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Dissertations / Theses on the topic 'Galaxy formation clusters'

Author: Grafiati

Published: 11 March 2023

Last updated: 31 July 2025

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1

Beasley, Michael Andrew. "Globular clusters as probes of galaxy formation." Thesis, Durham University, 2001. http://etheses.dur.ac.uk/4949/.

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Observations and analysis of globular cluster systems associated with three galaxy types are presented. Spectroscopy of globular cluster (GC) candidates in the Sculptor spirals NGC 253 and NGC 55 has identified 15 GCs in these galaxies. This spectroscopic sample, combined with plate scans, indicates total GC populations consistent with that expected for their luminosity and morphological type. From these data, we define new GC samples for spectroscopy. Radial velocities of 87 GCs in the Virgo elliptical NGC 4472 have been obtained, yielding data for 144 GCs when combined with previous studies.

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2

Contini, Emanuele. "Galaxy populations in clusters and proto-clusters." Doctoral thesis, Università degli studi di Trieste, 2014. http://hdl.handle.net/10077/9964.

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2012/2013<br>The aim of my Thesis is to explore the physical properties of the galaxy population in clusters and proto-clusters. A large number of physical processes plays an important role in the formation and evolution of galaxies: cooling, that allows the condensation of gas in the centre of dark matter haloes; star formation, that converts cold gas in stars; feedback from Active Galactic Nuclei (AGN), that prevents the gas in the central regions of haloes from "over-cooling"; feedback from Supernovae, which liberates energy in the surrounding, mixing the gas and enriching it with hea

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3

Finn, Rose A. "Star-formation rates of high-redshift galaxy clusters." Diss., The University of Arizona, 2003. http://hdl.handle.net/10150/289932.

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In this thesis, we take the first step toward building a star-formation limited sample of z ∼ 0.8 cluster galaxies with the goal of understanding the physical processes that affect star formation within the cluster environment. We present Hα narrow-band imaging results for four z ∼ 0.8 clusters. We reach 3σ star-formation rate (SFR) limits of ≤ 0.3 h⁻²₁₀₀M(⊙) yr⁻¹, demonstrating that near-infrared, narrow-band imaging centered on the observed wavelength of Hα is a powerful technique for sampling the entire Halpha luminosity function even at relatively high redshifts where Halpha emission moves

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4

Ruggiero, Rafael. "Galaxy Evolution in Clusters." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-14022019-140755/.

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In this thesis, we aim to further elucidate the phenomenon of galaxy evolution in the environment of galaxy clusters using the methodology of numerical simulations. For that, we have developed hydrodynamic models in which idealized gas-rich galaxies move within the ICM of idealized galaxy clusters, allowing us to probe in a detailed and controlled manner their evolution in this extreme environment. The main code used in our simulations is RAMSES, and our results concern the changes in gas composition, star formation rate, luminosity and color of infalling galaxies. Additionally to processes ta

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5

Steel, James. "Surface photometry of early-type galaxies in rich clusters." Thesis, Durham University, 1998. http://etheses.dur.ac.uk/4868/.

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This thesis investigates the morphology of early-type galaxies in two rich clusters using 2D surface photometry. In particular, the amount of light in the 'disk' component is focussed upon, as the presence of a disk is the main morphological criterion in distinguishing between the traditional 'elliptical' and 'S0' classes. Extensive and photometric E-band CCD observations of continuous areas of the Coma and Abell 1367 clusters were obtained at the 2.5 m Isaac Newton telescope, La Palma during March 1994. A subset of this large data-set has been used in this study, comprising a magnitude-limite

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6

Tyler, Krystal D. "Star Formation and Galaxy Evolution in Different Environments, from the Field to Massive Clusters." Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/265395.

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This thesis focuses on how a galaxy's environment affects its star formation, from the galactic environment of the most luminous IR galaxies in the universe to groups and massive clusters of galaxies. Initially, we studied a class of high-redshift galaxies with extremely red optical-to-mid-IR colors. We used Spitzer spectra and photometry to identify whether the IR outputs of these objects are dominated by AGNs or star formation. In accordance with the expectation that the AGN contribution should increase with IR luminosity, we find most of our very red IR-luminous galaxies to be dominated b

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7

Croft, Rupert Alfred Charles. "Galaxy clusters and the formation of large-scale structures in the universe." Thesis, University of Oxford, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.308751.

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8

Dias, Bruno Moreira de Souza. "Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds." Universidade de São Paulo, 2014. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/.

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Globular clusters are tracers of the formation and evolution of their host galaxies. Kinematics, chemical abundances, age and position of the clusters allows tracing interactions between Milky Way and surrounding galaxies and outlines their chemical enrichment history. In this thesis we analyse mid-resolution spectra of about 800 red giant stars in 51 Galactic globular clusters. It is the first time that [Fe/H] and [Mg/Fe] derived in a consistent way are published for such a huge sample of globular clusters, almost 1/3 of the total number of catalogued clusters. Our metallicities are showed to

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9

Renaud, Florent. "Dynamics of the Tidal Fields and Formation of Star Clusters in Galaxy Mergers." Phd thesis, Université de Strasbourg, 2010. http://tel.archives-ouvertes.fr/tel-00508301.

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Dans les galaxies en interaction, de colossales forces de marée perturbent la morphologie des progéniteurs pour engendrer les longs bras d'étoiles, gaz et poussières que l'on observe parfois. En plus de leur effet destructeur, les forces de marée peuvent, dans certain cas, se placer dans une configuration protectrice appelée mode compressif. De tels modes protègent alors la matière en leur sein, en augmentant son énergie de liaison. Cette thèse se concentre sur l'étude de ce régime peu connu en quantifiant ses propriétés grâce à des outils numériques et analytiques appliqués à un spectaculaire

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10

Snyder, Gregory Frantz. "Modeling Spatially and Spectrally Resolved Observations to Diagnose the Formation of Elliptical Galaxies." Thesis, Harvard University, 2013. http://dissertations.umi.com/gsas.harvard:10893.

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In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processes affect the appearance of elliptical galaxies. The primary approach is to combine hydrodynamical simulations of galaxy formation, including all major components, with dust radiative transfer to predict their observational signatures. The current paradigm implies that a quiescent elliptical emerges

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11

Simanton, Lesley Ann. "Star Cluster Populations in the Spiral Galaxy M101." University of Toledo / OhioLINK, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=toledo1437587267.

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12

Rudick, Craig S. "The Formation and Evolution of Intracluster Light: Simulations and Observations." Case Western Reserve University School of Graduate Studies / OhioLINK, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=case1282831433.

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13

Franck, Jay. "IDENTIFYING PROTOCLUSTERS IN THE HIGH REDSHIFT UNIVERSE AND MAPPING THEIR EVOLUTION." Case Western Reserve University School of Graduate Studies / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=case1501165130716782.

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14

Pensabene, Francesco. "Open clusters in Gaia era." Doctoral thesis, Università degli studi di Padova, 2018. http://hdl.handle.net/11577/3421954.

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The goal of my work is to address the topic of the formation and evolution of the Galactic disk through the properties of open clusters. During my PhD I use photometric and astrometric data to derive open clusters properties such as distance, age, proper motions and metallicity. The aim is to take advantage of the high quality astrometry and photometry of first Gaia data release to build a homogeneous data base and to improve the cluster census. This is the first step towards Gaia second data release exploitation. To analyze large samples of data I develop and validate an automated pipeline. T

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15

Narbutis, Donatas. "Star Clusters in the M31 Galaxy Southwest Field. Photometric Survey and Population Properties." Doctoral thesis, Lithuanian Academic Libraries Network (LABT), 2010. http://vddb.laba.lt/obj/LT-eLABa-0001:E.02~2010~D_20101230_094017-50405.

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Observational evidence that star formation proceeds in a clustered manner raises a question on the mass function of star clusters and their evolution. However, we have a limited scope of these processes in the Milky Way galaxy. The M31 galaxy is the nearest stellar system similar to our Galaxy, therefore, it is the most suitable one to provide clues for understanding the star cluster population and the evolution of galactic structures. However, detailed study of stellar populations and star clusters is a challenging task for ground-based observations due to crowded stellar fields. Using Subar

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16

Fabjan, Dunja. "The effect of star formation and feedback on the X-ray properties of simulated galaxy clusters." Doctoral thesis, Università degli studi di Trieste, 2010. http://hdl.handle.net/10077/3434.

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2008/2009<br>The aim of this Thesis was to study the X--ray properties of the IntraCluster Medium (ICM) in a cosmological context resorting to high resolution hydrodynamical simulations. The thermodynamical and chemical properties of the ICM were inspected and studied within a set of galaxy clusters that were simulated with the TREE-SPH Gadget2 code (Springel 2005). This code included a detailed model of chemical evolution (Tornatore et al. 2007) as well as prescriptions for different physical processes: star formation, galactic winds and AGN feedback. We use this large set of simulated gala

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17

Belles, Pierre-Emmanuel Aime Marcel. "Formation of stars and star clusters in colliding galaxies." Thesis, University of Hertfordshire, 2013. http://hdl.handle.net/2299/10312.

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Mergers are known to be essential in the formation of large scale structures and to have a significant role in the history of galaxy formation and evolution. Besides a morphological transformation, mergers induce important bursts of star formation. These starburst are characterised by high Star Formation Efficiencies (SFEs) and Specific Star Formation Rates, i.e., high Star Formation Rates (SFR) per unit of gas mass and high SFR per unit of stellar mass, respectively, compared to spiral galaxies. At all redshifts, starburst galaxies are outliers of the sequence of star-forming galaxies defined

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18

Lotz, Marcel [Verfasser], and Andreas [Akademischer Betreuer] Burkert. "Evolution of galactic star formation in galaxy clusters and post-starburst galaxies / Marcel Lotz ; Betreuer: Andreas Burkert." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2021. http://d-nb.info/1232176338/34.

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19

Alberts, Stacey, Alexandra Pope, Mark Brodwin, et al. "STAR FORMATION AND AGN ACTIVITY IN GALAXY CLUSTERS FROM z = 1–2: A MULTI-WAVELENGTH ANALYSIS FEATURING HERSCHEL /PACS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621395.

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We present a detailed, multi-wavelength study of star formation (SF) and active galactic nucleus (AGN) activity in 11 near-infrared (IR) selected, spectroscopically confirmed massive (greater than or similar to 10(14)M(circle dot)) galaxy clusters at 1 < z < 1.75. Using new deep Herschel/PACS imaging, we characterize the optical to far-IR spectral energy distributions (SEDs) for IR-luminous cluster galaxies, finding that they can, on average, be well described by field galaxy templates. Identification and decomposition of AGNs through SED fittings allows us to include the contribution to clust

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Guglielmo, Valentina. "Groups and clusters of galaxies in the XXL survey." Doctoral thesis, Università degli studi di Padova, 2018. http://hdl.handle.net/11577/3421945.

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This thesis presents one of the first census of the properties of galaxies in X-ray selected groups and clusters at intermediate redshift, with the aim of assessing the role of envi- ronment on the galaxy stellar mass assembly, star formation activity and observed stellar population properties. My project is framed in the XXL Survey (Pierre et al. 2016), the largest XMM-Newton programme approved to date, covering two extragalactic regions in the sky of 25 deg2 each one. Extended X-ray sources identified as groups and clusters are spectroscopically confirmed and their main properties are chara

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21

Dodd, Elizabeth Frances. "The environments of active galaxies over cosmic time." Thesis, University of Hertfordshire, 2014. http://hdl.handle.net/2299/15622.

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The overall aim of this thesis is to investigate the environments of AGN, in particular, the density of galaxies in the environments of radio-loud and radio-quiet AGN. This determines whether AGN trace dense environments at high redshifts and whether the environments are important in addressing the problem of radio-loud dichotomy. I extend my research by investigating whether star-formation evolves differently in high-redshift AGN environments compared to the field. I begin by investigating the environments of 169 AGN using Spitzer data at z ∼ 1. I investigate the source density of star-formin

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22

Parroni, Carolina. "Cluster mass scaling relations through weak lensing measurements." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC232/document.

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Les amas de galaxies sont des outils cosmologiques et astrophysiques essentiels, car ce sont les objets les plus grands et les plus massifs gravitationnellement liées dans l'Univers. L'étude de leur fonction de masse, de leur fonction de corrélation et des relations d'échelle entre leur masse et différentes observables nous permettent de tester les prévisions des modèles cosmologique et les scenarii de formation des structures. Ils sont aussi d'intéressants laboratoires pour l'étude de la formation et de l'évolution des galaxies, et de leur interactions avec le milieu qui les entourent, dans d

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23

Jauzac, Mathilde. "Cosmological constraints : from the cosmic infrared background measurement to the gravitational lensing in massive galaxy clusters." Thesis, Aix-Marseille 1, 2011. http://www.theses.fr/2011AIX10096.

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La thématique principale de mon travail de thèse est l’é;volution et la formation structures en fonction du décalage vers le rouge (redshift par la suite).Mon travail de thèse se divise en deux parties distinctes, qui finalement se regroupent au cours de mes derniers travaux. Dans un premier temps, j’ai étudié l’évolution du Fond Diffus Infrarouge (Cosmic Infrared Background, CIB par la suite) en fonction du redshift à 70 et 160 µm en utilisant des données provenant du satellite Spitzer. J’ai effectué ce travail dans les champs GOODS & COSMOS en appliquant la méthode d’empilement (stacking

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24

Fensch, Jérémy. "Star and stellar cluster formation in gas-dominated galaxies." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC207/document.

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Nous étudions la formation d’étoiles et d’amas d’étoiles dans les galaxies dominées par le gaz. Ce terme réfère en premier lieu aux galaxies de l’époque du pic de formation d’étoiles dans l’histoire de l’Univers, qui s’est déroulé vers z ~ 2, mais aussi à leurs analogues locaux, les galaxies naines de marées. En premier lieu, en utilisant des simulations numériques, nous montrons que les galaxies massives typiques de z=2, avec une fraction de gaz d’environ 50%, forment des structures gazeuses massives (10**7-8 masses solaires) et liées gravitationnellement, appelées grumeaux dans la suite. Ces

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Blanco-Cuaresma, Sergi. "Test de la technique de marquage chimique avec des amas ouverts." Thesis, Bordeaux, 2014. http://www.theses.fr/2014BORD0079/document.

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Contexte. Les étoiles naissent ensemble dans des nuages moléculaires géants. Si nous faisons l’hypothèse qu’ils étaient à l’origine chimiquement homogènes et bien mélangés, nous nous attendrions à ce que les étoiles issues d’un même nuage aient la même composition chimique. La plupart des groupes d’étoiles sont perturbés lors de leur évolution dans la galaxie et l’information dynamique est perdue. Ainsi la seule possibilité que nous ayons de reconstruire l’histoire de la formation stellaire est d’analyser les abondances chimiques que l’on observe aujourd’hui.But. La technique de marquage chimi

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Mulia, Alexander John. "Stellar Populations in Nearby Merging Galaxies." University of Toledo / OhioLINK, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=toledo1449827923.

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27

Clarenc, Benjamin. "Candidats (proto-)amas de galaxies à grand redshift vus par le CFHT." Thesis, Université Paris-Saclay (ComUE), 2018. http://www.theses.fr/2018SACLS234/document.

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Les galaxies locales ont des propriétés différentes selon leur environnement : couleur, morphologie, fraction de gaz, etc. Cette différentiation s'est opérée durant leur formation. Les observations indiquent que ce pic d'activité de formation stellaire a eu lieu vers z=2 et que les environnements denses étaient à cette époque des lieux de formation stellaire très intense, soit l'inverse d'aujourd'hui. C'est en observant les progéniteurs des amas massifs actuels que l'on pourra comprendre l’origine de ces différences. Mais les (proto-)amas à grand z sont difficilement observables. De bons candi

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Burgess, Andrew. "Exploration de la fonction de faible masse initiale dans les amas jeunes et les r ´egions de formation stellaire." Phd thesis, Université de Grenoble, 2010. http://tel.archives-ouvertes.fr/tel-00576460.

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La détermination de l'extrémité inférieure de la fonction de masse initiale (FMI) prévoit de fortes contraintes sur les théories de la formation des étoiles. IC4665 est un amas d'´étoile jeune (30Myr) et il a situe 356pc de la Terre. L'extinction est Av~ 0.59 ± 0.15 mag. WIRCam Y, J, H et K observations ont été faites par le CFHT et a comprise 10 champs (de 1.1sq.deg totale) et deux zones de contrle de 20'x20' chacun. Diagrammes couleur/magnitude et couleur/couleur ont été utilisées pour comparer les candidats sélectionnées par les modèles BT-SETTL 30 et 50Myr. Les images CH4off et CH4on ont é

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29

Strader, Jay. "Extragalactic globular cluster subpopulations and galaxy formation /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2007. http://uclibs.org/PID/11984.

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30

Cho, Jaeil. "Globular cluster systems and their implications of galaxy formation." Thesis, Durham University, 2008. http://etheses.dur.ac.uk/2427/.

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In this thesis the spectroscopic and photometric results of the Galactic and extragalactic globular clusters are presented. And their implications on galaxy formation have been investigated. Integrated spectroscopy with a high resolution of 24 Galactic globular clusters were obtained using the Isacc Newton Telescope, from which 21 line indices were carefully measured and calibrated. By comparing with recent simple stellar population models (Thomas et al. 2003 and Lee & Worthey 2005), it is confirmed that Galactic globular clusters are old (~10- 12 Gyr). There is a discrepancy between the t

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Ruppin, Florian. "Cosmologie via les observations d'amas de galaxies par effet Sunyaev-Zel'dovich avec NIKA2." Thesis, Université Grenoble Alpes (ComUE), 2018. http://www.theses.fr/2018GREAY029/document.

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La distribution de masse dans l'Univers telle que tracée par les amas de galaxies constitue une sonde cosmologique puissante. La caractérisation des processus associés à l'origine et à la croissance des grandes structures permet de contraindre des paramètres cosmologiques via l'étude de la distribution des amas en fonction de leur masse et de leur redshift. Cependant, il existe un désaccord statistiquement significatif observé entre les contraintes cosmologiques établies par l'étude des anisotropies primaires du fond diffus cosmologique et celles issues de l'analyse de la distribution des amas

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Santoro, Fernando. "Semi analytical simulations of primordial star cluster formation." Thesis, University of Sussex, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.288843.

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Cai, Zheng. "Cosmic Structure Formation: From First Star to Large-scale Filamentary Structure." Diss., The University of Arizona, 2015. http://hdl.handle.net/10150/578387.

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Theory of cosmic structure formation outlines how stars, galaxies, clusters of galaxies, and large-scale structures formed out of primordial density fluctuations. It presents us a picture of cosmic mass assembly, and places strong constraints on cosmological model. Both observations and theories suggest that structures formation follows a "bottom up" process, in which small, low-mass component form first, and gradually develop into larger, more massive systems. This dissertation focuses on three crucial stages of cosmic structure formation: first generation stars, quasar host galaxies and the

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Bai, Lei. "The Effects of Dense Cluster Environments on Galaxies and Intracluster Dust." Diss., The University of Arizona, 2007. http://hdl.handle.net/10150/193609.

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Dense cluster environment influences the properties of galaxies and their evolution. In order to understand this environmental effect and how it evolves with time, we study the infrared (IR) properties of galaxies in three rich clusters. The IR luminosities provide us with extinction-free measurements of the star formation rates (SFRs) of these cluster galaxies. We find a strong evolution in the IR luminosity function (LF) of two z ∼ 0:8 clusters when compared to two local clusters. The evolution rate of the IR LF found in these clusters is consistent with the evolution in field IR LFs. The si

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Kriwattanawong, Wichean. "The formation and evolution of the galaxy population in the nearby cluster abell 1367." Thesis, Liverpool John Moores University, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.502762.

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Kotze, J. P. "Studying the environmental dependence of star formation properties of galaxies in the Abell 1437 galaxy cluster and its surrounding large scale structure." Doctoral thesis, University of Cape Town, 2014. http://hdl.handle.net/11427/8801.

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Includes bibliographical references.<br>It has become clear that the local galaxy environment plays a crucial role in the evolution of galaxies. Recent studies show a strong bimodal distribution of galaxy properties, with red, passive galaxies dominating the bimodal distribution in dense environments, compared to blue, actively star forming galaxies dominating the bimodal distribution in low density environments. Blue, star-forming galaxies are continuously transformed into red, passive galaxies through one or more processes while being accreted into higher density environments. The processes

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Beuret, Maxime. "Formation stellaire dans la galaxie et interaction avec le milieu interstellaire." Thesis, Strasbourg, 2016. http://www.theses.fr/2016STRAE017/document.

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Comment les étoiles se forment elles ?. Cette vaste question fait appel à des connaissances dans plusieurs domaines dont deux majeurs, la Formation Stellaire et le Milieu Interstellaire. C’est dans ce cadre générale que s’inscrit ma thèse. Notre galaxie est un vaste laboratoire d’études de cette formation et je me suis donc intéressé aux premières étapes de la formation des étoiles, allant du nuage moléculaire à la proto-étoile. J’ai principalement utilisé des données provenant du télescope Herschel qui nous fournit des images et des données dans l’infrarouge lointain et le domaine sub-milimét

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Cao, Orjales Jose Manuel. "A Study of AGN and their environments in the far-infrared." Thesis, University of Hertfordshire, 2014. http://hdl.handle.net/2299/14440.

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My Ph.D. has been composed of work involving the use of far–IR and submm observations of AGN. During this time it has focused on the in- terplay between AGN and their host galaxies and cluster environments. Understanding the role of AGN, and how they affect the evolution of both their host galaxies and surrounding environments, is a pressing concern in cosmological models of the universe, affecting as they do the chemical makeup, star formation rate, and morphology of their host galaxies. In Chapter 2, we focus on attempting to determine whether there is an inherent physical difference between

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Pope, Alexandra, Alfredo Montaña, Andrew Battisti, et al. "Early Science with the Large Millimeter Telescope: Detection of Dust Emission in Multiple Images of a Normal Galaxy at z > 4 Lensed by a Frontier Fields Cluster." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623817.

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We directly detect dust emission in an optically detected, multiply imaged galaxy lensed by the Frontier Fields cluster MACSJ0717.5+3745. We detect two images of the same galaxy at 1.1 mm with the AzTEC camera on the Large Millimeter Telescope leaving no ambiguity in the counterpart identification. This galaxy, MACS0717_Az9, is at z > 4 and the strong lensing model (mu = 7.5) allows us to calculate an intrinsic IR luminosity of 9.7 x 10(10) L-circle dot and an obscured star formation rate of 14.6 +/- 4.5 M-circle dot yr(-1). The unobscured star formation rate from the UV is only 4.1 +/- 0.3 M-

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Belles, Pierre-Emmanuel. "Formation d’étoiles et d’amas stellaires dans les collisions de galaxies." Thesis, Paris 11, 2012. http://www.theses.fr/2012PA112312/document.

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Les fusions sont un évènement essentiel dans la formation des grandes structures de l’Univers; elles jouent un rôle important dans l’histoire de formation et l’évolution des galaxies. Outre une transformation morphologique, les fusions induisent d’importants sursauts de formation d’étoiles. Ces sursauts sont caractérisés par des Efficacités de Formation Stellaire (EFS) et des Taux de Formation Stellaire Spécifiques (TFSS), i.e., respectivement, des Taux de Formation Stellaire (TFS) par unité de masse gazeuse et des TFS par unité de masse stellaire, plus élevés que ceux des galaxies spirales. A

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"Formation of Compact Stellar Clusters by High-Redshift Galaxy Outflows." Doctoral diss., 2012. http://hdl.handle.net/2286/R.I.14653.

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abstract: Using high-resolution three-dimensional adaptive mesh refinement simulations I study the interaction between primordial minihalo, a clump of baryonic and dark matter with a virial temperature below the atomic cooling limit, and a galaxy outflow. In Chapter 2 I concentrate on the formation of molecular coolants and their effect on the evolution of the minihalo gas. Molecular coolants are important since they allow gas to cool below 10000 K. Therefore, I implement a primordial chemistry and cooling network that tracks the evolution and cooling from these species. I show that the shock

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Lu, Ting. "Galaxy Transformations in the Last 5 Billion Years." Thesis, 2010. http://hdl.handle.net/10012/5466.

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It has become clear that the global star formation rate in the Universe has been decreasing since at least z~1, and blue, star-forming galaxies are transformed into red, passive galaxies through one or more processes. The origin of this decline and transformation remains unclear. The role environment plays in all this is especially uncertain. Despite the observed domination of a passive population in the cores of clusters, in contrast to the more actively star-forming field population, whether or not, and how environment affects the properties of galaxies when they fall into clusters is an u

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Rahman, Mubdi. "The Milky Way's Most Luminous Star Clusters: Engines of Galaxy Evolution." Thesis, 2012. http://hdl.handle.net/1807/34857.

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Massive young star clusters and OB associations (M > 10 000 Msun) dominate the energetic feedback from stars into the interstellar medium. They contain the most massive and luminous stars in the Galaxy, which shape their environments through winds, ionizing flux, radiation pressure, and eventually supernovae, destroying their natal molecular clouds and inflating superbubbles. Few such clusters have been identified in our Galaxy. We systematically investigate the most luminous H II regions, which we identify using the WMAP foreground maps. We find that the 13 most luminous sources produce one-t

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Deovrat, *. "AGN Feedback in Galaxy Clisters - Controlling Cooling Flows in Galaxy Clusters by Momentum-driven AGN Jets." Thesis, 2017. http://etd.iisc.ac.in/handle/2005/4219.

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Synopsis According to the hierarchical structure formation model, massive structures like galaxy clusters are formed due to the gravitational collapse of initial density perturbations and their subsequent mergers. As the formation of galaxy clusters is driven by gravity, they are expected to follow self-similar profiles for density, temperature, entropy etc (Kaiser 1986). However, observations show that self-similarity assumption is not followed in clusters due to the presence of cooling and other such non-gravitational processes (Markevitch et al. 1998; Ponman et al. 1999). More than a

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Bildfell, Christopher John. "The Stellar Content in Clusters of Galaxies." Thesis, 2013. http://hdl.handle.net/1828/4562.

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We investigate three separate topics associated with the formation and evolution of the stellar mass component in galaxy clusters. The work presented herein is based primarily on optical imaging and spectra taken with, respectively, the Canada-France-Hawaii Telescope and Gemini North/South. We confront the result from the optical data analysis with the results from the analysis of high-resolution X-ray data taken with the Chandra and XMM-Newton space observatories. Confirming earlier results, we find that 22% of brightest cluster galaxies (BCGs) show central inversions in their optical colo

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Roediger, Joel C. "The Stellar Populations and Evolution of Virgo Cluster Galaxies." Thesis, 2009. http://hdl.handle.net/1974/5087.

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Using a combination of optical and near-infrared photometry, we have studied both the resolved and integrated stellar populations for a sample of Virgo cluster galaxies spanning the full range of galaxian parameters. The derived stellar population properties are compared against galaxy structural and environmental measures to gauge the importance of these factors in establishing galaxy star formation histories and chemical evolution. Although galaxy colours do not uniquely probe a galaxy's star formation history, meaningful results may be obtained if considered in a relative sense. We find tha

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Oman, Kyle Andrew. "Probing the Environmental Dependence of Star Formation in Satellite Galaxies using Orbital Kinematics." Thesis, 2013. http://hdl.handle.net/10012/7840.

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(Abridged) Physical processes regulating star formation in satellite galaxies represent an area of ongoing research, but the projected nature of observed coordinates makes separating different populations of satellites (with different processes at work) difficult. The present-day phase space coordinates of a satellite galaxy carry information about its orbital history, which can then be compared to its star formation history (SFH). This is expected to reveal both a trigger time and timescale for environmental quenching. Finally, this can be related back to the physical process(es) regulating s

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Liu, Fan. "Chemical signatures of planet formation in field and open cluster stars." Phd thesis, 2016. http://hdl.handle.net/1885/106000.

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In this thesis, I have conducted a strictly line-by-line differential abundance analysis using high resolution, high signal-to-noise ratio spectra of field stars (e.g., stellar binaries, terrestrial planet hosts etc.) and open cluster stars (e.g., the Hyades stars) in order to identify the chemical signatures of planet formation. The three main results from this thesis are: First, we present a detailed differential abundance analysis of the HAT-P-1 stellar binary. The secondary star in this double system is known to host a transiting giant planet wh

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Trudeau, Ariane. "Deep radio observations of a high-redshift galaxy cluster." Thèse, 2018. http://hdl.handle.net/1866/21300.

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Opolot, Daniel Christopher. "Infrared-bright galaxies in the millennium simulation and Sunyaev Zeldovich effect contamination." Thesis, 2010. http://hdl.handle.net/11394/3451.

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>Magister Scientiae - MSc<br>Measuring the evolution of the abundance of galaxy clusters puts constraints on cosmological parameters like the cosmological density parameter m, σ8 and the dark energy equation of state parameter, w. Current observations that promise to give large cluster counts and their properties are those that rely on the Sunyaev-Zeldovich effect (SZE) from clusters. We study the contamination of the SZ signals from galaxy clusters by cluster infrared (IR) galaxies and particularly faint IR galaxies. We use the Millennium simulation database to extract galaxy clusters and ded

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