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Dissertations / Theses on the topic 'Dynamics of galaxies'

Author: Grafiati

Published: 4 June 2021

Last updated: 11 March 2023

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1

Huang, S. N. "Dynamics of interacting galaxies." Thesis, University of Manchester, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.378332.

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2

Zaritsky, Dennis Fabian. "The dynamics of satellite galaxies." Diss., The University of Arizona, 1991. http://hdl.handle.net/10150/185639.

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We use the positions and velocities of satellites of our galaxy and of other spiral galaxies to determine the radial mass profile of dark matter halos. We combine our measurement of the velocities of five remote Galactic satellites with published observations of the other Galactic satellites to obtain a complete sample of test particles. We then apply statistical techniques and timing arguments to deduce that the mass of the Galaxy is ≳ 1.3 x 10¹²M(⊙) for standard assumptions and that the halo extends beyond 100 kpc Galactocentric distance. We confirm our result by examining the dynamics of ot

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3

Millington, S. J. C. "Clusters of galaxies." Thesis, University of Oxford, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.382461.

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4

Naab, Thorsten. "Structure and dynamics of interacting galaxies." [S.l. : s.n.], 2000. http://deposit.ddb.de/cgi-bin/dokserv?idn=961763744.

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5

Lüghausen, Fabian [Verfasser]. "Galaxies in Milgromian Dynamics / Fabian Lüghausen." Bonn : Universitäts- und Landesbibliothek Bonn, 2015. http://d-nb.info/1077289189/34.

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6

Newton, A. J. "Distribution functions and dynamics of galaxies." Thesis, University of Oxford, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.371547.

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7

Hargreaves, Julia Catherine. "The dynamics of dwarf spheroidal galaxies." Thesis, University of Cambridge, 1995. https://www.repository.cam.ac.uk/handle/1810/270411.

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8

Yoachim, Peter. "Thick disks in external galaxies /." Thesis, Connect to this title online; UW restricted, 2007. http://hdl.handle.net/1773/5444.

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9

Velázquez, Hector Manuel. "Dynamics of disc galaxies and their satellites." Thesis, University of Cambridge, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.627438.

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10

El-Zant, A. A. "Nonlinear dynamics and the evolution of galaxies." Thesis, University of Sussex, 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.321419.

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It has been customary practice in galactic dynamics to implicitly assume that the corresponding N-body problem is (near) integrable. After a review of some relevant ideas from non-linear dynamics, I discuss the evidence suggesting that the above assumption is not generally satisfied and the consequences of such a situation. Next, I discuss the characterization of such "chaotic" behaviour. A geometric method-which I argue is best suited for measuring the instability properties of N-body systems-is tested on systems of 231 particles integrated with high precision and displaying "obvious" instabi

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11

Prada-Martinez, Francisco. "The physics and dynamics of starburst galaxies." Thesis, Queen's University Belfast, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.282295.

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12

Boardman, Nicholas Fraser. "The dark and luminous structure of early-type galaxies : observational dynamics and stellar populations." Thesis, University of St Andrews, 2018. http://hdl.handle.net/10023/15979.

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Lenticular and elliptical galaxies, collectively referred to as "early-type galaxies" (ETGs), are commonly thought to represent the end-points of galaxy evolution. Lying in the red sequence of galaxies, these objects are defined by their mostly old stellar populations and by their "red and dead" appearance in optical observations. Much progress in understanding these objects has been made with integral-field spectroscopy in recent years, with results repeatedly pointing to a link between early-type galaxies and high-redshift spiral galaxies. However, the exact nature of this link remains uncle

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13

Kristen, Helmuth. "Dynamics of the interstellar matter in galaxies : isolated barred spiral galaxies : cloud formation processes /." Stockholm : Univ, 1998. http://bvbr.bib-bvb.de:8991/F?func=service&doc_library=BVB01&doc_number=008210174&line_number=0001&func_code=DB_RECORDS&service_type=MEDIA.

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14

Lablanche, Pierre-Yves. "Study of the dynamics of barred early type galaxies via numerical simulations." Phd thesis, Université Claude Bernard - Lyon I, 2012. http://tel.archives-ouvertes.fr/tel-00943337.

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Since the 30's and Edwin Hubble's famous classification, galaxies are usually separated in twogroups : the late-type galaxies (LTGs) and the early-type galaxies (ETGs). The LTGs family ismainly made of spiral galaxies (S) while the ETGs family is composed of elliptical (E) and lenticular(S0) galaxies. A morphological study of all these galaxies revealed that around 60% of LTGs and45% of S0 present a bar. It has also been shown that, in the local Universe, galaxies fall into twobig groups : the blue cloud mostly populated by LTGs and the red sequence mainly made of ETGs.Several mechanisms are r

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15

Frank, Bradley Stanton. "The dynamics of molecular gas in nearby galaxies." Doctoral thesis, University of Cape Town, 2013. http://hdl.handle.net/11427/4420.

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16

Mogotsi, Keoikantse Moses. "The star formation and dynamics of nearby galaxies." Doctoral thesis, University of Cape Town, 2016. http://hdl.handle.net/11427/22855.

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A scaling relation between the surface density of star formation and gas in the disks of galaxies has become the basis of our understanding of extragalactic star formation on scales of hundreds of parsecs and larger. This is an empirical law but star formation is a complex process - the presence of gas at sufficiently high densities to collapse and form stars depends on a wide variety of physical processes. These processes can be thought of in terms of the stability of galaxy disks, which is a balance between the gravitational force and competing forces such as the outward force due to pressur

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17

Marinacci, Federico <1983&gt. "Dynamics of the halo gas in disc galaxies." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3743/1/Marinacci_Federico_tesi.pdf.

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This Thesis studies the dynamics of hot and cold gas outside the plane in galaxies like the Milky-Way (extra-planar gas) and focuses on the interaction between disc and halo material. Stationary models for the cold phase of the extra-planar gas are presented. They show that the kinematics of this phase must be influenced by the interaction with an ambient medium that we identify as the hot cosmological corona that surrounds disc galaxies. To study this interaction a novel hydrodynamical code has been implemented and a series of hydrodynamical simulations has been run to investigate the mass

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18

Marinacci, Federico <1983&gt. "Dynamics of the halo gas in disc galaxies." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3743/.

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This Thesis studies the dynamics of hot and cold gas outside the plane in galaxies like the Milky-Way (extra-planar gas) and focuses on the interaction between disc and halo material. Stationary models for the cold phase of the extra-planar gas are presented. They show that the kinematics of this phase must be influenced by the interaction with an ambient medium that we identify as the hot cosmological corona that surrounds disc galaxies. To study this interaction a novel hydrodynamical code has been implemented and a series of hydrodynamical simulations has been run to investigate the mass

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Shao, Yali, Ran Wang, Gareth C. Jones, et al. "Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625774.

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We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 mu m fine structure line emission toward a far-infrared-luminous quasar, ULAS J131911.29+095051.4 at z = 6.13, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution of similar to 0.'' 3, and resolve both the dust continuum and the [C II] line emission on a few kiloparsec scales. The [C II] line emission is more irregular than that of the dust continuum emission, which suggests different distributions between the dust and the [C II]

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Batiste, Merida, Misty C. Bentz, Sandra I. Raimundo, Marianne Vestergaard та Christopher A. Onken. "Recalibration of the MBH–σ⋆ Relation for AGN". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623860.

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We present a recalibration of the M-BH-sigma(star) relation, based on a sample of 16 reverberation-mapped galaxies with newly determined bulge stellar velocity dispersions (sigma(star)) from integral-field spectroscopy (IFS), and a sample of 32 quiescent galaxies with publicly available IFS. For both samples, sigma(star) is determined via two different methods that are popular in the literature, and we provide fits for each sample based on both sets of sigma(star). We find the fit to the active galactic nucleus sample is shallower than the fit to the quiescent galaxy sample, and that the slope

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21

Simons, Raymond C., Susan A. Kassin, Benjamin J. Weiner, et al. "z ∼ 2: An Epoch of Disk Assembly." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624922.

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We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star formation at z similar to 2 to today. Measurements of galaxy rotation velocity V-rot, which quantify ordered motions, and gas velocity dispersion sigma(g), which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift over 0.1 < z < 2.5, spanning 10 Gyr. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported (V-rot > sigma(g)). By z = 2, 50% and 70% of galaxies are rotatio

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22

Parry, Owen Huw. "The morphology and dynamics of galaxies from ʌCDM models". Thesis, Durham University, 2011. http://etheses.dur.ac.uk/3333/.

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The formation and evolution of galaxies is studied using two alternative modelling techniques within the context of the LCDM cosmogony. In particular, we consider the capacity of the models to reproduce the fundamental components and internal structure of galaxies. We begin by outlining the theoretical basis for the study, describing the standard paradigm for structure formation and the details of the modelling techniques we employ. The extent of our current understanding of the processes responsible for morphological transformation is explored and we discuss what the structure of the Milky Wa

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23

Harwood, Jeremy James. "The dynamics and energetics of radio-loud active galaxies." Thesis, University of Hertfordshire, 2014. http://hdl.handle.net/2299/14409.

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In this thesis, I use the new generation of radio interferometer along with X-ray observations to investigate the dynamics and energetics of radio-loud active galaxies which are key to understanding AGN feedback and the evolution of galaxies as a whole. I present new JVLA observations of powerful radio source and use innovative techniques to undertake a detailed analysis of JVLA observations of powerful radio galaxies. I compare two of the most widely used models of spectral ageing, the Kardashev-Pacholczyk and Jaffe-Perola models and also results of the more complex, but potentially more real

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24

Machado, Rubens Eduardo Garcia. "Dynamics of Barred Galaxies in Triaxial Dark Matter Haloes." Universidade de São Paulo, 2010. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-02122011-111155/.

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Cosmological N-body simulations indicate that the dark matter haloes of galaxies should be generally triaxial. Yet, the presence of a baryonic disc is believed to modify the shape of the haloes. The goal of this thesis is to study how bar formation is affected by halo triaxiality and how, in turn, the presence of the bar influences the shape of the halo. We performed a series of collisionless and hydrodynamical numerical simulations, using elliptical discs as initial conditions. Triaxial halos tend to become more spherical and we show that part of the circularisation of the halo is due to disc

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25

Machado, Rubens. "Dynamics of barred galaxies in triaxial dark matter haloes." Aix-Marseille 1, 2010. http://theses.univ-amu.fr.lama.univ-amu.fr/2010AIX11051.pdf.

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Des simulations cosmologiques à N-corps indiquent que les halos de matière noire des galaxies devraient être généralement triaxiaux. Pourtant, on croit que la présence d’un disque baryonique modifie la forme des halos. L’objectif de cette thèse est d’étudier comment la formation des barres est affectée par la triaxialité des halos et comment, à son tour, la présence de la barre influence la forme du halo. Nous réalisons un ensemble de simulations numériques non-collisionnelles et hydrodynamiques, utilisant des disques elliptiques comme conditions initiales. Les halos triaxiaux ont tendance à d

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26

Peñarrubia-Garrido, Jorge M. "Satellite dynamics in spiral galaxies with Dark Matter haloes." [S.l. : s.n.], 2003. http://www.bsz-bw.de/cgi-bin/xvms.cgi?SWB10518993.

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27

Fillmore, James Arthur Goldreich Peter Martin. "A study on the formation and dynamics of galaxies /." Diss., Pasadena, Calif. : California Institute of Technology, 1985. http://resolver.caltech.edu/CaltechETD:etd-09082008-150750.

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28

Tacconi, L. J., R. Genzel, A. Saintonge, et al. "PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627042.

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This paper provides an update of our previous scaling relations between galaxy-integrated molecular gas masses, stellar masses, and star formation rates (SFRs), in the framework of the star formation main sequence (MS), with the main goal of testing for possible systematic effects. For this purpose our new study combines three independent methods of determining molecular gas masses from CO line fluxes, far-infrared dust spectral energy distributions, and similar to 1 mm dust photometry, in a large sample of 1444 star-forming galaxies between z = 0 and 4. The sample covers the stellar mass rang

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29

Simons, Raymond C., Susan A. Kassin, Jonathan R. Trump, et al. "KINEMATIC DOWNSIZING AT z similar to 2." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624072.

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We present results from a survey of the internal kinematics of 49 star-forming galaxies at z similar to 2 in the CANDELS fields with the Keck/MOSFIRE spectrograph, Survey in the near-Infrared of Galaxies with Multiple position Angles (SIGMA). Kinematics (rotation velocity V-rot and gas velocity dispersion sg) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by z similar to 2, massive star-forming galaxies (log M-*/M-circle dot less than or similar to 10.2) have assembled primitive disks: their kinematics are dominated by ro

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30

Zaritsky, Dennis. "Clues to the nature of ultradiffuse galaxies from estimated galaxy velocity dispersions." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/624738.

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We describe how to estimate the velocity dispersions of ultradiffuse galaxies (UDGs) using a previously defined galaxy scaling relationship. The method is accurate for the two UDGs with spectroscopically measured dispersions, as well as for ultracompact galaxies, ultrafaint galaxies, and stellar systems with little or no dark matter. This universality means that the relationship can be applied without further knowledge or prejudice regarding the structure of a galaxy. We then estimate the velocity dispersions of UDGs drawn from two published samples and examine the distribution of total masses

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31

Pearson, Sarah, Gurtina Besla, Mary E. Putman, et al. "Local Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universe." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/617405.

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In this paper, we introduce the Local Volume TiNy Titans sample (LV-TNT), which is a part of a larger body of work on interacting dwarf galaxies: TNT . This LV-TNT sample consists of 10 dwarf galaxy pairs in the Local Universe (< 30 Mpc from Milky Way), which span mass ratios of M-*,M- 1/M-*,M- 2 < 20, projected separations < 100 kpc, and pair member masses of log(M-*/M-aS (TM)) < 9.9. All 10 LV-TNT pairs have resolved synthesis maps of their neutral hydrogen, are located in a range of environments and captured at various interaction stages. This enables us to do a comparative study of the dif

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32

Zhang, Huanian, Dennis Zaritsky, Guangtun Zhu, Brice Ménard, and David W. Hogg. "HYDROGEN EMISSION FROM THE IONIZED GASEOUS HALOS OF LOW-REDSHIFT GALAXIES." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622684.

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Using a sample of nearly half a million galaxies, intersected by over 7 million lines of sight from the Sloan Digital Sky Survey Data Release 12, we trace H alpha + [N II] emission from a galactocentric projected radius, r(p), of 5 kpc to more than 100 kpc. The emission flux surface brightness is alpha r(p) 1.9 +/- 0.4. We obtain consistent results using only the Ha or [N II] flux. We measure a stronger signal for the bluer half of the target sample than for the redder half on small scales, r(p) < 20 kpc. We obtain a 3 sigma detection of H alpha + [N II] emission in the 50-100 kpc r(p) bin. Th

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33

Spencer, Meghin E., Mario Mateo, Matthew G. Walker, and Edward W. Olszewski. "A Multi-epoch Kinematic Study of the Remote Dwarf Spheroidal Galaxy Leo II." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623237.

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We conducted a large spectroscopic survey of 336 red giants in the direction of the Leo II dwarf galaxy using Hectochelle on the Multiple Mirror Telescope, and we conclude that 175 of them are members based on their radial velocities and surface gravities. Of this set, 40 stars have never before been observed spectroscopically. The systemic velocity of the dwarf is 78.3 +/- 0.6 km s(-1) with a velocity dispersion of 7.4 +/- 0.4 km s(-1). We identify one star beyond the tidal radius of Leo II but find no signatures of uniform rotation, kinematic asymmetries, or streams. The stars show a strong

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34

Collins, Michelle L. M., Erik J. Tollerud, David J. Sand, Ana Bonaca, Beth Willman, and Jay Strader. "Dynamical evidence for a strong tidal interaction between the Milky Way and its satellite, Leo V." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623924.

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We present a chemodynamical analysis of the Leo V dwarf galaxy, based on the Keck II DEIMOS spectra of eight member stars. We find a systemic velocity for the system of nu(r) = 170.9(+2.1) (-1.9) km s(-1) and barely resolve a velocity dispersion for the system, with sigma nu(r) = 2.3(+3.2) (-1.6) km s(-1), consistent with previous studies of Leo V. The poorly resolved dispersion means we are unable to adequately constrain the dark-matter content of Leo V. We find an average metallicity for the dwarf of [ Fe/ H] =-2.48 +/- 0.21 and measure a significant spread in the iron abundance of its membe

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35

Mullin, Laura May. "Energy transport and dynamics of jets in FRII radio galaxies." Thesis, University of Cambridge, 2006. https://www.repository.cam.ac.uk/handle/1810/252006.

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36

Beifiori, Alessandra. "Dynamics induced by the central supermassive black holes in galaxies." Doctoral thesis, Università degli studi di Padova, 2010. http://hdl.handle.net/11577/3422248.

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In this thesis we focused on the determination of the mass (MBH) of supermassive black hole (SMBHs) and on the interpretation of their demography. We studied their scaling relations with the aim of understanding the role of SMBHs in the evolution of galaxies. This was done by increasing the demography of MBH and studying whether MBH results more closely linked to the bulge or to the global galaxy properties, including the dark matter halo. In the first part of the thesis we focused on the presentation of a spectral and imaging atlas of a large and various sample of galaxies we studied t

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Mendez, Abreu Jairo. "Structure and dynamics of the central regions of disk galaxies." Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3426747.

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In this thesis, we focus on the structural components observed in the central regions of disk galaxies, namely bulges and bars. We aim to better understand the formation and evolution scenarios which could lead to the bulges and bars observed in the nearby universe. This study was performed from an observational point of view, by analyzing either the structural and photometric properties of bulges and bars, their kinematics, and stellar population characteristics.

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Tribble, Peter C. "Hot gas and magnetic fields in clusters of galaxies." Thesis, University of Oxford, 1989. http://ora.ox.ac.uk/objects/uuid:2e46d7ad-c41d-4957-b404-a1cbc22c1d3b.

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Many clusters of galaxies contain large quantities of hot diffuse gas. I have studied the properties of waves in this gas using Lagrangian perturbations. The gas is far more thermally stable than is commonly thought. For bremsstrahlung cooling, all modes that remain oscillatory are damped. Galaxy motions, especially the oscillations of a central cD galaxy, are an important way of generating large amplitude waves in cluster gas. This is especially pertinent in view of the growing realization that cD galaxies are not at rest with respect to the cluster. I also present evidence that weak magnetic

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Williams, Michael J. "Early-type disk galaxies." Thesis, University of Oxford, 2011. http://ora.ox.ac.uk/objects/uuid:936168ab-f49a-410a-9e1b-80c7ad7cf556.

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In this thesis I investigate the dynamics and stellar populations of a sample of 28 edge-on early-type (S0--Sb) disk galaxies, 22 of which host a boxy or peanut-shaped bulge. I begin by constructing mass models of the galaxies based on their observed photometry and stellar kinematics. Subject to cosmologically motivated assumptions about the shape of dark haloes, I measure in a purely dynamical way their stellar and dark masses. I make a preliminary comparison between the dynamically determined stellar masses and those predicted by stellar population models. I then compare the Tully-Fisher (lu

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Donner, Ralf. "Numerical methods of resonant dynamics for the Galaxy." Thesis, University of Oxford, 2005. http://ora.ox.ac.uk/objects/uuid:136ae026-e3d4-4153-b124-edc8256c14c9.

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Numerical methods of resonant dynamics with applications to the Galaxy are considered in this thesis. We derive generating functions for first-order perturbation theory and the associated orbital frequencies by matrix calculus. For two action-angle spaces (J,θ) and (i,φ) related by a canonical map I·φ+s, we show that J can be averaged over ergodic orbits φ to provide an estimator of I to within O(|s|<sup>2</sup>). We provide examples in one and two dimensions and compare the technique to calculations of actions by numerical line integration in Poincaré sections. We then use spectral dynamics a

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Faber, Nicolas Boily Christian M. Portegies Zwart Simon. "Orbital complexity in Hamiltonian dynamics." Strasbourg : Université de Starsbourg, 2009. http://eprints-scd-ulp.u-strasbg.fr:8080/secure/00001111/01/FABER_Nicolas_2008-restrict.pdf.

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Thèse de doctorat : Astrophysique : Strasbourg 1 : 2008. Thèse de doctorat : Astrophysics : Universiteit van Amsterdam, Nederland : 2008.<br>Thèse soutenue sur un ensemble de travaux. Thèse soutenue en co-tutelle. Titre provenant de l'écran-titre. Notes bibliogr.

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Vine, Stephen Gary. "Dynamics of dark and visible matter in galaxies : simulations and observations." Thesis, University of Cambridge, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.624972.

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Blecha, Laura Elizabeth. "The Dynamics and Evolution of Supermassive Black Holes in Merging Galaxies." Thesis, Harvard University, 2012. http://dissertations.umi.com/gsas.harvard:10257.

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This thesis is a theoretical study of supermassive black holes (SMBHs) in merging galaxies. We consider the dynamics that govern inspiralling SMBH pairs and gravitational-wave (GW) recoiling SMBHs, as well as the fueling of active galactic nuclei (AGN) during galaxy mergers. In particular, we focus on the observable signatures that could distinguish dual or recoiling AGN from those in isolated galaxies, and we explore the implications of these events for the coordinated evolution of SMBHs and galaxies. In the second and third chapters, semi-analytical models for GW-recoiling SMBHs are develope

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Faber, Nicolas. "Orbital complexity in Hamiltonian dynamics." Université Louis Pasteur (Strasbourg) (1971-2008), 2008. https://publication-theses.unistra.fr/restreint/theses_doctorat/2008/FABER_Nicolas_2008.pdf.

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L’observation d’un phénomène physique s’appuie en général sur l’évolution d’une observable en fonction du temps. Une telle série temporelle contient les informations de base sur l’état du système étudié. Dans cette thèse, nous exploitons ce concept afin d’explorer l’évolution dynamique complexe qui peut avoir lieu dans les systèmes autogravitants Hamiltoniens. Nous traitons les coordonnées dans l’espace des phases des corps célestes comme des signaux, que nous analysons par la suite en utilisant différentes méthodes de traitement du signal, plus particulièrement la fonction d’autocorrélation e

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Spencer, Meghin E., Mario Mateo, Matthew G. Walker, et al. "The Binary Fraction of Stars in Dwarf Galaxies: The Case of Leo II." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624447.

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We combine precision radial velocity data from four different published works of the stars in the Leo II dwarf spheroidal galaxy. This yields a data set that spans 19 years, has 14 different epochs of observation, and contains 372 unique red giant branch stars, 196 of which have repeat observations. Using this multi-epoch data set, we constrain the binary fraction for Leo II. We generate a suite of Monte Carlo simulations that test different binary fractions using Bayesian analysis and determine that the binary fraction for Leo II ranges from 0.30(-0.10)(+0.09) to 0.34(-0.11)(+0.11), depending

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Manos, Athanasios. "A study of hamiltonian dynamics with applications to models of barred galaxies." Aix-Marseille 1, 2008. http://www.theses.fr/2008AIX11080.

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Cette thèse aborde des questions et présente de résultats qui exigent la combinaison des deux disciplines: d’une part, nous souhaitons comprendre et développer des outils fondamentaux des systèmes hamiltoniens et d’autre part nous envisageons de les utiliser pour étudier la dynamique de certains modèles de galaxies barrées. Pour cette raison, nous allons commencer par étudier d’importants phénomènes dynamiques concernant la stabilité des oscillations périodiques dans les systèmes hamiltoniens à N degrés de liberté ainsi que les applications N–symplectiques couplées. Ensuite, nous allons étendr

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Sormani, Mattia Carlo. "Understanding the large-scale dynamics of the interstellar medium in barred galaxies." Thesis, University of Oxford, 2015. https://ora.ox.ac.uk/objects/uuid:a8ea1747-86c0-4f56-bbc1-e345b5a6481d.

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Abstract:

We study the large-scale dynamics of the interstellar medium in barred galaxies. The interest in doing this is two-fold. On the one hand, the hydrodynamic flow is the source of many interesting physical phenomena, such as shocks and spiral arms. On the other hand, it is a powerful tool to constrain the characteristics of individual galaxies. Approximately half of this thesis is devoted to understanding the general characteristics of the gas dynamics. There are two key ingredients. The first is ballistic closed orbits. We investigate the connection between closed orbits and the full hydrodynami

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Besla, Gurtina, David Martínez-Delgado, der Marel Roeland P. van, et al. "LOW SURFACE BRIGHTNESS IMAGING OF THE MAGELLANIC SYSTEM: IMPRINTS OF TIDAL INTERACTIONS BETWEEN THE CLOUDS IN THE STELLAR PERIPHERY." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621396.

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We present deep optical images of the Large and Small Magellanic Clouds (LMC and SMC) using a low cost telephoto lens with a wide field of view to explore stellar substructure in the outskirts of the stellar disk of the LMC (< 10 degrees from the LMC center). These data have higher resolution than existing star count maps, and highlight the existence of stellar arcs and multiple spiral arms in the northern periphery, with no comparable counterparts in the south. We compare these data to detailed simulations of the LMC disk outskirts, following interactions with its low mass companion, the SMC.

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Balestra, I., A. Mercurio, B. Sartoris, et al. "CLASH-VLT: DISSECTING THE FRONTIER FIELDS GALAXY CLUSTER MACS J0416.1-2403 WITH ∼800 SPECTRA OF MEMBER GALAXIES." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621406.

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We present VIMOS-Very Large Telescope (VLT) spectroscopy of the Frontier Fields cluster MACS. J0416.1-2403 (z = 0.397). Taken as part of the CLASH-VLT survey, the large spectroscopic campaign provided more than 4000 reliable redshifts over similar to 600 arcmin(2), including similar to 800 cluster member galaxies. The unprecedented sample of cluster members at this redshift allows us to perform a highly detailed dynamical and structural analysis of the cluster out to similar to 2.2 r(200) (similar to 4Mpc). Our analysis of substructures reveals a complex system composed of a main massive clust

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Zahedy, Fakhri S., Hsiao-Wen Chen, Michael Rauch, Michelle L. Wilson, and Ann Zabludoff. "Probing the cool interstellar and circumgalactic gas of three massive lensing galaxies at z = 0.4–0.7." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/614764.

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We present multisightline absorption spectroscopy of cool gas around three lensing galaxies at z = 0.4-0.7. These lenses have half-light radii r(e) = 2.6-8 kpc and stellar masses of log M-*/M-circle dot = 10.9-11.4, and therefore resemble nearby passive elliptical galaxies. The lensed QSO sightlines presented here occur at projected distances of d = 3-15 kpc (or d approximate to 1-2 r(e)) from the lensing galaxies, providing for the first time an opportunity to probe both interstellar gas at r similar to r(e) and circumgalactic gas at larger radii r >> r(e) of these distant quiescent galaxies.

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