Large-Scale Structure of the Galactic Magnetic Field. Marijke Haverkorn & Jo-Anne Brown NRAO/UC-Berkeley University of Calgary
|
|
- Walter Simon
- 5 years ago
- Views:
Transcription
1 Large-Scale Structure of the Galactic Magnetic Field Marijke Haverkorn & Jo-Anne Brown NRAO/UC-Berkeley University of Calgary
2 Outline On the Large-Scale Structure of the GMF... Why do we care? What do we know? - How do we know it? What will we know? What can CMBPol contribute?
3 Why do we care? CMB Foregrounds are caused by Galactic magnetic field: Polarized Galactic synchrotron emission Dust polarization Both synchrotron and dust foreground components are stronger than the CMB B-mode! Galactic science origin of galactic magnetism: primordial and/or dynamo? magnetic field is dynamically important propagation and acceleration of cosmic rays
4 What do we know?
5 What do we know? First ask: How do we know it?
6 Magnetic Field Measurement Techniques Faraday Rotation of polarized radiation Zeeman splitting Polarization of infrared emission from dust grains Polarization of starlight by dust grains Synchrotron radiation intensity Polarization of synchrotron radiation
7 Magnetic Field Measurement Techniques Faraday Rotation of polarized radiation Zeeman splitting Polarization of infrared emission from dust grains Polarization of starlight by dust grains Synchrotron radiation intensity Polarization of synchrotron radiation
8 Faraday Rotation τ = τ 0 + λ 2 RM
9 Sources of linear polarization: Pulsars, External Galaxies ( point sources) Galactic synchrotron: see Maik Wolleben s talk
10 Compact Polarized Sources Pulsars: ~600 EGS: ~2000 Positive RM Negative RM
11 Compact Polarized Sources Pulsars: ~400 EGS: ~1000 Positive RM Negative RM
12 returning to... What do we know?
13 Galactic Magnetic Field Basics Two components: large, small Aligned with the disk Follows the spiral arms (?) Local field is clockwise Sagittarius field is counter-cw Determining the existence and location of additional reversals will help us understand the origin and evolution of the field - and possibly of the Galaxy itself!
14 And that is where the agreement ends
15 Possible symmetries Axisymmetric Mixed spiral symmetry Bisymmetric
16 Vertical Symmetry and Reconnection Quadrupolar (even symmetry) Dipolar (odd symmetry)
17 Recent Model Suggestions Axisymmetric and even (e.g. Page et al 2007, WMAP modeling) Axisymmetric and odd (e.g. Stanev 1997) Bisymmetric and even (Harari et al 1999, Prouza & Smída 2003) Bisymmetric and odd (Tinyakov & Tkachev 2002) Page et al (2007), from Sun et al (2008)
18 Recent Model Suggestions Axisymmetric and even Axisymmetric and odd Bisymmetric and even Bisymmetric and odd Reversal in every arm (Weisberg et al 2004)
19 Recent Model Suggestions Axisymmetric and even Axisymmetric and odd Bisymmetric and even Bisymmetric and odd Reversal in every arm Reversal in arms/interarms (Han et al 2007)
20 Recent Model Suggestions Axisymmetric and even Axisymmetric and odd Bisymmetric and even Bisymmetric and odd Reversal in every arm Reversal in arms/interarms One reversal in inner Galaxy (Brown et al 2007)
21 Recent Model Suggestions Axisymmetric and even Axisymmetric and odd Bisymmetric and even Bisymmetric and odd Reversal in every arm Reversal in arms/interarms One reversal in inner Galaxy Ring-shaped field (Vallée 2005)
22 Some models explain part of the GMF Brown Brown et al 2007: reversal between Carina and Crux arm Weisberg et al 2004: reversal between Sagittarius and Scutum arm
23 but none fit all the observational data! Sun et al (2007), Men et al (2008), Noutsos et al (2008) Sun et al (2008) RM [rad m -2 ] longitude [deg]
24 Typical χ 2 s are MUCH too high: Noutsos et al 2008
25 Why don t the current models fit the data? 1. Random field component is not completely averaged out = +
26 Why don t the current models fit the data? 1. Random field component is not completely averaged out 2. Magnetic pitch angle is not constant Beck 2007
27 Why don t the current models fit the data? 1. Random field component is not completely averaged out 2. Magnetic pitch angle is not constant 3. Mixed dynamo modes NGC Chyzy 2008
28 What will we know?
29 halo and disk-halo connection filling in of Galactic plane
30 Galactic caps: vertical component of field (Mao, Gaensler et al) Northern sky survey: LOFAR all Southern sky survey: ASKAP, MWA
31 WMAP sensitivity is too low to sample Galactic magnetic field in the halo 23 GHz Planck and/or CMBPol needed
32 How can CMBPol contribute?
33 Sensitivity? -- probing the magnetic halo. HOWEVER: Planck Resolution? -- less depolarization: depends on halo scale size
34 Outline/Summary On the Large-Scale Structure of the GMF... What do we know? at least 1 reversal, concentrated along disk, many different scale sizes - How do we know it? primarily Radio Polarization & Faraday Rotation What will we know? - actual number of large-scale reversals - magnitude, disk and vertical symmetries How can CMBPol contribute? Sensitivity: magnetic field in Galactic halo Depolarization: small-scale structure in halo
The Galactic magnetic field
The Galactic magnetic field Marijke Haverkorn (Nijmegen/Leiden) ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Big Questions: What is the origin of galactic magnetic fields?
More informationThe Global Magneto-Ionic Medium Survey
The Global Magneto-Ionic Medium Survey The Global Magneto-Ionic Medium Survey studying the polarized emission from the Galaxy The Global Magneto-Ionic Medium Survey GMIMS studying the polarized emission
More informationRotation Measure Synthesis of the Local Magnetized ISM
Rotation Measure Synthesis of the Local Magnetized ISM Maik Wolleben Covington Fellow, DRAO Outline Polarization, Faraday Rotation, and Rotation Measure Synthesis The Data: GMIMS The Global Magneto Ionic
More informationStudy of Large-Scale Galactic Magnetic Fields at Low Frequencies. Jana Köhler - MPIfR -
Study of Large-Scale Galactic Magnetic Fields at Low Frequencies Jana Köhler - MPIfR - How to measure Magnetic Fields??? How to measure Galactic Magnetic Field? Linear Polarization of Starlight product
More informationGalactic cosmic rays propagation
Galactic cosmic rays propagation Side view of the Galaxy The Solar system is 8.5 kpc away from the galactic center. One pc is 3.10 18 cm, so we are at a distance of 2.55 10 17 km and the light from it
More informationMagnetic fields of our Galaxy on large and small scales
Magnetic fields of our Galaxy on large and small scales JinLin Han National Astronomical Observatories Chinese Academy of Sciences hjl@bao.ac.cn A small work dedicated to IAU 242 Published on mid-march
More informationRadio Continuum: Cosmic Rays & Magnetic Fields. Rainer Beck MPIfR Bonn
Radio Continuum: Cosmic Rays & Magnetic Fields Rainer Beck MPIfR Bonn Synchrotron emission Beam angle: Ψ/2=1/γ=E o /E Radio continuum tools to study GeV Cosmic ray electrons (CRE) Synchrotron spectrum:
More informationMagnetic fields in galaxies
Magnetic fields in galaxies Selected items (high-speed version) Rainer Beck, MPIfR Bonn Fundamental questions on galactic magnetic fields When and how were the first magnetic fields generated? How and
More informationTesting the magnetic field models of disk galaxies with the SKA
Testing the magnetic field models of disk galaxies with the SKA, a R. Stepanov b, R. Beck a, P. Frick b and M. Krause a a Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 3121 Bonn, Germany b
More informationCosmic Microwave Background
Cosmic Microwave Background Carlo Baccigalupi,, SISSA CMB lectures at TRR33, see the complete program at darkuniverse.uni-hd.de/view/main/winterschoollecture5 These lectures are available in pdf format
More informationMagnetic Fields in Evolving Spiral Galaxies and their Observation with the SKA
Magnetic Fields in Evolving Spiral Galaxies and their Observation with the SKA Rainer Beck MPIfR Bonn & SKA Science Working Group Fundamental magnetic questions When and how were the first fields generated?
More informationMagnetic Fields in the Milky Way
Magnetic Fields in the Milky Way Wolfgang Reich Max-Planck-Institut für Radioastronomie Bonn Why is the Galactic B-field of interest? highest spatial resolution of B-fields clarify its role in spiral galaxies
More informationOrigin of Magnetic Fields in Galaxies
Lecture 4: Origin of Magnetic Fields in Galaxies Rainer Beck, MPIfR Bonn Generation and amplification of cosmic magnetic fields Stage 1: Field seeding Stage 2: Field amplification Stage 3: Coherent field
More informationPolarized Galactic foregrounds: a review
Polarized Galactic foregrounds: a review Joanna Dunkley University of Oxford CMBPol Chicago, July 1 2009 Foreground Working Groups Removal: Alex Amblard, Carlo Baccigalupi, Marc Betoule, David Chuss, Asantha
More informationarxiv: v1 [astro-ph] 10 Nov 2007
Astronomy & Astrophysics manuscript no. sim-rev.low c ESO 2008 February 2, 2008 Radio observational constraints on Galactic 3D-emission models X. H. Sun 1,, W. Reich 1, A. Waelkens 2 and T. A. Enßlin 2
More informationUsing Pulsars to study the Magnetic Field in The Milky way
Using Pulsars to study the Magnetic Field in The Milky way Dipanjan Mitra ( MPIFR Bonn) R. Wielebinski ( MPIFR Bonn) M. Kramer ( Jodrell Bank) A. Jessner ( MPIFR Bonn) MPIFR, Bonn (24 th April 2003) To
More informationG-ALFA Continuum Transit Survey GALFACTS. E. Momjian Prepared by A.R. Taylor for the GALFA Continuum Consortium
G-ALFA Continuum Transit Survey GALFACTS E. Momjian Prepared by A.R. Taylor for the GALFA Continuum Consortium GALFA Continuum Consortium Christy Bredeson Jo-Anne Brown Mike Davis Avinash Deshpande Tyler
More informationCosmic Magnetism. Marijke Haverkorn, on behalf of the SKA Cosmic Magnetism Science Working Group
Cosmic Magnetism Marijke Haverkorn, on behalf of the SKA Cosmic Magnetism Science Working Group The Magnetism Science Working Group Core Members: Sui Ann Mao (co-chair) George Heald (co-chair) Ivan Agudo
More informationMagnetic field structure from Planck polarization observations of the diffuse Galactic ISM
Magnetic field structure from Planck polarization observations of the diffuse Galactic ISM François Boulanger Institut d Astrophysique Spatiale on behalf of the Planck Consortium Outline The Planck data
More informationParkes MHz Rotation Measure Survey
Parkes 300-900 MHz Rotation Measure Survey Maik Wolleben E. Carretti, J. Dickey, A. Fletcher, B. Gaensler, J. L. Han, M. Haverkorn, T. Landecker, J. Leahy, N. McClure-Griffiths, D. McConnell, W. Reich,
More informationS-PASS and Giant Magnetised outflows from the Centre of the Milky Way
S-PASS and Giant Magnetised outflows from the Centre of the Milky Way Ettore Carretti The Universe as seen by Planck Noordwijk - 4 April 2013 CSIRO ASTRONOMY AND SPACE SCIENCE Outline S-PASS: S-band Polarization
More informationLecture 13 Interstellar Magnetic Fields
Lecture 13 Interstellar Magnetic Fields 1. Introduction. Synchrotron radiation 3. Faraday rotation 4. Zeeman effect 5. Polarization of starlight 6. Summary of results References Zweibel & Heiles, Nature
More informationarxiv: v1 [astro-ph.ga] 29 Oct 2012
Draft version September 10, 2018 Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE GALACTIC MAGNETIC FIELD Ronnie Jansson and Glennys R. Farrar Center for Cosmology and Particle Physics, Department
More informationarxiv: v1 [astro-ph.ga] 16 Apr 2012
Draft version March 2, 2013 Preprint typeset using L A TEX style emulateapj v. 5/2/11 A NEW MODEL OF THE GALACTIC MAGNETIC FIELD Ronnie Jansson and Glennys R. Farrar Center for Cosmology and Particle Physics
More informationarxiv: v1 [astro-ph] 18 Dec 2008
Proceedings Title IAU Symposium Proceedings IAU Symposium No. 259, 09 K.G. Strassmeier, A.G. Kosovichev, & J. Beckmann c 09 International Astronomical Union DOI: 00.0000/X000000000000000X The magnetic
More informationarxiv: v2 [astro-ph.ga] 4 Aug 2013
Solar and Astrophysical Dynamos and Magnetic Activity Proceedings IAU Symposium No. 294, 2012 c International Astronomical Union 2013 A.G. Kosovichev, E.M. de Gouveia Dal Pino, & Y.Yan, eds. DOI: 10.1017/S1743921313002561
More informationUltraHigh Energy Cosmic Rays Corrected for Galaxy Magnetic Field Models: FRIs & BL Lacs (Galactic Plane sources?)
UltraHigh Energy Cosmic Rays Corrected for Galaxy Magnetic Field Models: FRIs & BL Lacs (Galactic Plane sources?) Neil M. Nagar U. de Concepción, Chile Nagar & Matulich 2008, A&A, 488, 879 Nagar & Matulich,
More informationarxiv: v1 [astro-ph] 12 Jun 2008
To appear in Magnetic Fields in the Universe II (2008) RevMexAA(SC) MAGNETIC FIELDS AND STAR FORMATION IN SPIRAL GALAXIES Marita Krause, 1 RESUMEN arxiv:0806.2060v1 [astro-ph] 12 Jun 2008 ABSTRACT The
More informationMagnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Astronomy DFG Research Unit
Mainz, 9 July, 2012 Galactic and Intergalactic Magnetic Fields 1 Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Astronomy DFG Research Unit Mainz, 9 July, 2012
More informationChapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located
More informationMeasuring interstellar magnetic fields by radio synchrotron emission
Cosmic Magnetic Fields: From Planets, to Stars and Galaxies Proceedings IAU Symposium No. 259, 2008 K.G. Strassmeier, A.G. Kosovichev & J.E. Beckman, eds. c 2009 International Astronomical Union doi:10.1017/s1743921309030014
More informationObservations of magnetic fields in the Milky Way and in nearby galaxies with a Square Kilometre Array
New Astronomy Reviews 48 (2004) 1289 1304 www.elsevier.com/locate/newastrev Observations of magnetic fields in the Milky Way and in nearby galaxies with a Square Kilometre Array R. Beck a, *, B.M. Gaensler
More informationChapter 23 The Milky Way Galaxy Pearson Education, Inc.
Chapter 23 The Milky Way Galaxy The Milky Way is our own galaxy viewed from the inside. It is a vast collection of more than 200 billion stars, planets, nebulae, clusters, dust and gas. Our own sun and
More informationOur Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye
Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!
More informationDark Matter searches with radio observations
Marco Taoso Dpt. of Physics and Astronomy UBC Vancouver Dark Matter searches with radio observations IDM 2012 Chicago, 23-27 July Search for DM with astrophysical observations Gamma- rays Microwave Radio
More informationOur View of the Milky Way. 23. The Milky Way Galaxy
23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral
More informationPolarisation in Radio Astronomy: techniques of measurement, history and present status
Polarisation in Radio Astronomy: techniques of measurement, history and present status Richard Wielebinski Max-Planck-Institut für Radioastronomie, Bonn Maxwell s equations imply polarisation of electromagnetic
More informationGalactic radio loops. Philipp Mertsch with Subir Sarkar. The Radio Synchrotron Background Workshop, University of Richmond 21 July 2017
Galactic radio loops Philipp Mertsch with Subir Sarkar The Radio Synchrotron Background Workshop, University of Richmond 21 July 2017 Foregrounds in B-modes Adam et al., arxiv:1502.01588 1409.5738 (Planck
More informationSTRUCTURE IN THE ROTATION MEASURE SKY
Accepted for publication in The Astrophysical Journal Preprint typeset using L A TEX style emulateapj v. 11/26/04 STRUCTURE IN THE ROTATION MEASURE SKY J. M. Stil, A. R. Taylor, and C. Sunstrum Institute
More informationarxiv: v1 [astro-ph.ga] 24 Aug 2009
Astronomy & Astrophysics manuscript no. ver8-astro c ESO 2009 August 25, 2009 Simulated SKA maps from Galactic 3D-emission models X. H. Sun 1,2, and W. Reich 2 arxiv:0908.3378v1 [astro-ph.ga] 24 Aug 2009
More informationEnergy Sources of the Far IR Emission of M33
Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also
More informationMagnetic Fields in Galaxies
Planets, Stars and Stellar Systems, Springer, Berlin 2013, Vol. 5, Chapter 13 - corrected and updated version - Magnetic Fields in Galaxies Rainer Beck & Richard Wielebinski Max-Planck-Institut für Radioastronomie,
More informationPolarised synchrotron simulations for EoR experiments
Centre for Radio Cosmology Polarised synchrotron simulations for EoR experiments The broad impact of Low Frequency Observing Bologna, 19-23 June 2017 Marta Spinelli in collaboration with M. Santos and
More informationAnalyzing Spiral Galaxies Observed in Near-Infrared
Analyzing Spiral Galaxies Observed in Near-Infrared Preben Grosbøl European Southern Observatory Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany Abstract A sample of 54 spiral galaxies was observed
More informationPrimordial B-modes: Foreground modelling and constraints
Primordial B-modes: Foreground modelling and constraints Carlo Contaldi Imperial College London Model Polarisation Amplitude 40 60-180 160 140 120 100 20 80 0 60 40 20 0-20 -40-60 -80-100 -120-140 -160-20
More informationOur Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.
Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.
More informationLecture Outlines. Chapter 23. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 23 Astronomy Today 8th Edition Chaisson/McMillan Chapter 23 The Milky Way Galaxy Units of Chapter 23 23.1 Our Parent Galaxy 23.2 Measuring the Milky Way Discovery 23-1 Early Computers
More informationThe Origin and Evolution of Cosmic Magnetism: Perspective from SKA. Luigina Feretti IRA - Bologna MCCT-SKADS School, Medicina,
The Origin and Evolution of Cosmic Magnetism: Perspective from SKA Luigina Feretti IRA - Bologna MCCT-SKADS School, Medicina, 25 9-07 This topic is one of the 5 Key Science Projects of SKA, selected by
More informationInterstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
More informationSynchrotron Radiation, magnetic fields and cosmic rays
Synchrotron Radiation, magnetic fields and cosmic rays Giuseppe Di Bernardo 1 in collaboration with Evoli, C., Gaggero, D., Grasso, D. 1 Max Planck Institute for Astrophysics bernardo@mpa-garching.mpg.de
More informationOur Galaxy. Chapter Twenty-Five. Guiding Questions
Our Galaxy Chapter Twenty-Five Guiding Questions 1. What is our Galaxy? How do astronomers know where we are located within it? 2. What is the shape and size of our Galaxy? 3. How do we know that our Galaxy
More informationarxiv: v1 [astro-ph.ga] 15 Feb 2019
Article Magnetic field vector maps of nearby spiral galaxies Hiroyuki Nakanishi 1, Kohei Kurahara 1, and Kenta Anraku 1 1 Graduate School of Science and Engineering, Kagoshima university, 1-21-35 Korimoto,
More informationWMAP Excess Interpreted as WIMP Annihilation
WMAP Excess Interpreted as WIMP Annihilation idm2004, Edinburgh September 9, 2004 Douglas Finkbeiner Princeton University Outline " " " WMAP ISM emission (expected) The Galactic synchrotron Haze (unexpected)
More informationASTR 101 Introduction to Astronomy: Stars & Galaxies
We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light! ASTR 101 Introduction to Astronomy: Stars & Galaxies Infrared light reveals stars whose visible light
More informationKrzysztof T. Chyży, Jagiellonian University, Kraków
Krzysztof T. Chyży, Jagiellonian University, Kraków Outline Magnetism KSP (MSKP) organisation, people, meetings, received grants Cosmic targets, submitted proposals What s new in cosmic magnetism Synergy
More informationIndirect dark matter detection and the Galactic Center GeV Excess
Image Credit: Springel et al. 2008 Indirect dark matter detection and the Galactic Center GeV Excess Jennifer Siegal-Gaskins Caltech Image Credit: Springel et al. 2008 Jennifer Siegal-Gaskins Caltech Image
More informationCosmic Microwave Background
Cosmic Microwave Background Following recombination, photons that were coupled to the matter have had very little subsequent interaction with matter. Now observed as the cosmic microwave background. Arguably
More informationASTR 101 Introduction to Astronomy: Stars & Galaxies
ASTR 101 Introduction to Astronomy: Stars & Galaxies We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light Infrared light reveals stars whose visible light
More informationarxiv: v2 [astro-ph] 24 Apr 2008
Astrophysics and Space Science DOI 10.1007/sXXXXX-XXX-XXXX-X Galactic Dynamos and Galactic Winds Rainer Beck arxiv:0711.4700v2 [astro-ph] 24 Apr 2008 c Springer-Verlag Abstract Spiral galaxies host dynamically
More information3/1/18 LETTER. Instructors: Jim Cordes & Shami Chatterjee. Reading: as indicated in Syllabus on web
Astro 2299 The Search for Life in the Universe Lecture 9 Last time: Star formation Formation of protostars and planetary systems This time A few things about the epoch of reionization and free fall times
More informationThe Planck Mission and Ground-based Radio Surveys
The Planck Mission and Ground-based Radio Surveys Russ Taylor University of Calgary Kingston Meeting UBC, November 2003 Current state of that art in ground-based radio surveys How Planck factors into the
More informationMulti-frequency polarimetry of a complete sample of faint PACO sources. INAF-IRA (Bologna)
Multi-frequency polarimetry of a complete sample of faint PACO sources. Vincenzo Galluzzi Marcella Massardi DiFA (University of Bologna) INAF-IRA (Bologna) INAF-IRA & Italian ARC The state-of-the-art The
More informationMagnetic Fields in the Milky Way and in Galaxies 1
Magnetic Fields in the Milky Way and in Galaxies 1 Rainer Beck & Richard Wielebinski Max-Planck-Institut für Radioastronomie, Bonn, Germany Abstract. Most of the visible matter in the Universe is ionized,
More informationDistance Measuring Techniques and The Milky Way Galaxy
Distance Measuring Techniques and The Milky Way Galaxy Measuring distances to stars is one of the biggest challenges in Astronomy. If we had some standard candle, some star with a known luminosity, then
More informationPoS(EXTRA-RADSUR2015)011
Magnetic fields on a wide range of scales in star-forming galaxies, abc Anna Williams d and Sarrvesh S. Sridhar cb a CSIRO Astronomy and Space Science, 26 Dick Perry Avenue, Kensington WA 6151, Australia
More informationIndirect Dark Matter constraints with radio observations
Indirect Dark Matter constraints with radio observations In collaboration with E.Borriello and G.Miele, University of Naples Federico II Alessandro Cuoco, Institute for Physics and Astronomy University
More informationAstronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 14 The Milky Way Galaxy Lecture Presentation 14.0 the Milky Way galaxy How do we know the Milky Way exists? We can see it even though
More informationThe High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
More informationStars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Lecture Outline A galaxy is a collection of 100 billion stars! Our Milky Way Galaxy (1)Components - HII regions, Dust Nebulae, Atomic Gas (2) Shape & Size (3) Rotation of
More informationLOFAR Key Science Projects and Science Network in Germany
LOFAR Key Science Projects and Science Network in Germany Rainer Beck MPIfR Bonn LOFAR A revolution in radio telescope design: Software telescope: no moving parts, no mirrors, simultaneous multi-beaming,
More informationThe Magnetized Universe
CERN-TH/2003-307 arxiv:astro-ph/0312614v2 10 Mar 2004 The Magnetized Universe Massimo Giovannini 1 CERN, Theoretical Physics Division, CH-1211 Geneva 23, Switzerland Abstract Cosmology, high-energy physics
More informationNumber of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
More information6: Observing Warm Phases: Dispersion ( n e dl ) & Emission ( n
6: Observing Warm Phases: Dispersion ( n e dl ) & Emission ( n 2 e dl ) Measure James R. Graham University of California Berkeley NGC 891 NGC 891 AY 216 2 Techniques & Components The Warm Ionized Medium
More informationAstronomy. Astrophysics. High-resolution radio continuum survey of M 33. III. Magnetic fields
A&A 490, 15 1017 (08) DOI: 10.1051/04-6361:0810590 c ESO 08 Astronomy & Astrophysics High-resolution radio continuum survey of M 33 III. Magnetic fields F. S. Tabatabaei 1,M.Krause 1,A.Fletcher 2, and
More informationMidterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10
Lecture 13 : The Interstellar Medium and Cosmic Recycling Midterm Results A2020 Prof. Tom Megeath The Milky Way in the Infrared View from the Earth: Edge On Infrared light penetrates the clouds and shows
More informationThe Milky Way Galaxy
1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure
More informationReduced MHD. Nick Murphy. Harvard-Smithsonian Center for Astrophysics. Astronomy 253: Plasma Astrophysics. February 19, 2014
Reduced MHD Nick Murphy Harvard-Smithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics February 19, 2014 These lecture notes are largely based on Lectures in Magnetohydrodynamics by Dalton
More informationLecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
More informationStudying Cosmic Magnetism in the Nearby Universe with LOFAR. LOFAR Key Science Project Project Plan
Studying Cosmic Magnetism in the Nearby Universe with LOFAR LOFAR Key Science Project Project Plan P. Alexander 1, J. M. Anderson 2, R. Beck 2, D. J. Bomans 3, M. Brentjens 4,5, A. G. de Bruyn 4,5, K.
More informationLecture 29. Our Galaxy: "Milky Way"
Lecture 29 The Milky Way Galaxy Disk, Bulge, Halo Rotation Curve Galactic Center Apr 3, 2006 Astro 100 Lecture 29 1 Our Galaxy: "Milky Way" Milky, diffuse band of light around sky known to ancients. Galileo
More informationEstimate of an environmental magnetic field of fast radio bursts
Research in Astron. Astrophys. 20XX Vol. X No. XX, 000 000 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Estimate of an environmental magnetic field
More informationThe FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley)
The FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley) w/ Todd Thompson & Eli Waxman Thompson, Quataert, & Waxman 2007, ApJ, 654, 219 Thompson,
More informationCosmic Rays and Magnetic Fields in the ISM
Cosmic Rays and Magnetic Fields in the ISM Cosmic rays -Introduction and history -Observed properties -Ionization rate Magnetic fields -Synchrotron radiation -Faraday rotation -Zeeman splitting -Polarization
More informationThe Norma spiral arm: large-scale pitch angle
The Norma spiral arm: large-scale pitch angle Jacques P. Vallée National Research Council of Canada, National Science Infrastructure, Herzberg Astronomy & Astrophysics, 5071 West Saanich Road, Victoria,
More informationChapter 19: Our Galaxy
Chapter 19 Lecture Chapter 19: Our Galaxy Our Galaxy 19.1 The Milky Way Revealed Our goals for learning: What does our galaxy look like? How do stars orbit in our galaxy? What does our galaxy look like?
More informationS- PASS: a new view of the polarized Sky Polarized Foregrounds for CMB Garching
S- PASS: a new view of the polarized Sky Polarized Foregrounds for CMB Garching EJore CarreK CSIRO ASTRONOMY AND SPACE SCIENCE S- PASS: S- band PolarizaMon All Sky Survey To survey the polarized emission
More informationDark Matter: Observational Constraints
Dark Matter: Observational Constraints Properties of Dark Matter: What is it? And what isn t it? Leo Blitz UC Berkeley Stanford July 31, 2007 How much is there? WMAP results Rotation curves of Galaxies
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Bernard F. Burke Massachusetts Institute of Technology and Francis Graham-Smith Jodrell Bank, University of Manchester CAMBRIDGE UNIVERSITY PRESS Contents Preface Acknowledgements
More informationYou are here! The Solar System! Jo-Anne Brown
You are here! * The Solar System! Jo-Anne Brown Outline Questions! Earth, Moon, Sun A little, teeny, tiny bit of history... Terrestrial planets Gas Giants Poor Pluto Magnetic fields Tell me what you know!
More informationVERY LARGE ARRAY SKY SURVEY
1 VERY LARGE ARRAY SKY SURVEY POLARIZATION (TOMOGRAPHY) Lawrence Rudnick, University of Minnesota Galactic Center (Survey) Multiwavelength Image Credit: X-ray: NASA/UMass/D.Wang et al., Radio: N RAO/AUI/NSF/NRL/N.Kassim,
More informationTowards a New Era of Observing Cosmic Magnetic Fields
Towards a New Era of Observing Cosmic Magnetic Fields Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany E-mail: rbeck@mpifr-bonn.mpg.de The origin of magnetic fields in the
More informationMapping the Galaxy using hydrogen
The Swedish contribution to EU-HOU: A Hands-On Radio Astronomy exercise Mapping the Galaxy using hydrogen Daniel Johansson Christer Andersson Outline Introduction to radio astronomy Onsala Space Observatory
More informationGalaxies and Cosmology
F. Combes P. Boisse A. Mazure A. Blanchard Galaxies and Cosmology Translated by M. Seymour With 192 Figures Springer Contents General Introduction 1 1 The Classification and Morphology of Galaxies 5 1.1
More informationMAGNETIC FIELDS IN NORMAL GALAXIES AND PROSPECTS FOR THE SQUARE KILOMETER ARRAY
MAGNETIC FIELDS IN NORMAL GALAXIES AND PROSPECTS FOR THE SQUARE KILOMETER ARRAY R. BECK Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 53121 Bonn Germany E-mail: rbeck@mpifr-bonn.mpg.de Grand-design,
More informationAccretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants
Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath Review: Creating Stellar Remnants Binaries may be destroyed in white dwarf supernova Binaries be converted into black holes Review: Stellar
More informationFaraday rotation measure synthesis of edge-on galaxy UGC 10288
Faraday rotation measure synthesis of edge-on galaxy UGC 10288 PATRICK KAMIENESKI PI: DANIEL WANG KENDALL SULLIVAN DYLAN PARÉ Extragalactic magnetic fields Global configuration of the disk and halo components
More informationNeutralino Dark Matter as the Source of the WMAP Haze
Neutralino Dark Matter as the Source of the WMAP Haze Gabriel Caceres Penn State University & Fermilab Based on work with Dan Hooper INT Summer School 2009 Dark Matter: The Evidence The Search Direct Detection
More informationChapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
More informationNearby Galaxies at Low Frequencies: Processes and Probes
Nearby Galaxies at Low Frequencies: Processes and Probes May 30 June 2, 2017 List of participants (as of May 10, 2017) 1. Aalto Susanne, Chalmers Univ. of Technology, Sweden 2. Basu Aritra, Max-Planck
More informationThe interpretation is that gravity bends spacetime and that light follows the curvature of space.
7/8 General Theory of Relativity GR Two Postulates of the General Theory of Relativity: 1. The laws of physics are the same in all frames of reference. 2. The principle of equivalence. Three statements
More information