale sheets and filaments of galaxies and voids. The investigation of the evolution of large-scale structure not only provides us with the key test of theories of structure formation, but also allows us to measure fundamental cosmological parameters. The CNOC2 (Canadian Network for Observational Cosmology) Field Galaxy Redshift Survey is the first large redshift survey of faint galaxies carried out with the explicit goal of investigating the evolution of large scale structure. This survey also provides the largest redshift and photometric data set currently available for the study of galaxy population and evolution at the moderate redshift range between 0.1 and 0.6. In this paper we describe the scope and technique of the survey, its status, and some preliminary results.

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Maartens, Roy, José Fonseca, Stefano Camera, Sheean Jolicoeur, Jan-Albert Viljoen, and Chris Clarkson. "Magnification and evolution biases in large-scale structure surveys." Journal of Cosmology and Astroparticle Physics 2021, no. 12 (2021): 009. http://dx.doi.org/10.1088/1475-7516/2021/12/009.

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Abstract Measurements of galaxy clustering in upcoming surveys such as those planned for the Euclid and Roman satellites, and the SKA Observatory, will be sensitive to distortions from lensing magnification and Doppler effects, beyond the standard redshift-space distortions. The amplitude of these contributions depends sensitively on magnification bias and evolution bias in the galaxy number density. Magnification bias quantifies the change in the observed number of galaxies gained or lost by lensing magnification, while evolution bias quantifies the physical change in the galaxy number density relative to the conserved case. These biases are given by derivatives of the number density, and consequently are very sensitive to the form of the luminosity function. We give a careful derivation of the magnification and evolution biases, clarifying a number of results in the literature. We then examine the biases for a variety of surveys, encompassing galaxy surveys and line intensity mapping at radio and optical/near-infrared wavelengths.

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Nagai, Daisuke, Monique Arnaud, Sarthak Dasadia, Michael McDonald, Ikuyuki Mitsuishi, and Andrea Morandi. "Cluster Physics & Evolution." Proceedings of the International Astronomical Union 11, A29B (2015): 70–78. http://dx.doi.org/10.1017/s1743921316004543.

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AbstractRecent advances in X-ray and microwave observations have provided unprecedented insights into the structure and evolution of the hot X-ray emitting plasma from their cores to the virialization region in outskirts of galaxy clusters. Recent Sunyaev-Zel'dovich (SZ) surveys (ACT, Planck, SPT) have provided new cluster catalogs, significantly expanding coverage of the mass-redshift plane, whileChandraandXMM-NewtonX-ray follow-up programs have improved our understanding of cluster physics and evolution as well as the surveys themselves. However, the current cluster-based cosmological constraints are still limited by uncertainties in cluster astrophysics. In order to exploit the statistical power of the current and upcoming X-ray and microwave cluster surveys, it is critical to improve our understanding of the structure and evolution of the hot X-ray emitting intracluster medium (ICM). In this session, we discussed recent advances in observations and simulations of galaxy clusters, with highlights on (i) the evolution of ICM profiles and scaling relations, (ii) physical processes operating in the outskirts of galaxy clusters, and (iii) impact of mergers on the ICM structure in groups and clusters.

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Conselice, Christopher J. "The Evolution of Galaxy Structure Over Cosmic Time." Annual Review of Astronomy and Astrophysics 52, no. 1 (2014): 291–337. http://dx.doi.org/10.1146/annurev-astro-081913-040037.

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Gilmore, Gerard, and Rosemary F. G. Wyse. "Structure and Evolution of the Milky Way Galaxy." International Astronomical Union Colloquium 111 (1989): 83–102. http://dx.doi.org/10.1017/s0252921100011465.

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AbstractThe combination of chemical abundance, kinematic, and age data for stars near the sun provides important information about the early evolution of the Galaxy. We review available data, with some new analysis, to show that the sum of all available information strongly suggests that the extreme population II subdwarf system formed during a period of rapid collapse of the proto-Galaxy. This subdwarf system now forms a flattened, pressure-supported distribution, with axial ratio ∼2:1. The thick disk formed subsequent to the subdwarf system. At least the metal-poor tail of the thick disk is comparable in age to the globular cluster system. The thick disk is probably kinematically discrete from the Galactic old disk, though the data remain inadequate for robust conclusions.

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Robin, A. C., C. Reylé, and D. Marshall. "Modelling the Galaxy from survey data." Proceedings of the International Astronomical Union 3, S248 (2007): 443–49. http://dx.doi.org/10.1017/s1743921308019789.

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AbstractRecent optical and near-infrared surveys have considerably improved our knowledge of galactic structure and galactic evolution. Two ways can be used to infer this knowledge from datasets: either inversing the data to get parameters describing the Galaxy, or using a synthetic approaches to test scenarios of formation and theoretical models for star and galaxy formation and evolution, both approaches being complementary. Using the synthetic approach the Besancon Galaxy model allows to test scenarios for the structure and evolution of the Galaxy by comparing simulations with the survey data. Examples are given using the 2MASS survey. Future uses of astrometric survey data are shown to be able to efficiently constrain the kinematics and dynamics of the Galaxy.

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Mazzei, P., A. Marino, R. Rampazzo, H. Plana, M. Rosado, and L. Arias. "Galaxy evolution in groups." Astronomy & Astrophysics 610 (February 2018): A8. http://dx.doi.org/10.1051/0004-6361/201731182.

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Context. Local Group (LG) analogs (LGAs) are galaxy associations dominated by a few bright spirals reminiscent of the LG. The NGC 3447/NGC 3447A system is a member of the LGG 225 group, a nearby LGA. This system is considered a physical pair composed of an intermediate-luminosity late-type spiral, NGC 3447 itself, and an irregular companion, NGC 3447A, linked by a faint, short filament of matter. A ring-like structure in the NGC 3447 outskirts has been emphasised by Galaxy Evolution Explorer (GALEX) observations. Aims. This work aims to contribute to the study of galaxy evolution in low-density environments, a favourable habitat to highly effective encounters, shedding light on the evolution of the NGC 3447/NGC 3447A system. Methods. We performed a multi-λ analysis of the surface photometry of this system to derive its spectral energy distribution and structural properties using ultraviolet (UV), Swift UVOT, and optical Sloan Digital Sky Survey (SDSS) images complemented with available far-IR observations. We also characterised the velocity field of the pair using two-dimensional Hα kinematical observations of the system obtained with PUMA Fabry-Perot interferometer at the 2.1 m telescope of San Pedro Mártir (Mexico). All these data are used to constrain smooth particle hydrodynamic simulations with chemo-photometric implementation to shed light on the evolution of this system. Results. The luminosity profiles, from UV to optical wavelengths, are all consistent with the presence of a disc extending and including NGC 3447A. The overall velocity field does not emphasise any significant rotation pattern, rather a small velocity gradient between NGC 3447 and NGC 3447A. Our simulation, detached from a large grid explored to best-fit the global properties of the system, suggests that this arises from an encounter between two halos of equal mass. Conclusions. NGC 3447 and NGC 3447A belong to the same halo, NGC 3447A being a substructure of the same disk including NGC 3447. The halo gravitational instability, enhanced by the encounter, fuels a long-lived instability in this dark-matter-dominated disk, driving the observed morphology. The NGC 3447/NGC 3447A system may warn of a new class of “false pairs” and the potential danger of a misunderstanding of such objects in pair surveys that could produce a severe underestimate of the total mass of a system.

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Linke, Laila, Patrick Simon, Peter Schneider, et al. "KiDS+VIKING+GAMA: Testing semi-analytic models of galaxy evolution with galaxy–galaxy–galaxy lensing." Astronomy & Astrophysics 640 (August 2020): A59. http://dx.doi.org/10.1051/0004-6361/202038355.

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Context. Several semi-analytic models (SAMs) try to explain how galaxies form, evolve, and interact inside the dark matter large-scale structure. These SAMs can be tested by comparing their predictions for galaxy–galaxy–galaxy lensing (G3L), which is weak gravitational lensing around galaxy pairs, with observations. Aims. We evaluate the SAMs by Henriques et al. (2015, MNRAS, 451, 2663, hereafter H15) and by Lagos et al. (2012, MNRAS, 426, 2142, hereafter L12), which were implemented in the Millennium Run, by comparing their predictions for G3L to observations at smaller scales than previous studies and also for pairs of lens galaxies from different populations. Methods. We compared the G3L signal predicted by the SAMs to measurements in the overlap of the Galaxy And Mass Assembly survey (GAMA), the Kilo-Degree Survey (KiDS), and the VISTA Kilo-degree Infrared Galaxy survey (VIKING) by splitting lens galaxies into two colour and five stellar-mass samples. Using an improved G3L estimator, we measured the three-point correlation of the matter distribution with “mixed lens pairs” with galaxies from different samples, and with “unmixed lens pairs” with galaxies from the same sample. Results. Predictions by the H15 SAM for the G3L signal agree with the observations for all colour-selected samples and all but one stellar-mass-selected sample with 95% confidence. Deviations occur for lenses with stellar masses below 9.5 h−2 M⊙ at scales below 0.2 h−1 Mpc. Predictions by the L12 SAM for stellar-mass selected samples and red galaxies are significantly higher than observed, while the predicted signal for blue galaxy pairs is too low. Conclusions. The L12 SAM predicts more pairs of low stellar mass and red galaxies than the H15 SAM and the observations, as well as fewer pairs of blue galaxies. This difference increases towards the centre of the galaxies’ host halos. Likely explanations are different treatments of environmental effects by the SAMs and different models of the initial mass function. We conclude that G3L provides a stringent test for models of galaxy formation and evolution.

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Gilmore, Gerard, and Rodrigo Ibata. "Large Scale Galactic Structure." International Astronomical Union Colloquium 148 (1995): 258–66. http://dx.doi.org/10.1017/s0252921100022004.

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AbstractModern models of Galaxy formation make fairly specific predictions which are amenable to detailed tests with galactic kinematic and chemical abundance data. For example, popular Cold Dark Matter models ‘predict’ growth of the Galaxy about a central core, which should contain the oldest stars. Later accretion of material forms the outer halo and the disks, while continuing accretion will continue to affect the kinematic structure of both the outer halo and the thin disk. This picture, which contains aspects of both the monolithic (‘ELS’) and the multifragment (‘Searle-Zinn’) pictures often discussed in chemical evolution models, makes some specific predictions which can be tested. The essential feature of these predictions is that they are believable only for the largest scale effects. Large scale properties of the Galaxy must be measured to test them. It is these studies which need large angular scale data. One specific example of current interest is the ‘prediction’ that mergers of small satellites are an essential feature of galactic evolution. This leads one to look for kinematic and spatial structures, and ‘moving groups’, as a primary test of such models.

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Rozprawy doktorskie na temat "Structure and evolution of the Galaxy"

Machado, murtinheiras martins Andre. "Statistical analysis of large scale surveys for constraining the Galaxy evolution." Thesis, Besançon, 2014. http://www.theses.fr/2014BESA2026/document.

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La formation et l'évolution du disque épais de la Voie Lactée restent controversées. Nous avons utilisé un modèle de synthèse de la population de la Galaxie, le Modèle de la Galaxie de Besançon (Robin et al., 2003), qui peut être utilisé pour l'interprétation des données, étudier la structure galactique et tester différents scénarios de formation et évolution Galactique. Nous avons examiné ces questions en étudiant la forme et la distribution de métallicité du disque mince et du disque épais en utilisant l'approche de synthèse de la population. Nous avons imposé sur des simulations les erreurs d'observation et les biais afin de les rendre directement comparables aux observations. Nous avons corrigé les magnitudes et les couleurs des étoiles de la simulation, en utilisant un modèle d'extinction. Les modèles d'extinction disponibles ne reproduisent pas toujours la quantité exacte d'extinction le long de la ligne de visée. Un programme a été développé pour corriger la distribution de l'extinction en fonction de la distance le long de ces lignes. Les extinctions correctes ont ensuite été appliquées sur les simulations du modèle. Nous avons étudié la forme du disque mince en utilisant des données photométriques aux basses latitudes du sondage SDSS-SEGUE. Nous avons comparé qualitativement et quantitativement les observations et les simulations et nous avons essayé de contraindre la fonction de masse initiale. En utilisant la spectroscopie du relevé SEGUE, nous avons sélectionné les étoiles du turn-off de la séquence principale (MSTO) (Cheng et al 2012) et des géantes K pour étudier la distribution de métallicité du disque mince et du disque épais. Nous avons calculé une estimation de distance pour chaque étoile à partir de la relation entre les températures effectives et magnitudes absolues pour les catalogues observés et simulés. Ces deux catalogues ont les mêmes biais sur les distances, elles sont donc comparables. Nous avons développé un outil basé sur une méthode MCMC-ABC pour déterminer la distribution de la métallicité et étudier les corrélations entre les paramètres ajustés. Nous avons confirmé la présence d'un gradient de métallicité radiale de -0.079 ± 0.015 dex kpc−1 pour le disque mince. Nous avons obtenu une métallicité du disque épais au voisinage solaire de -0.47 ± 0.03 dex, compatible avec les résultats obtenus par les études précédentes. De plus, le disque épais ne montre pas de gradient, mais les données sont compatibles avec un gradient positif intérieur suivi d'un négatif extérieur. Nous avons ensuite appliqué les outils développés au relevé spectroscopique Gaia-ESO et calculé la distribution de métallicité des étoiles F/G/K dans le disque mince et épais en supposant une formation en deux époques du disque épais de la Voie Lactée. Nous avons obtenu une métallicité locale dans le disque épais de -0.23 ± 0.04 dex légèrement plus élevée que celle obtenue avec SEGUE mais en accord avec Adibekyan et al. (2013) et un gradient de métallicité radiale du disque épais en accord avec notre analyse précédente des données de SEGUE et la littérature. La métallicité locale est en accord avec la littérature au niveau de 3σ mais parce que les données GES sont préliminaires, une analyse plus approfondie avec plus de données et de meilleurs calibrations doit être faite. L'existence d'un gradient plat dans le disque épais peut être une conséquence d'une formation à partir d’un gaz turbulent et bien homogène, ou bien un fort mélange radial a brassé après coup les étoiles The 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

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Cole, Shaun. "Evolution of large scale structure and galaxy formation." Thesis, University of Cambridge, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.315745.

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Majewski, Steven R., Ricardo P. Schiavon, Peter M. Frinchaboy, et al. "The Apache Point Observatory Galactic Evolution Experiment (APOGEE)." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625493.

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE), one of the programs in the Sloan Digital Sky Survey III (SDSS-III), has now completed its systematic, homogeneous spectroscopic survey sampling all major populations of the Milky Way. After a three-year observing campaign on the Sloan 2.5 m Telescope, APOGEE has collected a half million high-resolution (R similar to 22,500), high signal-to-noise ratio (>100), infrared (1.51-1.70 mu m) spectra for 146,000 stars, with time series information via repeat visits to most of these stars. This paper describes the motivations for the survey and its overall design-hardware, field placement, target selection, operations-and gives an overview of these aspects as well as the data reduction, analysis, and products. An index is also given to the complement of technical papers that describe various critical survey components in detail. Finally, we discuss the achieved survey performance and illustrate the variety of potential uses of the data products by way of a number of science demonstrations, which span from time series analysis of stellar spectral variations and radial velocity variations from stellar companions, to spatial maps of kinematics, metallicity, and abundance patterns across the Galaxy and as a function of age, to new views of the interstellar medium, the chemistry of star clusters, and the discovery of rare stellar species. As part of SDSS-III Data Release 12 and later releases, all of the APOGEE data products are publicly available.

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Durkalec, Anna. "Properties and evolution of galaxy clustering at 2." Thesis, Aix-Marseille, 2014. http://www.theses.fr/2014AIXM4758/document.

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Cette thèse porte sur l'étude des propriétés et l'évolution de regroupement de galaxies pour les galaxies de la gamme de 22. Je ai pu mesurer la distribution spatiale d'une population générale de galaxie à redshift z~3 pour la première fois avec une grande précision. Je ai quantifié le regroupement de galaxie en estimation et la modélisation de la fonction de corrélation projetée (espace réel) à deux points, pour une population générale de 3022 galaxies. Je ai prolongé les mesures de regroupement à la luminosité et des sous-échantillons de masse sélectionné stellaires. Mes résultats montrent que la force de regroupement de la population générale de la galaxie ne change pas de redshift z~3,5 à z~2,5, mais dans les deux redshift va plus lumineux et des galaxies plus massives sont plus regroupées que les moins lumineux (massives). En utilisant la distribution d'occupation de halo (HOD) formalisme je mesuré une masse moyenne de halo hôte au redshift z~3 significativement plus faible que les masses halo moyens observés à faible redshift. Je ai conclu que la population de formation d'étoiles observé des galaxies à z~3 aurait évolué dans le massif et lumineux la population de galaxies au z=0. Aussi, je interpréter les mesures de regroupement en termes de biais de galaxies à grande échelle linéaire. Je trouve que ce est nettement plus élevé que le biais des galaxies redshift intermédiaire et faible. Enfin, je ai calculé le ratio-stellaire Halo masse (SHMR) et l'efficacité intégrée de formation d'étoiles (ISFE) pour étudier l'efficacité de la formation des étoiles et l'assemblage masse stellaire This thesis focuses on the study of the properties and evolution of galaxy clustering for galaxies in the redshift range 22. I was able to measure the spatial distribution of a general galaxy population at redshift z~3 for the first time with a high accuracy. I quantified the galaxy clustering by estimating and modelling the projected (real-space) two-point correlation function, for a general population of 3022 galaxies. I extended the clustering measurements to the luminosity and stellar mass-selected sub-samples. My results show that the clustering strength of the general galaxy population does not change significantly from redshift z~3.5 to z~2.5, but in both redshift ranges more luminous and more massive galaxies are more clustered than less luminous (massive) ones. Using the halo occupation distribution (HOD) formalism I measured an average host halo mass at redshift z~3 significantly lower than the observed average halo masses at low redshift. I concluded that the observed star-forming population of galaxies at z~3 might have evolved into the massive and bright (Mr<-21.5) galaxy population at redshift z=0. Also, I interpret clustering measurements in terms of a linear large-scale galaxy bias. I find it to be significantly higher than the bias of intermediate and low redshift galaxies. Finally, I computed the stellar-to-halo mass ratio (SHMR) and the integrated star formation efficiency (ISFE) to study the efficiency of star formation and stellar mass assembly. I find that the integrated star formation efficiency is quite high at ~16% for the average galaxies at z~3

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Legrand, Louis. "Large surveys : from galaxy evolution to cosmological probes." Thesis, université Paris-Saclay, 2020. http://www.theses.fr/2020UPASP023.

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Les grands relevés de galaxies sont des fenêtres ouvertes sur notre Univers: ils nous offrent de précieuses informations sur son contenu et sur son évolution. D'une part les relevés profonds explorent la formation et l'évolution des galaxies. D'autre part, les relevés à grand champ cartographient la distribution de la matière dans le but de comprendre la nature de l'énergie noire et de la matière noire.Au cours de cette thèse, j'explore les capacités offertes par ces relevés afin de répondre aux questions suivantes:1. Quels sont les principaux moteurs de l'évolutions des galaxies ? 2. Quelles progrès dans notre connaissance de l'Univers seront apportés par les futurs relevés de galaxies ? Je commence par déterminer la relation entre la masse stellaire et la masse des halos de matière noire des galaxies en utilisant des mesures précises de la fonction de masse stellaire dans le champ COSMOS. Grâce à l'exhaustivité du relevé COSMOS entre z ~0.2 et z ~ 5, j'obtiens pour la première fois cette relation sur une aussi grande gamme de redshifts à partir d'un seul relevé.Je constate que la masse de halo caractéristique, définie comme maximisant le rapport entre la masse stellaire et la masse du halo, augmente entre z=0 et z=2.3 et reste stable jusqu'à z = 4.Cette augmentation de la masse de halo caractéristique met en lumière le rôle des flux de gaz froid comme moteurs de la formation des galaxies à grand redshift. Afin d'approfondir ce sujet, je combine des observations de la teneur en gaz moléculaire froid des galaxies jusqu'à z=4, avec la relation entre masse stellaire et masse du halo de matière noire. Je constate que l'évolution de la fraction de masse du gaz froid est en accord avec l'hypothèse selon laquelle les apports de gaz froid sont responsables de la plus grande efficacité de formation des galaxies à grand redshift dans les halos massifs.Ensuite, dans le but de maximiser les contraintes cosmologique qui seront apportées par les prochains grands relevés spectroscopiques, je montre qu'une nouvelle observable, les fluctuations angulaires de redshift (ARF), apportent des informations complémentaires par rapport au traditionnel ``angular galaxy clustering''. Grâce à leurs sensibilités particulières au champ de vélocité de la matière, je montre que les dégénérescences entre les paramètres cosmologiques et de biais des galaxies sont différentes lorsqu'elles se basent sur les ARF ou sur le ``angular galaxy clustering''. Dès lors, la combinaison des deux observables permet de lever des dégénérescences et d'améliorer les contraintes, d'un facteur au moins deux, sur la plupart des paramètres des modèles ^CDM et wCDM.Finalement, en tant que membre de la collaboration Euclid, j'ai exploré le potentiel cosmologique de ce futur relevé de galaxies. Ce relevé nous permettra de mesurer très précisément la distribution de la matière sur tout le ciel extra-galactique. Dans le but d'exploiter entièrement tout son potentiel, il est crucial de le combiner avec les futurs relevés du CMB.J'utilise le formalisme de Fisher afin de prédire l'intérêt d'une analyse combinée des sondes CMB avec les sondes Euclid. Je teste à la fois le modèle ^CDM standard et ses extensions, et montre que le CMB améliorera les contraintes d'un facteur au moins deux sur la plupart des paramètres cosmologiques, et notamment sur les modèles d'énergie noire alternatifs, qui font partie des intérêts majeurs pour Euclid Large galaxy surveys are like open windows on our Universe: they provide precious insights on its components and on its evolution. On the one hand, pencil surveys go deep into the cosmos to explore the formation and evolution of galaxies. On the other hand, wide surveys are mapping the distribution of matter on large scales to understand the nature of dark energy and dark matter.During my thesis, I explore the capabilities of these large surveys to address the following questions:1. What are the main drivers of galaxy evolution? 2. What improvements on our knowledge of the Universe will be brought by upcoming wide galaxy surveys? Using precise galaxy stellar-mass function measurements in the COSMOS field, I first determine the stellar-to-halo mass relation through a parametric abundance matching technique. Thanks to the completeness of the COSMOS survey from z ~ 0.2 to z ~ 5, I obtain for the first time this relation over such a large redshift range from a single coherent sample.I find that the ratio of stellar-to-halo mass content peaks at a characteristic halo mass which increases up to z = 2.3 and remains flat up to z = 4.This steady increase of the characteristic halo mass questions the role of cold gas inflows as drivers of galaxy formation at high redshift.To address this question, I link observations of the cold molecular gas content in galaxies up to z = 4 to the evolution of the dark matter halo mass. I find that the joint evolution of cold gas mass fraction and halo mass is in agreement with the hypothesis of cold gas inflows being responsible of efficient galaxy formation at high redshift.With the scope of maximising the cosmological power of next generation spectroscopic surveys, I show that a novel cosmological observable, the angular redshift fluctuations (ARF) will provide complementary cosmological information in addition to the standard angular galaxy clustering. Due to its distinct sensitivity to the peculiar velocity field, I find that the cosmological and galaxy bias parameters express different degeneracies when inferred from ARF or from angular galaxy clustering.As such, combining both observables breaks these degeneracies and greatly decreases the marginalised uncertainties, by a factor of at least two on most parameters in the ^CDM and wCDM models.As part of the Euclid collaboration, I then investigate the cosmological power of the upcoming Euclid survey, which will offer us an exquisite measurement of the matter distributions on the full extra-galactic sky.In order to fully exploit all the potential of the Euclid survey it is crucial to combine it with upcoming CMB surveys.I use the Fisher formalism to forecast the benefits of performing a joint analysis of CMB probes with Euclid main probes (weak lensing and galaxy clustering). I test both the standard cosmological model, ^CDM, and its extensions, and show that CMB will improve the constraints by a factor two on most cosmological parameters, and most notably on dark energy modified models which are of key interest for Euclid

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Hatzidimitriou, D. "The evolution and geometry of the oouter parts of the Small Magellanic Cloud." Thesis, University of Edinburgh, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.234097.

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Laporte, 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.

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We present N-body and hydrodynamical simulations of the response of the Milky Way's baryonic disc to the presence of the Large Magellanic Cloud during a first infall scenario. For a fiducial Galactic model reproducing the gross properties of the Galaxy, we explore a set of six initial conditions for the Large Magellanic Cloud (LMC) of varying mass which all evolve to fit the measured constraints on its current position and velocity with respect to the Galactic Centre. We find that the LMC can produce strong disturbances - warping of the stellar and gaseous discs - in the Galaxy, without violating constraints from the phase-space distribution of stars in the Solar Neighbourhood. All models correctly reproduce the phases of the warp and its antisymmetrical shape about the disc's mid-plane. If the warp is due to the LMC alone, then the largest mass model is favoured (2.5 x 10(11) M-circle dot). Still, some quantitative discrepancies remain, including deficits in height of Delta Z = 0.7 kpc at R = 22 kpc and Delta Z = 0.7 kpc at R = 16 kpc. This suggests that even higher infall masses for the LMC's halo are allowed by the data. A comparison with the vertical perturbations induced by a heavy Sagittarius dSph model (10(11) M-circle dot) suggest that positive interference with the LMC warp is expected at R = 16 kpc. We conclude that the vertical structure of the Galactic disc beyond the Solar Neighbourhood may jointly be shaped by its most massive satellites. As such, the current structure of the Milky Way suggests we are seeing the process of disc heating by satellite interactions in action.

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Kruk, Sandor J. "Evolution of barred galaxies and associated structures." Thesis, University of Oxford, 2018. http://ora.ox.ac.uk/objects/uuid:34cc9283-a386-464f-b9ae-1d4e3b4fdf77.

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Bars are common in disc galaxies along with many associated structures such as disc-like bulges, boxy/peanut bulges, rings, etc. They are a sign of maturity of disc galaxies and can play an important role in their evolution. In this thesis, I investigate the specific role bars play in quenching the star formation in, and shaping of their host galaxies. In order to test how bars affect their host galaxies, I study the discs, bars and bulges of what is currently the largest sample of barred galaxies (~3,500), selected with visual morphologies from the Galaxy Zoo project. I perform multi-wavelength and multi-component photometric decomposition, with the novel GALFITM software. With the detailed structural analysis I obtain physical quantities such as the bar- and bulge-to-total luminosity ratios, effective radii, Sérsic indices and colours of the individual components. I find a clear difference in the colours of the components, the discs being bluer than the bars and bulges. An overwhelming fraction of bulge components have Sérsic indices consistent with being disc-like bulges. I compare the barred galaxies with a mass- and environment-matched volume-limited sample of unbarred galaxies, finding that the discs of unbarred galaxies are bluer compared to the discs of barred galaxies, while there is only a small difference in the colours of the bulges. I suggest that this is evidence for secular evolution via bars that leads to the build-up of disc-like bulges and to the quenching of star formation in the galaxy discs. I identify a subsample of unbarred galaxies that are better fitted with an additional component, identified as an inner lens/oval. I find that their structural properties are similar to barred galaxies, and speculate that lenses might be former bars. Using the decompositions, I identify a sample of 271 late-type galaxies with curious bars that are off-centre from the disc. I measure offsets up to 2.5 kpc between the photometric centres of the stellar disc and stellar bar, which are in good agreement with predictions from simulations of dwarf-dwarf tidal interactions. The median mass of these galaxies is 109.6 M⊙, and they are similar to the Large Magellanic Cloud, which also has an offset bar. Very few high mass galaxies with significant bulges show offsets, thus I suggest that the self-gravity of a significant bulge prevents the disc and bar from getting displaced with respect to each other. I conduct a search for companions to test the hypothesis of tidal interactions, but find that a similar fraction of galaxies with offset bars have companions within 100 kpc as galaxies with centred bars. Since many of these galaxies appear isolated, interactions might not be the only way to produce an offset bar. One suggested alternative is that the dark matter haloes surrounding the galaxies are lopsided, which distorts the potential, and imprints the lopsidedness and offsets onto the galaxy discs. I investigate the asymmetries in the kinematics of a subsample of such galaxies using data from the MaNGA survey, and find that the perturbations in the haloes are ~ 6% for both galaxies with off-centre and centred bars. I also measure the amplitude of non-circular motions in the outer discs due to an oval potential and find only minor departures from circularity, suggesting that the dark matter haloes are consistent with being spherical (axis ratio q ≳ 0.96). Therefore, the lopsidedness of the dark matter haloes cannot be the origin of the offsets. Either small companions are missed due to the incompleteness of the Sloan Digital Sky Survey spectroscopic survey, or interactions with dark matter satellites might explain the offsets. Modeling the kinematics of these galaxies, I find that the Hα gas rotation is centred closer to the centre of the bar than the centre of stellar rotation, suggesting that, in general, the bars are located closer to the dynamical centres of these galaxies than the discs. This implies that the discs are offset in these galaxies, not the bars. If offsets are characteristic of low mass galaxies only, high mass galaxies show vertically extended bars, known as boxy/peanut bulges. I investigate, for the first time, the formation and evolution of these structures associated to bars, from z≈0 to z=1. I compare two samples of moderately inclined galaxies with masses M* > 1010 M⊙, imaged by the Sloan Digital Sky Survey and the Hubble Space Telescope. Using a novel technique to classify bar isophotes, and based on the visual inspection of three expert astronomers, I find an evolving fraction of galaxies having boxy/peanut bulges from 30% at z≈0 to ~ 0% at z=1, and a strong correlation with stellar mass. I find 26 galaxies (15 at higher redshifts) in the phase of bar buckling, the mechanism proposed to form boxy/peanut bulges. The peak redshift of buckling is z≈0.75, where the bar buckling fraction is 4 times higher than in the local Universe. My observations suggest that many, if not all, of the boxy/peanut bulges are formed via buckling, ~ 2 Gyr after bar formation, with the buckling phase lasting for approximately 0.8 Gyr. I discuss my findings in the context of the evolution of barred galaxies and propose ideas for future work - applying similar decomposition techniques to higher redshift, and better resolution datasets, using integral field spectroscopic data to study the stellar populations of barred galaxies in greater detail, as well as a novel project to identify large nuclear discs in galaxies.

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Laigle, Clotilde. "Observational and theoretical constraints on galaxy evolution at high redshift." Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066343.

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Je présente dans cette thèse de nouvelles contraintes sur la formation et l’évolution des galaxies, en étudiant leur croissance en masse et leur évolution au sein de la toile cosmique depuis l’époque de leur formation jusqu’à maintenant. Pour cela, j’ai créé un catalogue photométrique sur le champ COSMOS. Ce catalogue permet de sonder avec précision l’Univers à haut redshift. J’analyse ce relevé observé à l’aide de relevés virtuels, produits à partir de simulations hydrodynamiques. Ces simulations implémentent nos connaissances sur la formation et l’évolution des galaxies.Dans un premier temps, je montre que l’évolution en redshift des propriétés des galaxies est relativement bien comprise en invoquant des processus qui dépendent essentiellement de la masse, tels que le feedback des étoiles et des AGN. Je souligne également comment nos méthodes observationnelles génèrent des biais dans les propriétés physiques des galaxies calculées à partir de la photométrie.Dans un deuxième temps, je montre comment la dynamique des flots de matière à grande échelle gouverne l’acquisition du moment angulaire des galaxies et halos de matière noire, ce qui implique que certaines propriétés des galaxies sont supposées dépendre de leur environnement anisotrope. J’ai extrait la structure filamentaire du catalogue photométrique que j’ai créé sur le champ COSMOS et j’ai mesuré cette dépendance. Je trouve des gradients de masse et de couleurs dans la direction du filament. Il apparaît que la masse et le moment angulaire des galaxies sont deux quantités interdépendantes et tous deux impactés par leur environnement anisotrope I present in this thesis new constraints on galaxy formation and evolution while studying the galaxy mass growth and the co-evolution of the cosmic web and the embedded galaxies, from the epoch of cosmic dawn to today.To do so, I first created a new photometric catalog on the COSMOS field with precise photometric redshifts allowing to probe accurately the high-redshift Universe. I analyze this survey while relying heavily on comparisons with virtual galaxy surveys produced from state-of-the- art cosmological hydrodynamical simulations, which capture all our current knowledge of galaxy formation and evolution.From this comparative analysis, in the first part of my thesis I show that the redshift evolution of galaxy properties is reasonably well understood when invoking mass-dependent processes (AGN and stellar feed- back). I highlight also the effect of simplifying assumptions inherent to our observational methods, which bias the physical properties computed from galaxy photometry.Galaxies and haloes are embedded in the cosmic web, an intricate large-scale structure of walls, filaments and nodes. In the second part of my thesis, I show how galaxies and dark haloes gain their angular momentum from the large-scale flow, implying that some of their properties depend on their anisotropic filamentary environment. I then extract the filamentary structure from the observed photometric catalog and measure the dependence of galaxy properties to the anisotropic environment. I find mass and colour gradients towards the filaments. In turn it emerges that galaxy masses and angular momenta are two dependent quantities impacted by their anisotropic environment

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Roldán, Carlos Antonio Calcáneo. "The evolution of dark matter substructure." Thesis, Durham University, 2001. http://etheses.dur.ac.uk/4232/.

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This thesis investigates the dynamical evolution of systems orbiting within deeper potentials. Initially we use a simple satellite-halo interaction to study the dynamical processes that act on orbiting systems and we compare these results to analytical theory. Deep images of the Centaurus cluster reveal a spectacular arc of diffuse light that stretches for over 100 kpc and yet is just a few kpc wide. We use numerical simulations to show that this feature can be produced by the tidal debris of a spiral galaxy that has been disrupted by the potential of one of the central cD galaxies of the cluster. The evolution of sub-halos is then studied in a cosmological context using high resolution N-body simulations of galactic mass halos that form in a cold dark matter (CDM) simulation. CDM halos form via a complex series of mergers, accretion events and violent relaxation. Halos are non-spherical, have steep singular density profiles and contain many thousands of surviving dark matter substructure clumps. This will lead to several unique signatures for experiments that aim to detect dark matter either indirectly, through particle annihilation, or directly in a laboratory. For the first time it is possible to construct maps of the gamma-ray sky that result from the annihilation of dark matter particles within simulated dark matter halo distributions.

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Książki na temat "Structure and evolution of the Galaxy"

S, Mulchaey John, Dressler Alan Michael, and Oemler Augustus 1945-, eds. Clusters of galaxies: Probes of cosmological structure and galaxy evolution. Cambridge University Press, 2004.

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Guillermo Haro Conference on Astrophysics (3rd 1999 Puebla, Pue., Mexico). Cosmic evolution and galaxy formation: Structure, interactions, and feedback : the 3rd Guillermo Haro Astrophysics Conference. Astronomical Society of the Pacific, 2000.

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Giuseppina, Fabbiano, Harvard-Smithsonian Center for Astrophysics, and United States. National Aeronautics and Space Administration., eds. The evolution of gas and stars in the merger galaxy NGC 1316 (Fornax A). Harvard-Smithsonian Center for Astrophysics, 1998.

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Weinzirl, Timothy. Probing Galaxy Evolution by Unveiling the Structure of Massive Galaxies Across Cosmic Time and in Diverse Environments. Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-06959-3.

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1956-, Clemens Dan P., Shah Ronak Y, Brainerd Tereasa G. 1964-, and Boston University. Institute for Astrophysical Research., eds. Milky Way surveys: The structure and evolution of our Galaxy : the fifth Boston University Astrophysics conference : proceedings of a meeting held in Boston, Massachusetts, 15-17 June 2003. Astronomical Society of the Pacific, 2004.

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Van den Bosch, Frank, 1969- and White S, eds. Galaxy formation and evolution. Cambridge University Press, 2010.

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Galaxy formation and evolution. Springer, 2005.

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Spinrad, Hyron. Galaxy formation and evolution. Springer, 2005.

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Bender, Ralf, and Roger L. Davies, eds. New Light on Galaxy Evolution. Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9.

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Kippenhahn, Rudolf, Alfred Weigert, and Achim Weiss. Stellar Structure and Evolution. Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-30304-3.

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Części książek na temat "Structure and evolution of the Galaxy"

Grosbøl, Preben. "Spiral Structure and Galaxy Evolution." In Astrophysics and Space Science Library. Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_13.

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Navarro, Julio F. "The Structure of Cold Dark Matter Halos." In New Light on Galaxy Evolution. Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_38.

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Villumsen, Jens Verner. "Evolution of the Vertical Structure of Galactic Disks." In The Milky Way Galaxy. Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5291-1_94.

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Burkert, A. "The Structure of Dark Matter Halos in Dwarf Galaxies." In New Light on Galaxy Evolution. Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0229-9_25.

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Valentijn, Edwin A. "Are Cooling Flows Governing E-Galaxy Evolution?" In Structure and Dynamics of Elliptical Galaxies. Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3971-4_59.

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Hidalgo, Sebastian L., Antonio Aparicio, and David Martínez-Delgado. "The Extended Structure of the Phoenix Dwarf Galaxy." In The Evolution of Galaxies. Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-3315-1_57.

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van der Laan, H., P. Katgert, and M. J. A. Oort. "Radio Galaxy Populations: A Progress Report." In Structure and Evolution of Active Galactic Nuclei. Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4562-3_25.

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Van Loon, Jacco. "Structure and Evolution of the Inner Milky Way Galaxy." In The Evolution of Galaxies. Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3313-7_69.

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Meurs, E. J. A. "Towards the Luminosity Function of Seyfert Galaxy Nuclei." In Structure and Evolution of Active Galactic Nuclei. Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4562-3_66.

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Marconi, M., I. Musella, M. Di Criscienzo, et al. "STREGA@VST: Structure and Evolution of the Galaxy." In Astrophysics and Space Science Proceedings. Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-19330-4_22.

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Streszczenia konferencji na temat "Structure and evolution of the Galaxy"

Kelvin, Lee, Simon Driver, Aaron Robotham, et al. "Exploring Galaxy Formation and Evolution via Structural Decomposition." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458501.

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Bouchard, Antoine, Sarah Blyth, W. J. G. de Blok, Benne Holwerda, and Kurt van der Heyden. "The Environmental Impact on Galaxy Evolution: Highlighting the Structure of the Local Cosmic Web." In Panoramic Radio Astronomy: Wide-field 1-2 GHz research on galaxy evolution. Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.089.0053.

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Pan, Jing, Yijie Shen, Hao Wang, and Qiang Liu. "Galaxy waves: 3D inhomogeneous auto-accelerating beams." In CLEO: Science and Innovations. Optica Publishing Group, 2022. http://dx.doi.org/10.1364/cleo_si.2022.sf3i.8.

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We propose and generate a new class of structured light whose wavepackets have 3D inhomogeneous angular velocity evolution with auto-accelerating upon both its longitudinal propagation and transverse multilayer rotation akin to galactic kinematics.

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Stanghellini, Carlo. "Radio galaxy Evolution." In First MCCT-SKADS Training School. Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.059.0015.

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Silk, Joseph, and Rychard Bouwens. "Simulating galaxy evolution." In AFTER THE DARK AGES. ASCE, 1999. http://dx.doi.org/10.1063/1.58639.

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Madore, Barry F. "GALEX: Galaxy Evolution Explorer." In THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP, 2005. http://dx.doi.org/10.1063/1.1913948.

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Martin, Christopher, Thomas Barlow, William Barnhart, et al. "The Galaxy Evolution Explorer." In Astronomical Telescopes and Instrumentation, edited by J. Chris Blades and Oswald H. W. Siegmund. SPIE, 2003. http://dx.doi.org/10.1117/12.460034.

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Tonnesen, Stephanie. "Environmentally-Driven Galaxy Evolution." In Frank N. Bash Symposium 2011: New Horizons in Astronomy. Sissa Medialab, 2012. http://dx.doi.org/10.22323/1.149.0008.

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Page, M. J., F. J. Carrera, J. A. Stevens, A. Comastri, L. Angelini, and M. Cappi. "QSO winds and galaxy evolution." In X-RAY ASTRONOMY 2009; PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES: Proceedings of the International Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3475264.

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Fraternali, Filippo, Victor P. Debattista, and C. C. Popescu. "Gas Circulation and Galaxy Evolution." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458468.

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Raporty organizacyjne na temat "Structure and evolution of the Galaxy"

Arraki, Kenza Sigrid. Evolution of dwarf galaxy properties in local group environments. Office of Scientific and Technical Information (OSTI), 2016. http://dx.doi.org/10.2172/1491856.

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Zhang, Yuanyuan. Looking Wider and Further: The Evolution of Galaxies Inside Galaxy Clusters. Office of Scientific and Technical Information (OSTI), 2016. http://dx.doi.org/10.2172/1248222.

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Bunker, A. J., and W. J. M. van Breugel. The Hy-Redshift Universe: Galaxy Formation and Evolution at High Redshift. Office of Scientific and Technical Information (OSTI), 1999. http://dx.doi.org/10.2172/793845.

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Meyer, B. S., and D. N. Schramm. General constraints on the age and chemical evolution of the Galaxy. Office of Scientific and Technical Information (OSTI), 1986. http://dx.doi.org/10.2172/5797647.

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España Fontán, Paula, and Maria Angeles Gomez Flechoso. Effects of the orbit orientation on the evolution of dwarf satellite galaxies. Fundación Avanza, 2023. http://dx.doi.org/10.60096/fundacionavanza/2492022.

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Cosmological models propose a hierarchical scenario for galaxy evolution, where dwarf galaxies are accreted in the halo of larger ones. We study the effect of the satellite’s orbital orientation on the planar alignment of satellite galaxies.

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Piacentine, J. Detection of Galaxy Clusters with the XMM-Newton Large Scale Structure Survey. Office of Scientific and Technical Information (OSTI), 2004. http://dx.doi.org/10.2172/833122.

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Keller, Christopher J. Analysis of Pacific Enroute Structure in Support of C-5M Super Galaxy. Defense Technical Information Center, 2015. http://dx.doi.org/10.21236/ada619564.

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Arnold, Frances H. Evolution by Structure-Based Protein Recombination. Defense Technical Information Center, 2003. http://dx.doi.org/10.21236/ada417404.

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Martin, J. E., J. P. Wilcoxon, and R. A. Anderson. Evolution of structure during phase transitions. Office of Scientific and Technical Information (OSTI), 1996. http://dx.doi.org/10.2172/238582.

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Hoversten, Erik A. Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey. Office of Scientific and Technical Information (OSTI), 2007. http://dx.doi.org/10.2172/935485.

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