The Search for Dark Matter Annihilation in Galaxy Clusters at VERITAS
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The Puzzling Nature of Dwarf-Sized Gas Poor Disk Galaxies
Dissertation submitted to the Department of Physics Combined Faculties of the Astronomy Division Natural Sciences and Mathematics University of Oulu Ruperto-Carola-University Oulu, Finland Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by Joachim Janz born in: Heidelberg, Germany Public defense: January 25, 2013 in Oulu, Finland THE PUZZLING NATURE OF DWARF-SIZED GAS POOR DISK GALAXIES Preliminary examiners: Pekka Heinämäki Helmut Jerjen Opponent: Laura Ferrarese Joachim Janz: The puzzling nature of dwarf-sized gas poor disk galaxies, c 2012 advisors: Dr. Eija Laurikainen Dr. Thorsten Lisker Prof. Heikki Salo Oulu, 2012 ABSTRACT Early-type dwarf galaxies were originally described as elliptical feature-less galax- ies. However, later disk signatures were revealed in some of them. In fact, it is still disputed whether they follow photometric scaling relations similar to giant elliptical galaxies or whether they are rather formed in transformations of late- type galaxies induced by the galaxy cluster environment. The early-type dwarf galaxies are the most abundant galaxy type in clusters, and their low-mass make them susceptible to processes that let galaxies evolve. Therefore, they are well- suited as probes of galaxy evolution. In this thesis we explore possible relationships and evolutionary links of early- type dwarfs to other galaxy types. We observed a sample of 121 galaxies and obtained deep near-infrared images. For analyzing the morphology of these galaxies, we apply two-dimensional multicomponent fitting to the data. This is done for the first time for a large sample of early-type dwarfs. A large fraction of the galaxies is shown to have complex multicomponent structures. -
X-Ray and Gamma-Ray Variability of NGC 1275
galaxies Article X-ray and Gamma-ray Variability of NGC 1275 Varsha Chitnis 1,*,† , Amit Shukla 2,*,† , K. P. Singh 3 , Jayashree Roy 4 , Sudip Bhattacharyya 5, Sunil Chandra 6 and Gordon Stewart 7 1 Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India 2 Discipline of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India 3 Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, SAS Nagar, Manauli 140306, India; [email protected] 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India; [email protected] 5 Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India; [email protected] 6 Centre for Space Research, North-West University, Potchefstroom 2520, South Africa; [email protected] 7 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK; [email protected] * Correspondence: [email protected] (V.C.); [email protected] (A.S.) † These authors contributed equally to this work. Received: 30 June 2020; Accepted: 24 August 2020; Published: 28 August 2020 Abstract: Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission. -
Books, Magazines and Organizations
Contents 1 Some Background ..................................................................................... 1 The Many Types of Objects ........................................................................ 2 Telescope and Observing Essentials ........................................................... 3 Binoculars or Telescopes? ....................................................................... 3 Magnification .......................................................................................... 5 Resolution ............................................................................................... 8 Limiting Magnitude ................................................................................ 10 Field of View ........................................................................................... 11 Atmospheric Effects ................................................................................ 12 Dark Adaption and Averted Vision ......................................................... 14 Clothing................................................................................................... 16 Recording Observations .......................................................................... 17 The Science of Astronomy .......................................................................... 17 Angular Measurements ........................................................................... 18 Date and Time ......................................................................................... 18 -
Icecube Searches for Neutrinos from Dark Matter Annihilations in the Sun and Cosmic Accelerators
UNIVERSITE´ DE GENEVE` FACULTE´ DES SCIENCES Section de physique Professeur Teresa Montaruli D´epartement de physique nucl´eaireet corpusculaire IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. THESE` pr´esent´ee`ala Facult´edes sciences de l'Universit´ede Gen`eve pour obtenir le grade de Docteur `essciences, mention physique par M. Rameez de Kozhikode, Kerala (India) Th`eseN◦ 4923 GENEVE` 2016 i Declaration of Authorship I, Mohamed Rameez, declare that this thesis titled, 'IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.' and the work presented in it are my own. I confirm that: This work was done wholly or mainly while in candidature for a research degree at this University. Where any part of this thesis has previously been submitted for a degree or any other qualifica- tion at this University or any other institution, this has been clearly stated. Where I have consulted the published work of others, this is always clearly attributed. Where I have quoted from the work of others, the source is always given. With the exception of such quotations, this thesis is entirely my own work. I have acknowledged all main sources of help. Where the thesis is based on work done by myself jointly with others, I have made clear exactly what was done by others and what I have contributed myself. Signed: Date: 27 April 2016 ii UNIVERSITE´ DE GENEVE` Abstract Section de Physique D´epartement de physique nucl´eaireet corpusculaire Doctor of Philosophy IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. -
Why Gravity Cannot Be Quantized Canonically, and What We Can We Do About It
WHY GRAVITY CANNOT BE QUANTIZED CANONICALLY, AND WHAT WE CAN WE DO ABOUT IT Philip D. Mannheim Department of Physics University of Connecticut Presentation at Miami 2013, Fort Lauderdale December 2013 1 GHOST PROBLEMS, UNITARITY OF FOURTH-ORDER THEORIES AND PT QUANTUM MECHANICS 1. P. D. Mannheim and A. Davidson, Fourth order theories without ghosts, January 2000 (arXiv:0001115 [hep-th]). 2. P. D. Mannheim and A. Davidson, Dirac quantization of the Pais-Uhlenbeck fourth order oscillator, Phys. Rev. A 71, 042110 (2005). (0408104 [hep-th]). 3. P. D. Mannheim, Solution to the ghost problem in fourth order derivative theories, Found. Phys. 37, 532 (2007). (arXiv:0608154 [hep-th]). 4. C. M. Bender and P. D. Mannheim, No-ghost theorem for the fourth-order derivative Pais-Uhlenbeck oscillator model, Phys. Rev. Lett. 100, 110402 (2008). (arXiv:0706.0207 [hep-th]). 5. C. M. Bender and P. D. Mannheim, Giving up the ghost, Jour. Phys. A 41, 304018 (2008). (arXiv:0807.2607 [hep-th]) 6. C. M. Bender and P. D. Mannheim, Exactly solvable PT-symmetric Hamiltonian having no Hermitian counterpart, Phys. Rev. D 78, 025022 (2008). (arXiv:0804.4190 [hep-th]) 7. C. M. Bender and P. D. Mannheim, PT symmetry and necessary and sufficient conditions for the reality of energy eigenvalues, Phys. Lett. A 374, 1616 (2010). (arXiv:0902.1365 [hep-th]) 8. P. D. Mannheim, PT symmetry as a necessary and sufficient condition for unitary time evolution, Phil. Trans. Roy. Soc. A. 371, 20120060 (2013). (arXiv:0912.2635 [hep-th]) 9. C. M. Bender and P. D. Mannheim, PT symmetry in relativistic quantum mechanics, Phys. -
Fall 2005 ASTR 1120-001 General Astronomy: Stars & Galaxies
Fall 2005 ASTR 1120-001 General Astronomy: Stars & Galaxies. Problem Set 5. Due Th 17 Nov Your name: Your ID: Except for the tutorial, for which you should submit answers on line, please write your answers on this sheet, and make sure to show your working. Attach extra sheets if you need them. If you mess up, you can get another copy of the problem set at http://casa. colorado.edu/~ajsh/astr1120_05/prob.html. 1. Tutorial on Detecting Dark Matter in Spiral Galaxies Go to http://www.astronomyplace.com, press on the Cosmic Perspective 3rd Edition icon, log in. You should already have joined our class `cm651430', so that you can record your work and submit it for grade on line. Click on Tutorials, and do the tutorial on Detecting Dark Matter in Spiral Galaxies. You can redo the tutorial as often as you like, to improve your grade. Your score should be recorded automatically, but as a double check against your score disappearing into a black hole: My score was . If you like, you can comment here on the tutorial: 1 2. Recession velocity of Per A This is the observed spectrum (Kennicutt 1992) of NGC 1275, also known as Per A, the central galaxy in the Perseus cluster of galaxies. The name Per A is because it's the brightest radio source in the Perseus constellation. (a) Wavelength of Hα Measure, as accurately as you can, the wavelength of the Hα line (Hα is the leftmost of the two close prominent emission lines at the right of the graph). -
Searches for Leptophilic Dark Matter with Astrophysical Experiments
. Searches for leptophilic dark matter with astrophysical experiments . Von der Fakult¨atf¨urMathematik, Informatik und Naturwissenschaften der RWTH Aachen University zur Erlangung des akademischen Grades einer Doktorin der Naturwissenschaften genehmigte Dissertation vorgelegt von M. Sc. Leila Ali Cavasonza aus Finale Ligure, Savona, Italien Berichter: Universit¨atsprofessorDr. rer. nat. Michael Kr¨amer Universit¨atsprofessorDr. rer. nat. Stefan Schael Tag der m¨undlichen Pr¨ufung: 13.05.16 Diese Dissertation ist auf den Internetseiten der Universit¨atsbibliothekonline verf¨ugbar RWTH Aachen University Leila Ali Cavasonza Institut f¨urTheoretische Teilchenphysik und Kosmologie Searches for leptophilic dark matter with astrophysical experiments PhD Thesis February 2016 Supervisors: Prof. Dr. Michael Kr¨amer Prof. Dr. Stefan Schael Zusammenfassung Suche nach leptophilischer dunkler Materie mit astrophysikalischen Experimenten Die Natur der dunklen Materie (DM) zu verstehen ist eines der wichtigsten Ziele der Teilchen- und Astroteilchenphysik. Große experimentelle Anstrengungen werden un- ternommen, um die dunkle Materie nachzuweisen, in der Annahme, dass sie neben der Gravitationswechselwirkung eine weitere Wechselwirkung mit gew¨ohnlicher Materie hat. Die dunkle Materie in unserer Galaxie k¨onnte gew¨ohnliche Teilchen durch An- nihilationsprozesse erzeugen und der kosmischen Strahlung einen zus¨atzlichen Beitrag hinzuf¨ugen.Deswegen sind pr¨aziseMessungen der Fl¨ussekosmischer Strahlung ¨außerst wichtig. Das AMS-02 Experiment misst die -
Gas Density Fluctuations in the Perseus Cluster: Clumping Factor and Velocity Power Spectrum
SLAC-PUB-16739 Mon. Not. R. Astron. Soc. 000, 1{16 (2015) Printed 30 January 2015 (MN LATEX style file v2.2) Gas Density Fluctuations in the Perseus Cluster: Clumping Factor and Velocity Power Spectrum I. Zhuravleva1;2?, E. Churazov3;4, P. Ar´evalo5, A. A. Schekochihin6;7, S. W. Allen1;2;8, A. C. Fabian9, W. R. Forman10, J. S. Sanders11, A. Simionescu12, R. Sunyaev3;4, A. Vikhlinin10, N. Werner1;2 1Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, California 94305-4085, USA 2Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, California 94305-4060, USA 3Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, D-85741 Garching, Germany 4Space Research Institute (IKI), Profsoyuznaya 84/32, Moscow 117997, Russia 5Instituto de F´ısica y Astronom´ıa,Facultad de Ciencias, Universidad de Valpara´ıso,Gran Bretana N 1111, Playa Ancha, Valpara´ıso,Chile 6Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Rd, Oxford OX1 3NP, UK 7Merton College, University of Oxford, Merton St, Oxford OX1 4JD, UK 8SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA 9Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 10Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA 11Max-Planck-Institut f¨urExtraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany 12Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 252-5210, Japan Accepted .... Received ... ABSTRACT X-ray surface brightness fluctuations in the core of the Perseus Cluster are analyzed, using deep observations with the Chandra observatory. -
Analysis of Repulsive Central Universal Force Field on Solar and Galactic
Open Phys. 2019; 17:364–372 Research Article Kamal Barghout* Analysis of repulsive central universal force field on solar and galactic dynamics https://doi.org/10.1515/phys-2019-0041 otic matter-energy to the matter side of Einstein field equa- Received Jun 30, 2018; accepted Apr 02, 2019 tions, dubbed “dark matter” and “dark energy”; see [5] and references therein. Abstract: Recent astrophysical observations hint toward The existence of dark matter is mostly inferred from the need for an extended theory of gravity to explain puz- gravitational effects on visible matter and is thought toac- zles presented by the standard cosmological model such count for approximately 85% of the matter in the universe as the need for dark matter and dark energy to understand while dark energy is inferred from the accelerated expan- the dynamics of the cosmos. This paper investigates the ef- sion of the universe and along with dark matter constitutes fect of a repulsive central universal force field on the be- about 95% of the total mass-energy content in the universe. havior of celestial objects. Negative tidal effect on the solar The origin of dark matter is a mystery and a wide range and galactic orbits, like that experienced by Pioneer space- of theories speculate its type, its particle’s mass, its self- crafts, was derived from the central force and was shown to interaction and its interaction with normal matter. Also, manifest itself as dark matter and dark energy. Vertical os- experiments to directly detect dark matter particles in the cillation of the sun about the galactic plane was modeled lab have failed to produce positive results which presents a as simple harmonic motion driven by the repulsive force. -
Dark Matter Searches Targeting Dwarf Spheroidal Galaxies with the Fermi Large Area Telescope
Doctoral Thesis in Physics Dark Matter searches targeting Dwarf Spheroidal Galaxies with the Fermi Large Area Telescope Maja Garde Lindholm Oskar Klein Centre for Cosmoparticle Physics and Cosmology, Particle Astrophysics and String Theory Department of Physics Stockholm University SE-106 91 Stockholm Stockholm, Sweden 2015 Cover image: Top left: Optical image of the Carina dwarf galaxy. Credit: ESO/G. Bono & CTIO. Top center: Optical image of the Fornax dwarf galaxy. Credit: ESO/Digitized Sky Survey 2. Top right: Optical image of the Sculptor dwarf galaxy. Credit:ESO/Digitized Sky Survey 2. Bottom images are corresponding count maps from the Fermi Large Area Tele- scope. Figures 1.1a, 1.2, 1.3, and 4.2 used with permission. ISBN 978-91-7649-224-6 (pp. i{xxii, 1{120) pp. i{xxii, 1{120 c Maja Garde Lindholm, 2015 Printed by Publit, Stockholm, Sweden, 2015. Typeset in pdfLATEX Abstract In this thesis I present our recent work on gamma-ray searches for dark matter with the Fermi Large Area Telescope (Fermi-LAT). We have tar- geted dwarf spheroidal galaxies since they are very dark matter dominated systems, and we have developed a novel joint likelihood method to com- bine the observations of a set of targets. In the first iteration of the joint likelihood analysis, 10 dwarf spheroidal galaxies are targeted and 2 years of Fermi-LAT data is analyzed. The re- sulting upper limits on the dark matter annihilation cross-section range 26 3 1 from about 10− cm s− for dark matter masses of 5 GeV to about 5 10 23 cm3 s 1 for dark matter masses of 1 TeV, depending on the × − − annihilation channel. -
Proton! Physics Under the Direction of Guido Energy Physics Under the Direction of We’Ll Even Print Your Abstract! Mueller
P R O T O N Physics Report on Things of Note January 2006 -- Vol. 5 No. 1 Physics Department Year-End Awards Announced Featured Publication(s) Each December, the Department holds an Awards Ceremony during the Annual Holiday Party, to recognize staff and faculty who have achieved superior perfor- T. S. Nunner, B. M. Ander- mance, and to announce the Graduate Student Awards which recognize outstand- sen, A. Melikyan, and P. J. ing graduate students from the past year. Hirschfeld. “Dopant-Modulated Pair Physics Teacher of the Year (2005) Interaction in Cuprate Super- Stephen Hill conductors.” Phys. Rev. Lett. 95, 177003 (2005). Physics Employee Excellence Awards (2005) Yvonne Dixon and Greg Labbe B. Abbott et al. (LIGO Scien- tific Collaboration). Graduate Student Awards (2005) “Upper Limits on a Stochastic Background of Gravitational Tom Scott Memorial Award : TA of the Year for the Introductory Waves.” James Ira Thorpe Labs : Sung-Soo Kim Phys. Rev. Lett. 95, 221101 (2005) This award is made annually to a se- This award recognizes Sung-Soo’s nior graduate student, in experimental commitment to his students and to the Submit your article to be featured physics, who has shown distinction in educational atmosphere in the labora- in this section. Whether it’s just research. Ira is a 2nd year graduate tory setting. Sung-Soo is a 4th year been submitted or accepted, we’d student working in experimental astro- student working in theoretical high like to feature it in the proton! physics under the direction of Guido energy physics under the direction of We’ll even print your abstract! Mueller. -
High Resolution Search for Dark Matter Axions in Milky Way Halo Substructure
HIGH RESOLUTION SEARCH FOR DARK MATTER AXIONS IN MILKY WAY HALO SUBSTRUCTURE By LEANNE DELMA DUFFY A DISSERTATION PRESENTED TO THE GRADUATE SCHOOL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY UNIVERSITY OF FLORIDA 2006 ACKNOWLEDGMENTS This work is based on research performed by the Axion Dark Matter eX- periment (ADMX). I am grateful to my ADMX collaborators for their efforts, particularly in running the experiment and providing the high resolution data. Without these efforts, this work would not have been possible. I thank my advisor, Pierre Sikivie, for his support and guidance thoughout graduate school. It has been a priviege to collaborate with him on this and other projects. I also thank Dave Tanner for his assistance and advice on this work. I would like to thank the other members of my advisory committee, Jim Fry, Guenakh Mitselmakher, Pierre Ramond, Richard Woodard and Fred Hamann, for their roles in my progress. I am also grateful to the other members of the University of Florida Physics Department who have contributed to my graduate school experience. I am especially grateful to my family and friends, both near and far, who have supported me through this long endeavor. Special thanks go to Lisa Everett and Ethan Siegel. ii TABLE OF CONTENTS page ACKNOWLEDGMENTS ............................. ii LIST OF TABLES ................................. v LIST OF FIGURES ................................ vi ABSTRACT .................................... viii CHAPTER 1 INTRODUCTION .............................. 1 2 AXIONS .................................... 7 2.1 Introduction ............................... 7 2.2 The Strong CP Problem ........................ 7 2.3 The Axion ................................ 11 2.3.1 Introduction ........................... 11 2.3.2 The Peccei-Quinn Solution to the Strong CP Problem ...