|
|
- Ronald Sanders
- 8 years ago
- Views:
Transcription
1 WIMP dark matter and the isotropic radio signal Roberto A. Lineros R. Instituto de Física Corpuscular - CSIC/U.
2 Outline Introduction Cosmic ray propagation Synchrotron emission Radio - galactic - extragalactic Conclusions 2
3 A little of history 1933: Fritz Zwicky postulated dark matter in order to explain Coma cluster dynamics as a bound system 3
4 A little of history 4
5 A little of history Coma Galaxy Cluster Virial Theorem Fritz Zwicky Dunkle Materie 5
6 A little of history 60's 70's Vera Rubin studied rotation curves of edge-on galaxies 6
7 Dark Matter Observations support Dark Matter at: Galactic scales Galaxy clusters scales Cosmological scales 7
8 Galactic scales Rotation curve Weak lensing Velocity dispersion of satellite galaxies Velocity dispersion of dsphs Galaxy cluster scales Velocity dispersion of individual galaxies Strong and weak lensing Peculiar velocity flows X-ray emission Cosmological scales CMB anisotropies Growth of structure LSS distribution BAOs SZ effect 8
9 The Standard Model 9
10 The Standard Model Dark Matter 10
11 Dark Matter particle Massive Non baryonic Electrically neutral (*) Stable (**) 11
12 Dark Matter particle Massive Non baryonic Electrically neutral (*) Stable (**) (*) Except Milicharged DM or CHAMPs (**) DM lifetime larger than 10²⁷ seconds (Universe = 10¹⁷ seconds) 12
13 Candidates Adapted from arxiv: Dark Matter 13
14 WIMPs Weakly Interactive Massive Particles 14
15 Candidates Adapted from arxiv: Dark Matter 15
16 WIMPs Big Bang Thermal relic Correct relic abundance for <σv> ~ 1 pb c Mass in GeV-TeV range For WIMPs: 16
17 WIMP Searches D S D D direct detection indirect detection D S S S D D relic abundance S D particle collider astrophysical probes S D D D 17
18 Indirect DM search D S D S Astrophysical activity SM particles Photons Neutrinos Cosmic rays Stable particles Astrophysical Environment 18
19 Cosmic ray propagation 19
20 Cosmic ray propagation NGC891 Radio emission 20
21 Cosmic ray propagation Turbulent magnetic field 21
22 1 14 kpc Cosmic ray propagation 20 kpc Turbulent magnetic field 22
23 1 14 kpc Cosmic ray propagation 20 kpc galactic source Turbulent magnetic field 23
24 Cosmic ray propagation The transport equation describes the evolution of the CR density Sources Time evolution Diffusion Convection Energy evolution Each specie has its own transport equation usually coupled with other CR specie 24
25 Cosmic ray propagation There is some degeneracy in the propagation's parameter space 25
26 Cosmic ray propagation Transport equation Secondaries From spallations Primaries From SNR and pulsars 26
27 Cosmic ray propagation Details in arxiv:
28 1 14 kpc Cosmic ray propagation 20 kpc Dark Matter source DM halo 28
29 Cosmic ray propagation Transport equation Source from DM annihilation Annihilation cross section Annihilation spectrum DM distribution 29
30 Cosmic rays propagation [arxiv: ] 30
31 WIMP Searches in radio 31
32 Synchrotron spectrum FM VHF Wifi 32
33 Synchrotron spectrum FM VHF Wifi 33
34 Observations from 22 to 1420 DRAO: Roger et @820MHz Guzmán et Haslam et al. Berkhuijsen et al al. The isotropic radio signal and WIMP dark CP3-Origins, Odense 2010 Reich and Reich et al
35 Galactic radio 35
36 Galactic radio 36
37 Galactic radio 37
38 Galactic radio 38
39 Constraining Galactic DM We divide Obs & DM skymaps into several patches ~10⁰x10⁰ We calculate an upper bound for (σv) using the most stringent patch in each skymap 39
40 Annihilation into b quarks [arxiv: ] Thermal cross section is reached at ~10 GeV 40
41 Annihilation into muons [arxiv: ] Constraints for DM lighter than ~15 GeV 41
42 Annihilation into W bosons [arxiv: ] Pbar constraints from Delahaye et al. ArXiv: Bounds for W bosons are not so strong 42
43 Extragalactic radio 43
44 Extragalactic radio 44
45 Extragalactic radio 45
46 Source Count Gervasi et al Sources per: unit angle unit of intensity 46
47 Isotropic radio background ARCADE 2 anomaly They have reported an excess in the radio background which is bigger that the expected with known sources Firxen et al. [arxiv: ] Seiffert et al. [arxiv: ] 47
48 ARCADE 2 anomaly PRL 107, (2011), arxiv: The source count is the key to understand the excess Source counts The ARCADE excess needs of a extragalactic population of sources that dominates at low luminosity and have a steep radio spectrum Could WIMPs do the job? intensity 48
49 ARCADE 2 anomaly PRL 107, (2011), arxiv: DM can provide the missing signal However, it is not unique Alternative explanations Faint quasars Radio-quite AGNs Star forming galaxies Unresolved galactic sources(?) More details: Gervasi et al. [arxiv: ] Singal et al. [arxiv: ] 49
50 Beyond the extra-galactic background [arxiv: ] Power spectrum description of the extragalactic DM radio. A full analysis and forecast are very challenging 50
51 Beyond the extra-galactic background [arxiv: ] 51
52 The isotropic radio background revisited [arxiv: ] 52
53 The isotropic radio background revisited [arxiv: ] 53
54 Intensity The method The data position 54
55 Intensity The method The data Model galactic Model isotropic position 55
56 The method Intensity 1st fit position 56
57 The method Intensity Removing residuals larger than 5σ position 57
58 The method Intensity n-1 fit position 58
59 The method Intensity Removing residuals larger than 5σ, again position 59
60 The method Intensity Convergence! position 60
61 Intensity The method position Repeat for every skymap and trace frequency dependence 61
62 Some results mask templates 62
63 The isotropic radio background revisited [arxiv: ] Experimental uncertainties ARCADE2 collab. results Galactic modeling Estimation from Source Counts 63
64 Conclusions The (extra) galactic radio sky gives an alternative way to constrain WIMP dark matter DM radio searches are able to explore regions with thermal cross section i.e. (σv) = 3 x 10 ²⁶ cm³/s Lower frequencies are more suitable to explore light DM candidates, however cross correlation with other observables are required (!) The ARCADE 2 anomaly is still an unresolved issue 64
65 ~ /pages/dark-matter-hunters/
66 Conclusions The (extra) galactic radio sky gives an alternative way to constrain WIMP dark matter DM radio searches are able to explore regions with thermal cross section i.e. (σv) = 3 x 10 ²⁶ cm³/s Lower frequencies are more suitable to explore light DM candidates, however cross correlation with other observables are required (!) The ARCADE 2 anomaly is still an unresolved issue 66
67 Thank you 67
68 Some references [ ] Radio data and synchrotron emission in consistent cosmic ray models T. Bringmann, F. Donato, R. A. Lineros [ ] Possibility of a Dark Matter Interpretation for the Excess in Isotropic Radio Emission Reported by ARCADE N. Fornengo, R. Lineros, M. Regis, M. Taoso [ ] Galactic synchrotron emission from WIMPs at radio frequencies N. Fornengo, R. A. Lineros, M. Regis, M. Taoso [ ] Cosmological Radio Emission induced by WIMP Dark Matter N. Fornengo, R. Lineros, M. Regis, M. Taoso [ ] The isotropic radio background revisited N. Fornengo, R. A. Lineros, M. Regis, M. Taoso 68
Institut für Kern- und Teilchenphysik Neutrinos & Cosmology
Neutrinos & Cosmology 1 Cosmology: WHY??? From laboratory experiment limits can be set ONLY in neutrino mass difference No information if neutrino masses are degenerated From kinematic experiment limits
More informationGamma-rays from Dark Matter Mini-Spikes in Andromeda Galaxy M31. Mattia Fornasa Dipartimento di Fisica G. Galilei I.N.F.N. Padova
Gamma-rays from Dark Matter Mini-Spikes in Andromeda Galaxy M31 Mattia Fornasa Dipartimento di Fisica G. Galilei I.N.F.N. Padova based on astro-ph/0703757 by M. Fornasa, M. Taoso and G.Bertone Journal
More informationMalcolm S. Longair. Galaxy Formation. With 141 Figures and 12 Tables. Springer
Malcolm S. Longair Galaxy Formation With 141 Figures and 12 Tables Springer Contents Part I Preliminaries 1. Introduction, History and Outline 3 1.1 Prehistory 3 1.2 The Theory of the Expanding Universe
More informationGamma Rays from Molecular Clouds and the Origin of Galactic Cosmic Rays. Stefano Gabici APC, Paris
Gamma Rays from Molecular Clouds and the Origin of Galactic Cosmic Rays Stefano Gabici APC, Paris The Origin of galactic Cosmic Rays Facts: the spectrum is (ALMOST) a single power law -> CR knee at few
More informationData Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
More informationHIGHLIGHTS OF RECENT RESULTS FROM THE VERITAS GAMMA-RAY OBSERVATORY TAUP-2015 TORINO. Lucy Fortson. VERITAS Collaboration. Fortson, TAUP 2015, Torino
HIGHLIGHTS OF RECENT RESULTS FROM THE VERITAS GAMMA-RAY OBSERVATORY TAUP-2015 TORINO Lucy Fortson forlucy the VERITAS Collaboration Fortson, TAUP 2015, Torino 1 499 PMTs 3.5o field of view 0.15o spacing
More informationREALIZING EINSTEIN S DREAM Exploring Our Mysterious Universe
REALIZING EINSTEIN S DREAM Exploring Our Mysterious Universe The End of Physics Albert A. Michelson, at the dedication of Ryerson Physics Lab, U. of Chicago, 1894 The Miracle Year - 1905 Relativity Quantum
More informationPerspective of discoveries from Intergalactic Space. Matteo Viel INAF/OATS & INFN/TS Off-the-beaten-track workshop ICTP Trieste - 14 th April 2015
Perspective of discoveries from Intergalactic Space Matteo Viel INAF/OATS & INFN/TS Off-the-beaten-track workshop ICTP Trieste - 14 th April 2015 1 OFF-THE-BEATEN-TRACK TOPIC #1: MASSIVE NEUTRINOS 2 COSMOLOGICAL
More informationThe Mainz LXe TPC MC simulations for a Compton scattering experiment
The Mainz LXe TPC MC simulations for a Compton scattering experiment Pierre Sissol Johannes Gutenberg Universität Mainz 12 November 2012 1 / 24 Outline 1 Dark Matter 2 Principle of a dual-phase LXe TPC
More information8 Radiative Cooling and Heating
8 Radiative Cooling and Heating Reading: Katz et al. 1996, ApJ Supp, 105, 19, section 3 Thoul & Weinberg, 1995, ApJ, 442, 480 Optional reading: Thoul & Weinberg, 1996, ApJ, 465, 608 Weinberg et al., 1997,
More informationThe Search for Dark Matter, Einstein s Cosmology and MOND. David B. Cline
The Search for Dark Matter, Einstein s Cosmology and MOND David B. Cline Astrophysics Division, Department of Physics & Astronomy University of California, Los Angeles, CA 90095 USA dcline@physics.ucla.edu
More informationGravity Testing and Interpreting Cosmological Measurement
Cosmological Scale Tests of Gravity Edmund Bertschinger MIT Department of Physics and Kavli Institute for Astrophysics and Space Research January 2011 References Caldwell & Kamionkowski 0903.0866 Silvestri
More informationBig Bang Nucleosynthesis
Big Bang Nucleosynthesis The emergence of elements in the universe Benjamin Topper Abstract. In this paper, I will first give a brief overview of what general relativity has to say about cosmology, getting
More informationAstronomy & Physics Resources for Middle & High School Teachers
Astronomy & Physics Resources for Middle & High School Teachers Gillian Wilson http://www.faculty.ucr.edu/~gillianw/k12 A cosmologist is.... an astronomer who studies the formation and evolution of the
More informationInterstellar Cosmic-Ray Spectrum from Gamma Rays and Synchrotron
Interstellar Cosmic-Ray Spectrum from Gamma Rays and Synchrotron Chuck Naval Research Laboratory, Washington, DC charles.dermer@nrl.navy.mil Andy Strong Max-Planck-Institut für extraterrestrische Physik,
More informationCosmology and Fundamental Physics with Gamma-Ray Astronomy
Cosmology and Fundamental Physics with Gamma-Ray Astronomy J.H. Buckley Washington University, Dept. Physics CB 1105, 1 Brookings Dr., St. Louis, MO. 63130 e-mail: buckleywuphys.wustl.edu phone: (314)
More informationSearch for supersymmetric Dark Matter with GLAST!!
Search for supersymmetric Dark Matter with GLAST!! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata ICCRC2003 The 28th International Cosmic Ray Conference Tsukuba, Japan, July 31-
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationThe Universe. The Solar system, Stars and Galaxies
The Universe The Universe is everything. All us, the room, the U.S. the earth, the solar system, all the other stars in the Milky way galaxy, all the other galaxies... everything. How big and how old is
More informationTheoretical Particle Physics FYTN04: Oral Exam Questions, version ht15
Theoretical Particle Physics FYTN04: Oral Exam Questions, version ht15 Examples of The questions are roughly ordered by chapter but are often connected across the different chapters. Ordering is as in
More informationSearch for Dark Matter at the LHC
Search for Dark Matter at the LHC Steven Lowette Vrije Universiteit Brussel - IIHE 19 November 2014 3rd CosPa Meeting Université de Liège Content Introduction Generic DM searches at the LHC Explicit DM
More informationOrigins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
More informationWorld of Particles Big Bang Thomas Gajdosik. Big Bang (model)
Big Bang (model) What can be seen / measured? basically only light (and a few particles: e ±, p, p, ν x ) in different wave lengths: microwave to γ-rays in different intensities (measured in magnitudes)
More informationBig Bang Cosmology. Big Bang vs. Steady State
Big Bang vs. Steady State Big Bang Cosmology Perfect cosmological principle: universe is unchanging in space and time => Steady-State universe - Bondi, Hoyle, Gold. True? No! Hubble s Law => expansion
More informationEllipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0
Elliptical galaxies: Ellipticals Old view (ellipticals are boring, simple systems)! Ellipticals contain no gas & dust! Ellipticals are composed of old stars! Ellipticals formed in a monolithic collapse,
More informationChapter 23 The Beginning of Time
Chapter 23 The Beginning of Time 23.1 The Big Bang Our goals for learning What were conditions like in the early universe? What is the history of the universe according to the Big Bang theory? What were
More informationthermal history of the universe and big bang nucleosynthesis
thermal history of the universe and big bang nucleosynthesis Kosmologie für Nichtphysiker Markus Pössel (vertreten durch Björn Malte Schäfer) Fakultät für Physik und Astronomie, Universität Heidelberg
More informationASTROPARTICLE PHYSICS WITH AMS-02: THE QUEST OF ANTIMATTER
ASTROPARTICLE PHYSICS WITH AMS-02: THE QUEST OF ANTIMATTER C.Sbarra a on behalf of the AMS collaboration INFN of Bologna, Viale B.Pichat 6/2 I-40127 Bologna, Italy Abstract.The Alpha Magnetic Spectrometer,
More informationA Universe of Galaxies
A Universe of Galaxies Today s Lecture: Other Galaxies (Chapter 16, pages 366-397) Types of Galaxies Habitats of Galaxies Dark Matter Other Galaxies Originally called spiral nebulae because of their shape.
More informationSelected Topics in Elementary Particle Physics ( Haupt-Seminar )
Selected Topics in Elementary Particle Physics ( Haupt-Seminar ) Paola Avella, Veronika Chobanova, Luigi Li Gioi, Christian Kiesling, Hans-Günther Moser, Martin Ritter, Pit Vanhoefer Time: Do, 12 ct -14
More informationTesting dark matter halos using rotation curves and lensing
Testing dark matter halos using rotation curves and lensing Darío Núñez Instituto de Ciencias Nucleares, UNAM Instituto Avanzado de Cosmología A. González, J. Cervantes, T. Matos Observational evidences
More informationTest 2 --- Natural Sciences 102, Professors Rieke --- VERSION B March 3, 2010
Enter your answers on the form provided. Be sure to write your name and student ID number on the first blank at the bottom of the form. Please mark the version (B) in the Key ID space at the top of the
More informationCosmological Analysis of South Pole Telescope-detected Galaxy Clusters
Cosmological Analysis of South Pole Telescope-detected Galaxy Clusters March 24th Tijmen de Haan (McGill) - Moriond 2014 Photo credit: Keith Vanderlinde Outline The galaxy cluster sample Calibrating the
More informationFaber-Jackson relation: Fundamental Plane: Faber-Jackson Relation
Faber-Jackson relation: Faber-Jackson Relation In 1976, Faber & Jackson found that: Roughly, L! " 4 More luminous galaxies have deeper potentials Can show that this follows from the Virial Theorem Why
More informationStructure formation in modified gravity models
Structure formation in modified gravity models Kazuya Koyama Institute of Cosmology and Gravitation University of Portsmouth Dark energy v modified gravity Is cosmology probing the breakdown of general
More informationThe Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
More informationTopic 3. Evidence for the Big Bang
Topic 3 Primordial nucleosynthesis Evidence for the Big Bang! Back in the 1920s it was generally thought that the Universe was infinite! However a number of experimental observations started to question
More informationEinstein Rings: Nature s Gravitational Lenses
National Aeronautics and Space Administration Einstein Rings: Nature s Gravitational Lenses Leonidas Moustakas and Adam Bolton Taken from: Hubble 2006 Science Year in Review The full contents of this book
More informationThe Milky Way Galaxy is Heading for a Major Cosmic Collision
The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing
More informationExploring the Universe Through the Hubble Space Telescope
Exploring the Universe Through the Hubble Space Telescope WEEK FIVE: THE HUBBLE DEEP FIELD + LIMITATIONS OF HUBBLE, COLLABORATIONS, AND THE FUTURE OF ASTRONOMY Date: October 14, 2013 Instructor: Robert
More informationGravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole
Gravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole Kinwah Wu Mullard Space Science Laboratory University College London United Kingdom kw@mssl.ucl.ac.uk
More informationGravitation modifiée à grande distance & tests dans le système solaire 10 avril 2008
Gravitation modifiée à grande distance et tests dans le système solaire Gilles Esposito-Farèse, GRεCO, IAP et Peter Wolf, LNE-SYRTE 10 avril 2008 Gravitation modifiée à grande distance & tests dans le
More informationThe dynamics and energetics of FR-II radio galaxies
The dynamics and energetics of FR-II radio galaxies Jeremy Harwood National Astronomy Meeting Llandudno, July2015 Collaborators: Martin Hardcastle (Hertfordshire) Judith Croston (Southampton) Raffaella
More informationSpecific Intensity. I ν =
Specific Intensity Initial question: A number of active galactic nuclei display jets, that is, long, nearly linear, structures that can extend for hundreds of kiloparsecs. Many have two oppositely-directed
More information1 Introduction. 1 There may, of course, in principle, exist other universes, but they are not accessible to our
1 1 Introduction Cosmology is the study of the universe as a whole, its structure, its origin, and its evolution. Cosmology is soundly based on observations, mostly astronomical, and laws of physics. These
More informationThe CGM around Dwarf Galaxies
The CGM around Dwarf Galaxies Rongmon Bordoloi STScI + the COS-Halos Team What is the CGM? Shen et al. 212 jectedcolumndensityinacubeof5(proper)kpc Diffuse gas, including metals and dust, o2en on extending
More informationPlanck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains
Planck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains Perseus in the optical Clive Dickinson Jodrell Bank Centre for Astrophysics (University of Manchester) On behalf
More informationFundamental Physics at Extreme High Energies
Fundamental Physics at Extreme High Energies Michael Kachelrieß NTNU, Trondheim [] Outline: Introduction Testing (new?) strong interactions Lorentz invariance violation Topological defects & superheavy
More informationYour years of toil Said Ryle to Hoyle Are wasted years, believe me. The Steady State Is out of date Unless my eyes deceive me.
Your years of toil Said Ryle to Hoyle Are wasted years, believe me. The Steady State Is out of date Unless my eyes deceive me. My telescope Has dashed your hope; Your tenets are refuted. Let me be terse:
More informationLecture 3 Properties and Evolution of Molecular Clouds. Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11
Lecture 3 Properties and Evolution of Molecular Clouds Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11 From slide from Annie Hughes Review CO t in clouds HI: Atomic Hydrogen http://www.atnf.csiro.au/research/lvmeeting/magsys_pres/
More informationIndirect dark matter detection offers a promising approach to
Separating astrophysical sources from indirect dark matter signals Jennifer M. Siegal-Gaskins 1 Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125 Edited
More informationClass #14/15 14/16 October 2008
Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM
More informationProbing Dark Energy with Baryon Acoustic Oscillations from Future Large Galaxy Redshift Surveys
Probing Dark Energy with Baryon Acoustic Oscillations from Future Large Galaxy Redshift Surveys Hee-Jong Seo (Steward Observatory) Daniel J. Eisenstein (Steward Observatory) Martin White, Edwin Sirko,
More informationAxion/Saxion Cosmology Revisited
Axion/Saxion Cosmology Revisited Masahiro Yamaguchi (Tohoku University) Based on Nakamura, Okumura, MY, PRD77 ( 08) and Work in Progress 1. Introduction Fine Tuning Problems of Particle Physics Smallness
More informationOlga Botner, Uppsala. Photo: Sven Lidström. Inspirationsdagar, 2015-03-17
Olga Botner, Uppsala Photo: Sven Lidström Inspirationsdagar, 2015-03-17 OUTLINE OUTLINE WHY NEUTRINO ASTRONOMY? WHAT ARE NEUTRINOS? A CUBIC KILOMETER DETECTOR EXTRATERRESTRIAL NEUTRINOS WHAT NEXT? CONCLUSIONS
More informationWave-particle and wave-wave interactions in the Solar Wind: simulations and observations
Wave-particle and wave-wave interactions in the Solar Wind: simulations and observations Lorenzo Matteini University of Florence, Italy In collaboration with Petr Hellinger, Simone Landi, and Marco Velli
More informationModified Gravity and the CMB
Modified Gravity and the CMB Philippe Brax, IphT Saclay, France arxiv:1109.5862 PhB, A.C. Davis Work in progress PhB, ACD, B. Li Minneapolis October 2011 PLANCK will give us very precise information on
More informationIonospheric Research with the LOFAR Telescope
Ionospheric Research with the LOFAR Telescope Leszek P. Błaszkiewicz Faculty of Mathematics and Computer Science, UWM Olsztyn LOFAR - The LOw Frequency ARray The LOFAR interferometer consist of a large
More informationThe Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC
The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is
More informationAstro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
More informationThe Gaia Archive. Center Forum, Heidelberg, June 10-11, 2013. Stefan Jordan. The Gaia Archive, COSADIE Astronomical Data
The Gaia Archive Astronomisches Rechen-Institut am Zentrum für Astronomie der Universität Heidelberg http://www.stefan-jordan.de 1 2 Gaia 2013-2018 and beyond Progress with Gaia 3 HIPPARCOS Gaia accuracy
More informationx 1 ' = x 1 vt 1 x 1 ' = 4.0 m t 1 = 1.0 s x 2 vt 2 ' = 4.0 m t 2 ' = x 2 = 3.0 s x 1 = x 2 x 1 ' + vt 1 ' + vt 2 v (t 1 t 2 ) = x 2 ' x 1 ' = x 2
Physics 2220 Module 16 Homework 01. A firecracker explodes in reference frame S at t 1 1.0 seconds. A second firecracker explodes at the same position at t 2 3.0 seconds. In reference frame S', which moves
More informationGalaxy clusters, in the light of Planck. Nabila Aghanim, Institut d'astrophysique Spatiale, CNRS-Univ. Paris Sud
Galaxy clusters, in the light of Planck Nabila Aghanim, Institut d'astrophysique Spatiale, CNRS-Univ. Paris Sud Galaxy clusters in the cosmic web CLEF-SSH hydro simulation, Kay et al. '06 Cluster components
More informationMAKING PARTICLE PHYSICS, COSMOLOGY AND ASTROPHYSICS WORK TOGETHER THE UNIVERSE CONSTITUENTS, FORCES, SPACE-TIME
MAKING PARTICLE PHYSICS, COSMOLOGY AND ASTROPHYSICS WORK TOGETHER THE UNIVERSE CONSTITUENTS, FORCES, SPACE-TIME Swiss Institute of Particle Physics an Association according to Swiss law IMPRESSUM Photographs
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationDark Matter in the Universe
A UNIVERSAL VIEW Dark Matter in the Universe by Vera Rubin FRANÇOIS SCHWEIZER Carnegie Institution of Washington, BRAD WHITMORE Space Telescope Science Institute AND NASA As much as 90 percent of the matter
More informationHow Do Galeries Form?
8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-1 8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-2 Galaxy Formation Leading questions for today How do
More informationLecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
More informationElliptical Galaxies. Galaxies and Their Properties, Part II: Fine Structure in E-Galaxies: A Signature of Recent Merging
Elliptical Galaxies Ay 21 - Lecture 12 Galaxies and Their Properties, Part II: Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals
More informationCalorimetry in particle physics experiments
Calorimetry in particle physics experiments Unit n. 8 Calibration techniques Roberta Arcidiacono Lecture overview Introduction Hardware Calibration Test Beam Calibration In-situ Calibration (EM calorimeters)
More informationSolar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
More informationHighlights of Recent CMS Results. Dmytro Kovalskyi (UCSB)
Highlights of Recent CMS Results Dmytro Kovalskyi (UCSB) Introduction Number of CMS publication is over 0 already It is very hard to review all the recent results in one talk This talk concentrates on
More informationFirst Discoveries. Asteroids
First Discoveries The Sloan Digital Sky Survey began operating on June 8, 1998. Since that time, SDSS scientists have been hard at work analyzing data and drawing conclusions. This page describes seven
More informationNeutrino properties from Cosmology
Neutrino properties from Cosmology Anže Slosar, BNL Neutrino16, July 16 1 / 30 plan for the talk Pedagogical introduction to the role neutrinos play in Cosmology aimed at a non-cosmo community Neutrinos
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More informationHow To Find The Higgs Boson
Dezső Horváth: Search for Higgs bosons Balaton Summer School, Balatongyörök, 07.07.2009 p. 1/25 Search for Higgs bosons Balaton Summer School, Balatongyörök, 07.07.2009 Dezső Horváth MTA KFKI Research
More informationElliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies
Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:
More informationPolarization, magnetic fields and radio galaxies in galaxy clusters. Gianfranco Gentile Universiteit Gent / Vrije Universiteit Brussel (Belgium)
Polarization, magnetic fields and radio galaxies in galaxy clusters Gianfranco Gentile Universiteit Gent / Vrije Universiteit Brussel (Belgium) Outline - Part 1: Introduction - Part 2: Perseus cluster
More informationMapping structure of the Universe. the very large scale. INAF IASF Milano
Mapping the large scale structure of the Universe the very large scale structure Marco Scodeggio INAF IASF Milano The large scale structure (100Mpc) Zero order approximation: the Universe is homegeneous
More informationPhysical Self-Calibration of X-ray and SZ Surveys
Physical Self-Calibration of X-ray and SZ Surveys Greg L. Bryan, Zoltan Haiman (Columbia University) and Joshua D. Younger (CfA) 1. Cluster Surveys and Self-Calibration Clusters of galaxies form at the
More informationNASA s Future Missions in X-ray Astronomy
NASA s Future Missions in X-ray Astronomy Nicholas E. White NASA s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, MD 20771 USA nwhite@lheapop.gsfc.nasa.gov Abstract The
More informationA Century of Paradigm Shifts in our Thinking About the Universe
A Century of Paradigm Shifts in our Thinking About the Universe George R. Blumenthal Chancellor, UC Santa Cruz Professor of Astronomy and Astrophysics Why start 100 years ago? Before 1910 there was no
More informationThe Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor)
The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) Didier BARRET on behalf of the SVOM collaboration didier.barret@cesr.fr Outline SVOM background
More informationDinamica del Gas nelle Galassie II. Star formation
Dinamica del Gas nelle Galassie II. Star formation Overview on ISM Molecular clouds: composition and properties. Plasmas Charge neutrality, infinite conductivity; Field freezing; Euler equation with magnetic
More informationIntermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints. Roeland van der Marel
Intermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints Roeland van der Marel Why Study IMBHs in Globular Clusters (GCs)? IMBHs: IMBHs can probe a new BH mass range, between
More informationEvolution of the Universe from 13 to 4 Billion Years Ago
Evolution of the Universe from 13 to 4 Billion Years Ago Prof. Dr. Harold Geller hgeller@gmu.edu http://physics.gmu.edu/~hgeller/ Department of Physics and Astronomy George Mason University Unity in the
More informationLecture 6: distribution of stars in. elliptical galaxies
Lecture 6: distribution of stars in topics: elliptical galaxies examples of elliptical galaxies different classes of ellipticals equation for distribution of light actual distributions and more complex
More informationLight as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
More informationCurriculum for Excellence. Higher Physics. Success Guide
Curriculum for Excellence Higher Physics Success Guide Electricity Our Dynamic Universe Particles and Waves Electricity Key Area Monitoring and Measuring A.C. Monitoring alternating current signals with
More informationThe Higgs Boson. Linac08 Victoria BC, Canada CANADA S NATIONAL LABORATORY FOR PARTICLE AND NUCLEAR PHYSICS
CANADA S NATIONAL LABORATORY FOR PARTICLE AND NUCLEAR PHYSICS Owned and operated as a joint venture by a consortium of Canadian universities via a contribution through the National Research Council Canada
More informationGRAVITINO DARK MATTER
GRAVITINO DARK MATTER Wilfried Buchmüller DESY, Hamburg LAUNCH09, Nov. 2009, MPK Heidelberg Why Gravitino Dark Matter? Supergravity predicts the gravitino, analog of W and Z bosons in electroweak theory;
More informationINTRODUCTION TO NEUTRINO PHYSICS
INTRODUCTION TO NEUTRINO PHYSICS Paolo Lipari Dipartimento di Fisica, Università di Roma la Sapienza, and I.N.F.N., Sezione di Roma, P.A. Moro, I-00185 Roma, Italy 1. INTRODUCTION Abstract Neutrino Physics
More informationNeutron Stars. How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967.
Neutron Stars How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967. Using a radio telescope she noticed regular pulses of radio
More informationThe accurate calibration of all detectors is crucial for the subsequent data
Chapter 4 Calibration The accurate calibration of all detectors is crucial for the subsequent data analysis. The stability of the gain and offset for energy and time calibration of all detectors involved
More informationSUSY Breaking and Axino Cosmology
SUSY Breaking and Axino Cosmology Masahiro Yamaguchi Tohoku University Nov. 10, 2010 ExDiP2010@KEK, Japan 1. Introduction Fine Tuning Problems of Particle Physics Smallness of electroweak scale Smallness
More informationScience Drivers for Big Data Joseph Lazio SKA Program Development Office & Jet Propulsion Laboratory, California Institute of Technology
Science Drivers for Big Data Joseph Lazio SKA Program Development Office & Jet Propulsion Laboratory, California Institute of Technology 2010 California Institute of Technology. Government sponsorship
More informationCosmic Ray Astrophysics with AMS-02 Daniel Haas - Université de Genève on behalf of the AMS collaboration
Cosmic Ray Astrophysics with AMS-02 Daniel Haas - Université de Genève on behalf of the AMS collaboration Overview of AMS-02 Cosmic ray studies p/he, Z>2, p/e +, γ-rays Comparison AMS vs. GLAST AMS vs.
More informationHow To Know If Dark Matter Exists
Lecture 1 A Brief History of Dark Matter Joel Primack, UCSC Although the first evidence for dark matter was discovered in the 1930s, it was in the early 1980s that astronomers became convinced that most
More informationChapter 9 Summary and outlook
Chapter 9 Summary and outlook This thesis aimed to address two problems of plasma astrophysics: how are cosmic plasmas isotropized (A 1), and why does the equipartition of the magnetic field energy density
More informationIndiana University Science with the WIYN One Degree Imager
Indiana University Science with the WIYN One Degree Imager Katherine Rhode (Indiana University, WIYN SAC member) Indiana University Department of Astronomy Nine faculty members, plus active emeritus faculty
More information