DOCSLIB.ORG

The Extragalactic Distance Scale

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Extragalactic Distance Scale The Extragalactic Distance Scale The Cepheid Distance Scale and its Application to the Absolute Calibration of the Luminosity { Linewidth Relation A thesis presented by Lucas Mat´ıasMacri to The Department of Astronomy in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the subject of Astronomy Harvard University Cambridge, Massachusetts September 2001 c 2001, by Lucas Mat´ıasMacri All Rights Reserved ii The Extragalactic Distance Scale The Cepheid Distance Scale and its Application to the Absolute Calibration of the Luminosity { Linewidth Relation Advisor: John P. Huchra Lucas Mat´ıasMacri Abstract This Thesis presents research into several topics related to the Extragalactic Distance Scale; in particular, the Cepheid Period { Luminosity Relation and the Luminosity { Linewidth relation for spiral galaxies. The primary distance indicator of choice in the Local Supercluster is the Cepheid Period { Luminosity Relation. While its absolute calibration is still uncertain at the 10% level, it can yield precise relative distances. I present the discovery of Cepheids in, and the determination of distances to, two galaxies in the Local Supercluster: M33 and NGC 2841. I also present a test of the standard extinction law in other galaxies using near-infrared observations of Cepheids. One of the most-widely used secondary distance indicators for extragalactic work is the luminosity { linewidth relation of spiral galaxies, commonly referred to as the Tully { Fisher relation. I present a complete and consistent database of optical and infrared magnitudes of spiral galaxies that are suitable for the absolute calibration of that relation, and I perform that calibration in the RIHK bands. iii iv Contents Abstract . iii Table of Contents . v List of Figures . ix List of Tables . xiii Acknowledgments . xv Citations to Previously Published Work . xvii 1 Introduction and Summary 1 1.1 Structure of this thesis . 1 1.2 The Cepheid Distance Scale . 2 1.2.1 A historical introduction to Cepheid variables . 2 1.2.2 A modern introduction to Cepheid variables . 8 1.3 The Tully-Fisher relation . 15 2 A Cepheid distance to M33 21 2.1 Introduction . 22 2.2 Observations and data reduction . 23 2.3 Photometry . 26 2.3.1 Initial Processing . 26 2.3.2 Photometry of template images . 27 2.3.3 Photometry of individual frames . 28 2.3.4 Determination of aperture correction coefficients . 28 v 2.3.5 Standard star observations and photometric solutions . 30 2.3.6 Photometric comparisons . 32 2.3.7 Artificial star tests . 35 2.4 The star catalog . 39 2.5 Variable search and classification . 42 2.5.1 Previously-known variables in M33 . 74 2.6 A Cepheid Distance to M33 . 75 2.6.1 The P-L relation of LMC Cepheids . 79 2.6.2 Extinction corrections . 81 2.6.3 Blending bias . 86 2.6.4 The metallicity dependence of the P-L relation . 94 2.6.5 The distance to the LMC . 97 2.6.6 An absolute distance to M33 . 99 3 A Cepheid distance to NGC 2841 101 3.1 Introduction . 102 3.2 Observations and Data Reduction . 102 3.3 Photometry and Calibration . 103 3.4 The Cepheids found in NGC 2841 . 111 3.5 Period-Luminosity Relations and Distance Moduli . 113 3.5.1 Methodology . 113 3.5.2 Distance moduli . 133 3.5.3 Metallicity correction . 136 3.5.4 Error Budget . 136 3.6 Discussion . 138 3.7 Conclusions . 140 4 Infrared observations of extragalactic Cepheids 143 4.1 Introduction . 144 vi 4.2 Observations and Data Reduction . 145 4.2.1 Observations . 145 4.2.2 Data reduction . 146 4.3 Photometry . 148 4.3.1 Technique . 148 4.3.2 Absolute photometric calibrations . 149 4.3.3 Photometric recovery tests . 152 4.3.4 Photometry checks . 153 4.4 The Cepheid sample . 157 4.4.1 Sample selection and identification . 157 4.4.2 Period-Luminosity relations . 174 4.4.3 Observed distance moduli . 174 4.5 Blending effects in M101 Inner . 175 4.6 Consistency of reddening determinations . 191 4.6.1 Predicted relation between E(V{I) and E(V{H) . 191 4.6.2 Observed relation . 192 4.7 Summary . 196 5 Optical and infrared observations of Tully-Fisher calibrators 197 5.1 Introduction . 198 5.2 Optical observations and data reduction . 199 5.3 Infrared observations and data reduction . 201 5.4 Galaxy photometry . 204 5.4.1 Surface photometry measurements . 204 5.4.2 Photometry results and external comparisons . 212 5.5 21-cm linewidths . 215 5.6 Conclusions . 216 6 The absolute calibration of the luminosity{linewidth relation 219 vii 6.1 Introduction . 220 6.2 The calibrator sample . 221 6.3 Analysis . 222 6.4 An application to 2MASS data . 227 6.5 Conclusion . 230 viii List of Figures 1.1 Light and radial velocity curves of δ Cephei . 4 1.2 P-L relation of SMC Cepheids . 6 1.3 Evolutionary track of a 7M star . 9 1.4 P-L tracks for Cepheids of different masses . 14 1.5 The original B- and H-band line width-luminosity relations . 16 2.1 Location of DIRECT M33 fields . 24 2.2 Mosaic of DIRECT M33 fields . 25 2.3 Histogram of seeing values in our frames . 29 2.4 Growth curve corrections . 31 2.5 Test of the internal consistency of our photometry . 34 2.6 Test of the external consistency of our photometry . 36 2.7 Artificial star tests . 37 2.8 Cumulative luminosity functions . 40 2.9 Color-magnitude diagram of 56950 stars in M33 . 41 2.10 Phase coverage as a function of period . 43 2.11 Representative Cepheid light curves . 46 2.12 Representative eclipsing binary light curves . 47 2.13 Representative miscellaneous variable light curves . 48 2.14 Color-magnitude diagram of 682 variables in M33 . 72 2.15 Observed I-band P-L relation for all Cepheids . 73 2.16 LMC Cepheid P-L relations . 80 ix 2.17 Interstellar extinction curves . 83 2.18 Determination of the extinction towards a Cepheid . 83 2.19 Effect of blends on Cepheid colors . 84 2.20 Blending data for 91 Cepheids in our sample . 87 2.21 V and I P-L relations of 61 Cepheids in M33 . 90 2.22 Distribution of ∆µ0 vs. P for 61 Cepheids with V & I data . 91 2.23 Distribution of ∆µ0 vs. P for 20 Cepheids with B, V & I data . 93 2.24 Distribution of ∆µ0 vs. r for 20 Cepheids with B, V & I data. 96 3.1 Ground-based image of NGC 2841 . 105 3.2 Mosaic of the WFPC2 field of view of NGC 2841 . 106 3.3 Medianed images of the four WFPC2 chips . 114-117 3.4 Individual finding charts for the variables . 118 3.5 V and I light curves for the variables . 119-123 3.6 Color-magnitude diagram for the stars detected in our images . 124 3.7 Observed differential luminosity functions . 125 3.8 V-band P-L relation for the selected Cepheids in our sample . 134 3.9 I-band P-L relation for the selected Cepheids in our sample . 135 3.10 Distribution of Leo Cloud & Spur galaxies . 141 4.1 Growth curves for the NICMOS bandpasses . 150 4.2 Photometric recovery tests . 154-155 4.3 External photometry comparison . 159 4.4 Astrometric selection of candidates . 161 4.5 Color-color selection of candidates . 162-163 4.6 Images of the fields . 164-169 4.7 Individual finding charts . 170-171 4.8 Near-IR P-L relations . 176-181 4.9 Optical P-L relations . 182-186 x 4.10 Simulated M101 Inner fields . 188 4.11 P-L relations from simulated M101 Inner fields . ..
Load more

Recommended publications
  • Requirements of Timely Performance in Time and Voyage Charterparties
    Graduate School REQUIREMENTS OF TIMELY PERFORMANCE IN TIME AND VOYAGE CHARTERPARTIES - AN EXPLORATION OF THEIR IDENTITY, SCOPE AND LIMITATIONS UNDER ENGLISH LAW Thesis submitted for the degree of Doctor of Philosophy at the University of Leicester by Tamaraudoubra Tom Egbe School of Law University of Leicester 2019 Abstract REQUIREMENTS OF TIMELY PERFORMANCE IN TIME AND VOYAGE CHARTERPARTIES - AN EXPLORATION OF THEIR IDENTITY, SCOPE AND LIMITATIONS UNDER ENGLISH LAW By Tamaraudoubra Tom Egbe The importance of time in the performance of contractual obligations under sea carriage of goods arrangements are until now little explored. For the avoidance of breach, certain obligations and responsibilities of the parties to the contract need to be performed promptly. Ocean transport is an expensive venture and a shipowner could suffer considerable financial losses if an unnecessary but serious delay interrupt the vessel’s earning power in the course of the charterer’s performance of his contractual obligation. On the other hand, a charterer could also incur a substantial loss if arrangements for the shipment and receipt of cargo fail to go according to plan as a result of the shipowner’s failure to perform his charterparty obligation timely and with reasonable diligence. With these considerations in mind, this thesis critically explores the concept of timely performance in the discharge of the contractual obligations of parties to a contract of carriage. While the thesis is not an expository of the occurrence of time in all the obligations of parties to the carriage contract, it focusses particularly on the identity, scope, and limitations of timeliness in the context of timely payment of hire, laytime and reasonable despatch.
    [Show full text]
  • Arxiv:Astro-Ph/0304318V1 16 Apr 2003
    The Globular Cluster Luminosity Function: New Progress in Understanding an Old Distance Indicator Tom Richtler Astronomy Group, Departamento de F´ısica, Universidad de Concepci´on, Casilla 160-C, Concepci´on, Chile Abstract. I review the Globular Cluster Luminosity Function (GCLF) with emphasis on recent observational data and theoretical progress. As is well known, the turn-over magnitude (TOM) is a good distance indicator for early-type galaxies within the limits set by data quality and sufficient number of objects. A comparison with distances derived from surface brightness fluctuations with the available TOMs in the V-band reveals, however, many discrepant cases. These cases often violate the condition that the TOM should only be used as a distance indicator in old globular cluster systems. The existence of intermediate age-populations in early-type galaxies likely is the cause of many of these discrepancies. The connection between the luminosity functions of young and old cluster systems is discussed on the basis of modelling the dynamical evolution of cluster systems. Finally, I briefly present the current ideas of why such a universal structure as the GCLF exists. 1 Introduction: What is the Globular Cluster Luminosity Function? Since the era of Shapley, who first explored the size of the Galaxy, the distances to globular clusters often set landmarks in establishing first the galactic, then the extragalactic distance scale. Among the methods which have been developed to determine the distances of early-type galaxies, the usage of globular clusters is one of the oldest, if not the oldest. Baum [5] first compared the brightness of the brightest globular clusters in M87 to those of M31.
    [Show full text]
  • Vssc163 Draftv3 IBVS 2 Colour Correct Graph.Pmd
    British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 163, March 2015 Contents IBVS 6080 – 6109 - J. Simpson ............................................... inside front cover From the Director - R. Pickard ........................................................................... 3 Polar V1432 Aquilae - Editor’s Note .................................................................. 4 Eclipsing Binary News - D. Loughney .............................................................. 4 Update on the Campaign to Observe the Dwarf Nova CSS 121005:212625+201948 - J. Shears ............... 6 How Variable Stars get Their Names - D. Griffin .............................................. 9 References to Naming of Variable Stars - D. Griffin ........................................ 11 The Discovery of Three New Variable Stars using the Bradford Robotic Telescope and the Software Package Muniwin - D. Conner .................. 12 FY Librae - a First Look at the Behaviour during 2014 - P. Williams .............. 16 FY Librae goes Active and Reaffirms the Howarth and Bailey Formula - J. Toone .............. 18 Refining the Period of V505 Scuti - I. Miller ................................................... 21 Binocular Programme - M. Taylor ................................................................... 21 Eclipsing Binary Predictions – Where to Find Them - D. Loughney .............. 22 Charges for Section Publications .............................................. inside back cover Guidelines for Contributing to the Circular .............................
    [Show full text]
  • 1. Introduction
    THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other.
    [Show full text]
  • Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae
    Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Gallagher, Joseph S., Peter M. Garnavich, Perry Berlind, Peter Challis, Saurabh Jha, and Robert P. Kirshner. 2005. “Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae.” The Astrophysical Journal 634 (1): 210–26. https:// doi.org/10.1086/491664. Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41399918 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 634:210–226, 2005 November 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. CHEMISTRY AND STAR FORMATION IN THE HOST GALAXIES OF TYPE Ia SUPERNOVAE Joseph S. Gallagher and Peter M. Garnavich Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670 Perry Berlind F. L. Whipple Observatory, 670 Mount Hopkins Road, P.O. Box 97, Amado, AZ 85645 Peter Challis Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Saurabh Jha Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411 and Robert P. Kirshner Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Received 2005 March 4; accepted 2005 July 22 ABSTRACT We study the effect of environment on the properties of Type Ia supernovae by analyzing the integrated spectra of 57 local Type Ia supernova host galaxies.
    [Show full text]
  • Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications
    Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC.
    [Show full text]
  • CONSTELLATION TRIANGULUM, the TRIANGLE Triangulum Is a Small Constellation in the Northern Sky
    CONSTELLATION TRIANGULUM, THE TRIANGLE Triangulum is a small constellation in the northern sky. Its name is Latin for "triangle", derived from its three brightest stars, which form a long and narrow triangle. Known to the ancient Babylonians and Greeks, Triangulum was one of the 48 constellations listed by the 2nd century astronomer Ptolemy. The celestial cartographers Johann Bayer and John Flamsteed catalogued the constellation's stars, giving six of them Bayer designations. The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within Triangulum's boundaries. HISTORY AND MYTHOLOGY In the Babylonian star catalogues, Triangulum, together with Gamma Andromedae, formed the constellation known as MULAPIN "The Plough". It is notable as the first constellation presented on (and giving its name to) a pair of tablets containing canonical star lists that were compiled around 1000 BC, the MUL.APIN. The Plough was the first constellation of the "Way of Enlil"—that is, the northernmost quarter of the Sun's path, which corresponds to the 45 days on either side of summer solstice. Its first appearance in the pre-dawn sky (heliacal rising) in February marked the time to begin spring ploughing in Mesopotamia.
    [Show full text]
  • Nature. Vol. XI, No. 277 February 18, 1875
    Nature. Vol. XI, No. 277 February 18, 1875 London: Macmillan Journals, February 18, 1875 https://digital.library.wisc.edu/1711.dl/LBXITYVRTMAPI83 Based on date of publication, this material is presumed to be in the public domain. For information on re-use, see: http://digital.library.wisc.edu/1711.dl/Copyright The libraries provide public access to a wide range of material, including online exhibits, digitized collections, archival finding aids, our catalog, online articles, and a growing range of materials in many media. When possible, we provide rights information in catalog records, finding aids, and other metadata that accompanies collections or items. However, it is always the user's obligation to evaluate copyright and rights issues in light of their own use. 728 State Street | Madison, Wisconsin 53706 | library.wisc.edu NATURE 301 SO The meeting was altogether a remarkable one consist THURSDAY, ° . ’ - FEBRUARY 18, 1875 Ing as it did of two of her Majesty’s Ministers, together ee . _—_ with many of the most eminent men of science in the as I country ; and their . unanimity . in . favour of the proposal is THE LOAN COLLECTION OF SCIENTIFIC | a Proof of its high importance, and we hope a guarantee INSTRUMENTS of its success, WE do not think we are going too far in assuming no stepe rd Teng 2 ee elt the wonder is that that the unusually influential meeting held at we, now been taken to organise a South Kensington last Saturday may be regarded as the Mogan fer Sues anon ofthe Physical, Chemical, and first and a very emphatic step in a most important work, | “&CHat Rann tue recommendations con- What the nature of that meeting was will be seen from life Inemeiee ot ae ee the comm of Sei on Scien- .
    [Show full text]
  • Effemeridi Astronomiche (Di Milano) Dall'ab. A. De Cesaris [And Others]
    Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali.
    [Show full text]
  • The Transfiguration in the Theology of Gregory Palamas And
    Duquesne University Duquesne Scholarship Collection Electronic Theses and Dissertations Spring 2015 Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology Cory Hayes Follow this and additional works at: https://dsc.duq.edu/etd Recommended Citation Hayes, C. (2015). Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology (Doctoral dissertation, Duquesne University). Retrieved from https://dsc.duq.edu/etd/640 This Immediate Access is brought to you for free and open access by Duquesne Scholarship Collection. It has been accepted for inclusion in Electronic Theses and Dissertations by an authorized administrator of Duquesne Scholarship Collection. For more information, please contact [email protected]. DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY A Dissertation Submitted to the McAnulty Graduate School of Liberal Arts Duquesne University In partial fulfillment of the requirements for the degree of Doctor of Philosophy By Cory J. Hayes May 2015 Copyright by Cory J. Hayes 2015 DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY By Cory J. Hayes Approved March 31, 2015 _______________________________ ______________________________ Dr. Bogdan Bucur Dr. Radu Bordeianu Associate Professor of Theology Associate Professor of Theology (Committee Chair) (Committee Member) _______________________________ Dr. Christiaan Kappes Professor of Liturgy and Patristics Saints Cyril and Methodius Byzantine Catholic Seminary (Committee Member) ________________________________ ______________________________ Dr. James Swindal Dr.
    [Show full text]
  • Lucan's Natural Questions: Landscape and Geography in the Bellum Civile Laura Zientek a Dissertation Submitted in Partial Fulf
    Lucan’s Natural Questions: Landscape and Geography in the Bellum Civile Laura Zientek A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Washington 2014 Reading Committee: Catherine Connors, Chair Alain Gowing Stephen Hinds Program Authorized to Offer Degree: Classics © Copyright 2014 Laura Zientek University of Washington Abstract Lucan’s Natural Questions: Landscape and Geography in the Bellum Civile Laura Zientek Chair of the Supervisory Committee: Professor Catherine Connors Department of Classics This dissertation is an analysis of the role of landscape and the natural world in Lucan’s Bellum Civile. I investigate digressions and excurses on mountains, rivers, and certain myths associated aetiologically with the land, and demonstrate how Stoic physics and cosmology – in particular the concepts of cosmic (dis)order, collapse, and conflagration – play a role in the way Lucan writes about the landscape in the context of a civil war poem. Building on previous analyses of the Bellum Civile that provide background on its literary context (Ahl, 1976), on Lucan’s poetic technique (Masters, 1992), and on landscape in Roman literature (Spencer, 2010), I approach Lucan’s depiction of the natural world by focusing on the mutual effect of humanity and landscape on each other. Thus, hardships posed by the land against characters like Caesar and Cato, gloomy and threatening atmospheres, and dangerous or unusual weather phenomena all have places in my study. I also explore how Lucan’s landscapes engage with the tropes of the locus amoenus or horridus (Schiesaro, 2006) and elements of the sublime (Day, 2013).
    [Show full text]
  • Classification of Galaxies Using Fractal Dimensions
    UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted.
    [Show full text]