Particle Acceleration and Radiation from Galaxy Clusters
|
|
- Roderick Waters
- 5 years ago
- Views:
Transcription
1 Particle Acceleration and Radiation from Galaxy Clusters 1,2 in collaboration with Anders Pinzke 3, Torsten Enßlin 4, Volker Springel 4, Nick Battaglia 1, Jon Sievers 1, Dick Bond 1 1 Canadian Institute for Theoretical Astrophysics, Canada 2 Kavli Institute for Theoretical Physics, Santa Barbara 3 Stockholm University, Sweden 4 Max-Planck Institute for Astrophysics, Germany 2 Oct 29 / KITP Conference on Astrophysical Plasmas
2 Outline 1 Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 2 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 3 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence
3 Outline Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 1 Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 2 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 3 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence
4 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters How universal is diffusive shock acceleration (DSA)? What can galaxy clusters teach us about the process of shock acceleration? Cosmological structure formation shock physics complementary to interplanetary and SNR shocks: probing unique regions of DSA parameter space: Mach numbers M with infinitely extended (Mpc) and lasting (Gyr) shocks (observationally z = ) plasma-β factors of β origin and evolution of large scale magnetic fields and nature of turbulent models in a cleaner environment (1-phase medium) consistent picture of non-thermal processes in galaxy clusters (radio, soft/hard X-ray, γ-ray emission) illuminating the process of structure formation history of individual clusters: cluster archeology
5 Shocks in galaxy clusters Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 1E 67-6 ( Bullet cluster ) (X-ray: NASA/CXC/CfA/M.Markevitch et al.; Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe et al.; Lensing: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al.) Abell 3667 (radio: Johnston-Hollitt. X-ray: ROSAT/PSPC.)
6 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Radiative simulations with GADGET flowchart CP, Enßlin, Springel (28)
7 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Radiative simulations with cosmic ray (CR) physics CP, Enßlin, Springel (28)
8 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Diffusive shock acceleration Fermi 1 mechanism (1) Spectral index depends on the Mach number of the shock, M = υ shock /c s : log f strong shock weak shock kev 1 GeV log p
9 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Diffusive shock acceleration efficiency (2) CR proton energy injection efficiency, ζ inj = ε CR /ε diss : CR energy injection efficiencyζinj Mach numberm 11/3 3 kt 2 = 1 kev kt 2 =.3 kev kt 2 =.1 kev α inj 3. 4.
10 Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Radiative cool core cluster simulation: gas density y [ h -1 Mpc ] δgas x [ h -1 Mpc ]
11 Cosmological simulations with cosmic rays Mass weighted temperature 1 1 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 1 8 y [ h -1 Mpc ] Tρgas / ρgas [K] x [ h -1 Mpc ] 1
12 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Mach number distribution weighted by ε diss y [ h -1 Mpc ] - M εdiss/ εdiss x [ h -1 Mpc ] 1
13 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Mach number distribution weighted by ε CR,inj y [ h -1 Mpc ] - M εcr,inj / εcr,inj x [ h -1 Mpc ] 1
14 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters CR pressure P CR y [ h -1 Mpc ] PCRρgas / ρgas [erg cm 3 h 2 7 ] x [ h -1 Mpc ] 1-17
15 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Relative CR pressure P CR /P total y [ h -1 Mpc ] PCR/Ptot ρgas / ρgas x [ h -1 Mpc ] 1-2
16 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Multi messenger approach for non-thermal processes
17 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Multi messenger approach for non-thermal processes
18 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Multi messenger approach for non-thermal processes
19 Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters Multi messenger approach for non-thermal processes
20 Non-thermal emission from clusters Exploring the memory of structure formation Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters primary, shock-accelerated CR electrons resemble current accretion and merging shock waves CR protons/hadronically produced CR electrons trace the time integrated non-equilibrium activities of clusters that is modulated by the recent dynamical activities How can we read out this information about non-thermal populations? new era of multi-frequency experiments, e.g.: GMRT, LOFAR, MWA, LWA, SKA: interferometric array of radio telescopes at low frequencies (ν (1 24) MHz) Simbol-X/NuSTAR: future hard X-ray satellites (E (1 1) kev) Fermi γ-ray space telescope (E (.1 3) GeV) Imaging air Čerenkov telescopes (E (.1 1) TeV)
21 Non-thermal emission from clusters Exploring the memory of structure formation Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters primary, shock-accelerated CR electrons resemble current accretion and merging shock waves CR protons/hadronically produced CR electrons trace the time integrated non-equilibrium activities of clusters that is modulated by the recent dynamical activities How can we read out this information about non-thermal populations? new era of multi-frequency experiments, e.g.: GMRT, LOFAR, MWA, LWA, SKA: interferometric array of radio telescopes at low frequencies (ν (1 24) MHz) Simbol-X/NuSTAR: future hard X-ray satellites (E (1 1) kev) Fermi γ-ray space telescope (E (.1 3) GeV) Imaging air Čerenkov telescopes (E (.1 1) TeV)
22 Outline Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 1 Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 2 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 3 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence
23 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus CR proton and γ-ray spectrum (Pinzke & CP 29) 1. f(p) p Fγ(> Eγ)Eγ [GeV cm 2 s 1 ] p = P p / (m p c) sic pic Pion decay E γ [ GeV ]
24 Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Hadronic γ-ray emission, E γ > 1 GeV y [ Mpc ] S γ (E γ > 1 GeV) [ ph cm -2 s -1 ] x [ Mpc ] 1-12
25 Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Inverse Compton emission, E IC > 1 GeV y [ Mpc ] S IC,total (E γ > 1 GeV) [ ph cm -2 s -1 ] x [ Mpc ] 1-12
26 Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Total γ-ray emission, E γ > 1 GeV y [ Mpc ] S total (E γ > 1 GeV) [ ph cm -2 s -1 ] x [ Mpc ] 1-12
27 ] ] Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Correlation between thermal X-ray and γ-ray emission 1-4 merger, 1 1 h -1 M O : merger, 1 1 h -1 M O : S γ (> 1 MeV) [ γ cm -2 s -1 h correlation space density [arbitrary units] S γ (> 1 MeV) [ γ cm -2 s -1 h correlation space density [arbitrary units] S X [ erg cm -2 s -1 h 3 7 ] S X [ erg cm -2 s -1 h 3 7 ] Correlation with pion decay/sec. IC emission, X-ray and secondary emission n 2 (CP, Enßlin, Springel 28) Correlation with primary IC emission, correlation space substructure oblique curved shocks; B-generation!
28 Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Photon index Γ - variations on large scales y [ Mpc ] Γ (1 MeV, 1 GeV) y [ Mpc ] Γ (1 GeV, 1 TeV) x [ Mpc ] x [ Mpc ] 1. Γ 1 1 GeV MeV (Fermi): pion bump (center) transition to pic (strong accretion shocks) Γ 1 1 TeV (IACT s): pion-decay (center) GeV pic (accretion shocks, cutoff E max)
29 Universal CR spectrum in clusters Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 1 1 Fermi: α p ~ 2. < f(p) p 2 >.1 IACT: α p ~ p Normalized CR spectrum shows universal concave shape governed by hierarchical structure formation and the implied distribution of Mach numbers that a fluid element had to pass through in cosmic history (Pinzke & CP 29).
30 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus An analytic model for the cluster γ-ray emission Comparison: simulation vs. analytic model, M vir (1 14, 1 1 ) M pion decay profile: simulation analytic model pion decay spectrum: simulation analytic model s -1 ] λ γ (r, Eγ = 1 MeV) [ph cm g914 g72a Fγ(> Eγ)Eγ [GeV cm 2 s 1 ] g914 g72a λ γ / λ γ R / R vir Spatial γ-ray emission profile Fγ/Fγ E γ [ GeV ] Pion decay spectrum
31 Gamma-ray scaling relations Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 1 46 total γ-ray emission, excl. galaxies, R<R vir pion-decay γ-ray emission primary IC emission secondary IC emission L γ (E γ > 1 MeV) [ ph s -1 ] M vir [ M O ] Scaling relation + complete sample of the brightest X-ray clusters (HIFLUGCS) predictions for Fermi and IACT s
32 Cosmological simulations with cosmic rays Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Predicted cluster sample for Fermi and IACT s Fγ(Eγ> 1 MeV) CRs with galaxies CRs witout galaxies FORNAX A74 A16 A326 COMA AWM7 PERSEUS 3C129 M49 A3627 OPHIUCHU Fγ(Eγ> 1 GeV) extended HIFLUGCS cluster ID black: optimistic model, including galactic point sources that bias γ-ray flux high; red: realistic model, excluding galactic point sources
33 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Predicted cluster sample for Fermi brightest objects 14 excl. galaxies 12 1 Nclusters C129 A3626, A16 Fornax A3627, Perseus Coma Ophiuchus F γ [ph cm 2 s 1 ]
34 MAGIC observations of Perseus Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus
35 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Upper limit on the TeV γ-ray emission from Perseus radiative physics w/ gal. x 3. radiative physics w/ gal. radiative physics w/o gal. F γ, min (B = 1 µg, ε B < ε th / 3) F γ ( >E ) [ph s -1 cm -2 ] E [GeV] The MAGIC Collaboration: Aleksic et al. & CP et al. 29
36 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Results from the Perseus observation by MAGIC assuming f p α with α = 2.1, P CR P th : E CR <.17E th most stringent constraint on CR pressure! upper limits consistent with cosmological simulations: F upper limits (1GeV ) = 3. F sim (optimistic model) simulation modeling of pressure constraint yields P CR / P th <.7 (.14) for the core (entire cluster) 3 physical effects that resolve the apparent discrepancy: concave curvature hides CR pressure at GeV energies galactic point sources bias γ-ray flux high and pressure limits low (partly physical) relative CR pressure increases towards the outer parts (adiabatic compression and softer equation of state of CRs)
37 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Minimum γ-ray flux in the hadronic model jν,ic(b)/ jν,ic(bcmb) jic(b)/ jic(bcmb) jν(b)/ jν(bcmb) For jν(b) : αν= 1 αν= 1.1 αν= 1.3 αν= B[µG] Synchrotron emissivity of highenergy, steady state electron distribution is independent of the magnetic field for B B CMB! Synchrotron luminosity: ε (αν+1)/2 B L ν = A ν dv n CR n gas ε CMB + ε B A ν dv n CR n gas (ε B ε CMB ) γ-ray luminosity: L γ = A γ dv n CR n gas minimum γ-ray flux: F γ,min = A γ L ν A ν 4πD 2
38 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Minimum γ-ray flux in the hadronic model jν,ic(b)/ jν,ic(bcmb) jic(b)/ jic(bcmb) jν(b)/ jν(bcmb) For jν(b) : αν= 1 αν= 1.1 αν= 1.3 αν= B[µG] Synchrotron emissivity of highenergy, steady state electron distribution is independent of the magnetic field for B B CMB! Synchrotron luminosity: ε (αν+1)/2 B L ν = A ν dv n CR n gas ε CMB + ε B A ν dv n CR n gas (ε B ε CMB ) γ-ray luminosity: L γ = A γ dv n CR n gas minimum γ-ray flux: F γ,min = A γ L ν A ν 4πD 2
39 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Minimum γ-ray flux in the hadronic model: Fermi Minimum γ-ray flux (E γ > 1 MeV) for the Coma cluster: CR spectral index F γ [1 1 ph cm 2 s 1 ] These limits can be made even tighter when considering energy constraints, P B < P gas /3 and B-fields derived from Faraday rotation studies, B = 3 µg: F γ,coma ( ) 1 9 γ cm 2 s 1 F Fermi, 2yr Non-detection by Fermi seriously challenges the hadronic model. Potential of measuring the CR acceleration efficiency for diffusive shock acceleration.
40 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus Minimum γ-ray flux in the hadronic model: IACT s Minimum γ-ray flux (E γ > 1 GeV) for the Coma cluster: CR spectral index F γ [1 14 ph cm 2 s 1 ] These limits can be made even tighter when considering energy constraints, P B < P gas /3, FRM B-fields with B = 3 µg, and α p < 2.3 (caution: this assumes a power-law scaling): F γ,coma ( ) 1 13 γ cm 2 s 1 Potential of measuring the CR spectrum, the effective acceleration efficiency for diffusive shock acceleration, and relate this to the history of structure formation shock waves (Mach number distribution).
41 Outline Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence 1 Cosmological simulations with cosmic rays Motivation and observations Cosmological galaxy cluster simulations Non-thermal processes in clusters 2 Spectra and morphology Predictions for Fermi and IACT s MAGIC observations of Perseus 3 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence
42 Cosmological simulations with cosmic rays Cosmic web: Mach number 1 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence 1 1 y [ h -1 Mpc ] - M εdiss/ εdiss x [ h -1 Mpc ] 1
43 ] Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Radio gischt (relics): primary CRe (1.4 GHz) y [ h -1 Mpc ] S ν,primary [ mjy arcmin -2 h x [ h -1 Mpc ] 1-8
44 ] Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Radio gischt: primary CRe (1 MHz) y [ h -1 Mpc ] S ν,primary [ mjy arcmin -2 h x [ h -1 Mpc ] 1-8
45 ] Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Radio gischt: primary CRe (1 MHz) y [ h -1 Mpc ] S ν,primary [ mjy arcmin -2 h x [ h -1 Mpc ] 1-8
46 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence ] Radio gischt: primary CRe (1 MHz), slower magnetic decline y [ h -1 Mpc ] S ν,primary [ mjy arcmin -2 h x [ h -1 Mpc ] 1-8
47 Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Radio gischt illuminates cosmic magnetic fields y [ h -1 Mpc ] 2 M εdiss / εdiss y [ h -1 Mpc ] x [ h -1 Mpc ] Structure formation shocks triggered by a recent merger of a large galaxy cluster x [ h -1 Mpc ] red/yellow: shock-dissipated energy, blue/contours: 1 MHz radio gischt emission from shock-accelerated CRe
48 The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Diffuse cluster radio emission an inverse problem Exploring the magnetized cosmic web Battaglia, CP, Sievers, Bond, Enßlin (28): By suitably combining the observables associated with diffuse polarized radio emission at low frequencies (ν 1 MHz, GMRT/LOFAR/MWA/LWA), we can probe the strength and coherence scale of magnetic fields on scales of galaxy clusters, the process of diffusive shock acceleration of electrons, the existence and properties of the WHIM, the exploration of observables beyond the thermal cluster emission which are sensitive to the dynamical state of the cluster.
49 Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Population of faint radio relics in merging clusters Probing the large scale magnetic fields Finding radio relics in 3D cluster simulations using a friends-of-friends finder with an emission threshold relic luminosity function y [ h -1 Mpc ] S ν [ mjy arcmin -2 ] y [ h -1 Mpc ] S ν [ mjy arcmin -2 ] x [ h -1 Mpc ] radio map with GMRT emissivity threshold x [ h -1 Mpc ] theoretical threshold (towards SKA) 1-3
50 Relic luminosity function theory The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence Relic luminosity function is very sensitive to large scale behavior of the magnetic field and dynamical state of cluster: F ν [mjy] for a z ~ F ν [mjy] for a z ~ ν = 1MHz, B = µg α B =.3 α B =. α B =.7 α B =.9 1 ν = 1MHz, α B =. B = 1 µg B = µg B = 2. µg Number of relics Number of relics ), Jν= 1 erg/hz/s/ster log(jν/jν varying magnetic decline with radius ), Jν= 1 erg/hz/s/ster log(jν/jν varying overall normalization of the magnetic field
51 Rotation measure (RM) The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence.4.2 RM maps and power spectra have the potential to infer the magnetic pressure support and discriminate the nature of MHD turbulence in clusters: arcmin [rad 2 m -4 ] P [RM](k) k 2 1 P [RM] (k) P [Bz ] (k) 1-6 P [Bz ](k) k 2 [µg 2 Mpc] y [ Mpc ] arcmin -7 RM [ rad m -2 ] P [RM](k) k 2 [rad 2 m -4 ] 1 1 MFR1 MFR2 MFR x [ Mpc ] k [h Mpc -1 ] Left: RM map of the largest relic, right: Magnetic and RM power spectrum comparing Kolmogorow and Burgers turbulence models.
52 Conclusions Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence In contrast to the thermal plasma, the non-equilibrium distributions of CRs preserve the information about their injection and transport processes and provide thus a unique window of current and past structure formation processes and diffusive shock acceleration! 1 Universal distribution of CR protons determined by maximum shock acceleration efficiency ζ max and adiabatic transport: mapping between the hadronic γ-ray emission and ζ max cosmological simulations are indispensable for exploring this (non-linear) map spectral shape illuminates the process of structure formation 2 Primary radio (gischt) emission traces the magnetized cosmic web; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allows determining the nature of the intra-cluster turbulence
53 Conclusions Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence In contrast to the thermal plasma, the non-equilibrium distributions of CRs preserve the information about their injection and transport processes and provide thus a unique window of current and past structure formation processes and diffusive shock acceleration! 1 Universal distribution of CR protons determined by maximum shock acceleration efficiency ζ max and adiabatic transport: mapping between the hadronic γ-ray emission and ζ max cosmological simulations are indispensable for exploring this (non-linear) map spectral shape illuminates the process of structure formation 2 Primary radio (gischt) emission traces the magnetized cosmic web; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allows determining the nature of the intra-cluster turbulence
54 Conclusions Cosmological simulations with cosmic rays The cosmic magnetized web Properties of cluster magnetic fields Cluster turbulence In contrast to the thermal plasma, the non-equilibrium distributions of CRs preserve the information about their injection and transport processes and provide thus a unique window of current and past structure formation processes and diffusive shock acceleration! 1 Universal distribution of CR protons determined by maximum shock acceleration efficiency ζ max and adiabatic transport: mapping between the hadronic γ-ray emission and ζ max cosmological simulations are indispensable for exploring this (non-linear) map spectral shape illuminates the process of structure formation 2 Primary radio (gischt) emission traces the magnetized cosmic web; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allows determining the nature of the intra-cluster turbulence
Cosmic Rays in Galaxy Clusters Simulations and Reality
Simulations and Reality 1,2 in collaboration with Torsten Enßlin 3, Volker Springel 3, Anders Pinzke 4, Nick Battaglia 1, Jon Sievers 1, Dick Bond 1 1 Canadian Institute for Theoretical Astrophysics, Canada
More informationCosmic Rays in Galaxy Clusters: Simulations and Perspectives
Cosmic Rays in Galaxy Clusters: Simulations and Perspectives 1 in collaboration with Volker Springel 2, Torsten Enßlin 2 1 Canadian Institute for Theoretical Astrophysics, Canada 2 Max-Planck Institute
More informationLiterature on which the following results are based:
Cosmic rays in galaxy clusters Physical processes in galaxy clusters High-resolution simulations of galaxy clusters Literature on which the following results are based: Pfrommer, 28, MNRAS, in print, ArXiv:77.1693,
More informationCosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation
Cosmic ray feedback in hydrodynamical simulations of galaxy and structure formation Canadian Institute for Theoretical Astrophysics, Toronto April, 13 26 / Workshop Dark halos, UBC Vancouver Outline 1
More informationCosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation
Cosmic ray feedback in hydrodynamical simulations of galaxy and structure formation Canadian Institute for Theoretical Astrophysics, Toronto April, 11 26 / Colloquium University of Victoria Outline 1 Cosmic
More informationFermi-LAT Analysis of the Coma Cluster
Fermi-LAT Analysis of the Coma Cluster a Fabio Zandanel GRAPPA Institute University of Amsterdam f.zandanel@uva.nl In collaboration with S. Ando (GRAPPA) 18 th Symposium on Astroparticle Physics in the
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 informationParticle Acceleration in the Universe
Particle Acceleration in the Universe Hiroyasu Tajima Stanford Linear Accelerator Center Kavli Institute for Particle Astrophysics and Cosmology on behalf of SLAC GLAST team June 7, 2006 SLAC DOE HEP Program
More informationDynamics of galaxy clusters A radio perspective
Dynamics of galaxy clusters A radio perspective Tiziana Venturi, INAF, Istituto di Radioastronomia Collaborators S. Giacintucci, D. Dallacasa, R. Kale, G. Brunetti, R. Cassano, M. Rossetti GEE 3 Padova,
More informationIntracluster Shock Waves
ρ Intracluster Shock Waves T R 200 Dongsu Ryu (UNIST, Ulsan National Institute of Science and Technology, Korea) Hyesung Kang (Pusan National U, Korea) Sungwook E. Hong (Korea Institute for Advanced Study)
More informationTHE MAGIC TELESCOPES. Major Atmospheric Gamma Imaging Cherenkov Telescopes
THE MAGIC TELESCOPES Observatorio del Roque de los Muchachos, La Palma (2200 m a.s.l.) System of two 17 m Cherenkov Telescopes for VHE γ-ray astronomy MAGIC-I operational since 2004, Stereo system since
More informationLOFAR Observations of Galaxy Clusters
LOFAR Observations of Galaxy Clusters The Toothbrush Radio Relic Reinout van Weeren Harvard-Smithsonian Center for Astrophysics M. Brüggen, G. Brunetti, H. Röttgering F. de Gasperin, A. Bonafede, W. Forman,
More informationFormation and properties of shock waves in galaxy clusters
Formation and properties of shock waves in galaxy clusters Hyesung Kang (Pusan National University) Dongsu Ryu (UNIST, Korea) T. W. Jones (Univ. of Minnesota) Sungwook E. Hong (KAIST, Korea) Ref: Kang,
More informationGamma-ray Observations of Galaxy Clusters!
Gamma-ray Observations of Galaxy Clusters! a! Fabio Zandanel! (GRAPPA Institute University of Amsterdam)! f.zandanel@uva.nl! SnowCluster 2015 The Physics Of Galaxy Clusters! Snowbird (Utah, US) March 15-20,
More informationRadio relis (and halos) in galaxy clusters
Radio relis (and halos) in galaxy clusters Matthias Hoeft Thüringer Landessternwarte Tautenburg - overall spectrum of relics - relic statistics - an unusual radio halo Radio relic: the textbook example
More informationUri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 2008
Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Relaxed, cool
More informationThe role of Planck in understanding galaxy cluster radio halos
The role of Planck in understanding galaxy cluster radio halos Radio data Radio data Planck measurements Planck measurements 1 The role of Planck in understanding galaxy cluster radio halos Kaustuv Basu
More informationRadio relics and magnetic field amplification in the Intra-cluster Medium
Radio relics and magnetic field amplification in the Intra-cluster Medium Annalisa Annalisa Bonafede Bonafede Hamburger Hamburg Sternwarte University Hamburg University Jacobs University Bremen Collaborators:
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 informationCosmic Ray Astronomy. Qingling Ni
Cosmic Ray Astronomy Qingling Ni What is Cosmic Ray? Mainly charged particles: protons (hydrogen nuclei)+helium nuclei+heavier nuclei What s the origin of them? What happened during their propagation?
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 informationA New View of the High-Energy γ-ray Sky with the Fermi Telescope
A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11
More informationProbing Cosmic Hadron Colliders with hard X-ray detectors of ASTRO-H
Probing Cosmic Hadron Colliders with hard X-ray detectors of ASTRO-H F.A. Aharonian, DIAS (Dublin) & MPIK (Heidelberg) ASTRO-H SWG Meeting, ISAS, Tokyo, Feb 25-26, 2009 X-rays - tracers of high energy
More informationAGN Outflows in Dynamic ICMs: Winds and Twists
AGN Outflows in Dynamic ICMs: Winds and Twists Tom Jones University of Minnesota Pete Mendygral (UMN, Cray Computer) David Porter (UMN) Klaus Dolag (MPA, U Munich) 11/29/2012 Binary Black Holes & Dual
More informationFermi: Highlights of GeV Gamma-ray Astronomy
Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy
More informationGamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
More informationEmmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile,
Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile, Italy Emmanuel Moulin CTA meeting, Zürich 2009 1 Core-energy
More informationCTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters
CTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters Moritz Hütten (MPP Munich) for the CTA consortium "The extreme Universe viewed in very-highenergy
More informationGiant cosmic tsunamis:
Giant cosmic tsunamis: reconciling observations and models of cluster radio relics Andra Stroe ESO Fellow astroe@eso.org Twitter: @Andra_Stroe www.eso.org/~astroe From Oct Clay Fellow T. Shimwell, C. Rumsey,
More informationX-ray and radio observations of the radio relic galaxy clusters 1RXS J and RXC J
X-ray and radio observations of the radio relic galaxy clusters 1RXS J0603.3+4214 and RXC J1053.7+5453 Motokazu Takizawa (Yamagata University) Itahana, Takizawa, Akamatsu et al. (2015), PASJ, 67, 113 Itahana,
More informationPoS(ICRC2017)283. Acceleration of Cosmic Ray Electrons at Weak Shocks in Galaxy Clusters. Hyesung Kang. Dongsu Ryu
Acceleration of Cosmic Ray Electrons at Weak Shocks in Galaxy Clusters Pusan National University E-mail: hskang@pusan.ac.kr Dongsu Ryu UNIST E-mail: ryu@sirius.unist.ac.kr T. W. Jones University of Minnesota
More informationOccurrence of Radio Halos in galaxy clusters Insight from a mass-selected sample Virginia Cuciti
Occurrence of Radio Halos in galaxy clusters Insight from a mass-selected sample Virginia Cuciti In collaboration with: Gianfranco Brunetti, Rossella Cassano, Daniele Dallacasa Coma WSRT radio contours
More informationMergers and Radio Sources in Abell 3667 and Abell 2061
Mergers and Radio Sources in Abell 3667 and Abell 2061 Craig Sarazin University of Virginia A3667 XMM X-ray image and radio contours SLAM Simulation of A2061 Collaborators Alexis Finoguenov (MPE, UMBC)
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 informationSimulating the gamma-ray emission from galaxy clusters: a universal cosmic ray spectrum and spatial distribution
Mon. Not. R. Astron. Soc. 000, 1 33 (2008) Printed 29 May 2018 (MN LATEX style file v2.2) Simulating the gamma-ray emission from galaxy clusters: a universal cosmic ray spectrum and spatial distribution
More informationA few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda
A few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda Radio/X constraints on CSM around SNe Ia Useful limit for SN 2011fe: Mdot/v w < ~10-8 M yr -1 /100km s -1 Radio Chomiuk+
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 informationGalaxy Clusters with Swift/BAT
Galaxy Clusters with Swift/BAT Marco Ajello [KIPAC/SLAC] with Paola Rebusco (MIT), Nico Cappelluti(MPE), Olaf Reimer (UIBK), Hans Böhringer (MPE) Outline Why studying clusters at high energies? The BAT
More informationMergers and Non-Thermal Processes in Clusters of Galaxies
Mergers and Non-Thermal Processes in Clusters of Galaxies Craig Sarazin University of Virginia A85 Chandra A133 Chandra and VLA Collaborators Liz Blanton, Tracy Clarke, Scott Randall, Thomas Reiprich (UVa)
More informationNUMERICAL STUDY OF NON-THERMAL EMISSION FROM LAGRANGIAN PARTICLES IN AGN ENVIRONMENTS.
13th AGILE Workshop, ASI, Rome May 25, 2015 NUMERICAL STUDY OF NON-THERMAL EMISSION FROM LAGRANGIAN PARTICLES IN AGN ENVIRONMENTS. Dr. Bhargav Vaidya Università degli Studi di Torino, Torino. Collaborators:
More informationCosmic Accelerators. 2. Pulsars, Black Holes and Shock Waves. Roger Blandford KIPAC Stanford
Cosmic Accelerators 2. Pulsars, Black Holes and Shock Waves Roger Blandford KIPAC Stanford Particle Acceleration Unipolar Induction Stochastic Acceleration V ~ Ω Φ I ~ V / Z 0 Z 0 ~100Ω P ~ V I ~ V 2 /Z
More informationConstraints on cosmic-ray origin from gamma-ray observations of supernova remnants
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Marianne Lemoine-Goumard (CENBG, Université Bordeaux, CNRS-IN2P3, France) On behalf of the Fermi-LAT and HESS Collaborations
More informationCosmic Ray acceleration in clusters of galaxies. Gianfranco Brunetti. Istituto di Radioastronomia INAF, Bologna, ITALY
Cosmic Ray acceleration in clusters of galaxies Gianfranco Brunetti Istituto di Radioastronomia INAF, Bologna, ITALY Outline NT components (CRe,CRp,B) in galaxy clusters : observations Physics and dynamics
More informationHard X-ray emission from Novae
Hard X-ray emission from Novae Indrek Vurm (Columbia University) in collaboration with: Brian D. Metzger, Andrei M. Beloborodov (Columbia) Koji Mukai (NASA) Shocks and Particle Acceleration in Novae and
More informationObservations of diffuse radio emission in cool-core clusters
Observations of diffuse radio emission in cool-core clusters Simona Giacintucci U.S. Naval Research Laboratory Maxim Markevitch (GSFC), Tracy Clarke (NRL), Tiziana Venturi (INAF-IRA), Rossella Cassano
More informationTwo Topics: Prospects of detection of Hard X- rays from I. Active Cool Stars, II. Clusters of galaxies. K.P. Singh (TIFR, Mumbai)
Two Topics: Prospects of detection of Hard X- rays from I. Active Cool Stars, ì II. Clusters of galaxies LAXPC Workshop @ Hyderabad December 15 17, 2014 K.P. Singh (TIFR, Mumbai) The Sun an active star
More informationMULTIWAVELENGTH OBSERVATIONS OF CLUSTERS OF GALAXIES AND THE ROLE OF CLUSTER MERGERS PASQUALE BLASI
MULTIWAVELENGTH OBSERVATIONS OF CLUSTERS OF GALAXIES AND THE ROLE OF CLUSTER MERGERS PASQUALE BLASI NASA/Fermilab Astrophysics Center Fermi National Accelerator Laboratory, Box 500, Batavia, IL 60510-0500,
More informationParticle acceleration and pulsars
Meudon, nov. 2013 p. 1/17 Particle acceleration and pulsars Fabrice Mottez LUTH - Obs. Paris-Meudon - CNRS - Univ. Paris Diderot Meudon, nov. 2013 p. 2/17 Pulsars (PSR) and pulsar wind nebulae (PWNe) Mostly
More informationRadio emission in clusters of galaxies. An observational perspective
Radio emission in clusters of galaxies An observational perspective Tiziana Venturi INAF, IRA, Bologna IV ESTRELA Workshop, Bologna, 19 January 2009 Overview - What are galaxy clusters - Radio emission
More informationUltra High Energy Cosmic Rays I
Ultra High Energy Cosmic Rays I John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020 ev. Problem: the microwave background radiation is discovered
More informationGalactic Novae Simulations for the Cherenkov Telescope Array
Galactic Novae Simulations for the Cherenkov Telescope Array REU Final Presentation August 4, 2017 Colin Adams Primary Mentors: Brian Humensky, Deivid Ribeiro Outline Introduction Why and how do we study
More informationStructure of Dark Matter Halos
Structure of Dark Matter Halos Dark matter halos profiles: DM only: NFW vs. Einasto Halo concentration: evolution with time Dark matter halos profiles: Effects of baryons Adiabatic contraction Cusps and
More informationUltra High Energy Cosmic Rays. UHECRs from Mildly Relativistic Supernovae
Ultra High Energy Cosmic Rays from Mildly Relativistic Supernovae Tata Institute of Fundamental Research Mumbai, India March 13, 2012 Outline UHECRS Chakraborti, Ray, Soderberg, Loeb, Chandra 2011 Nature
More informationRemnants and Pulsar Wind
High Energy Supernova Remnants and Pulsar Wind Nebulae F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari For the Fermi-LAT Collaboration Scineghe 2010 The Afterlife of a star IC443 Crab
More informationUltrahigh Energy Cosmic Rays propagation II
Ultrahigh Energy Cosmic Rays propagation II The March 6th lecture discussed the energy loss processes of protons, nuclei and gamma rays in interactions with the microwave background. Today I will give
More informationHigh energy neutrino signals from NS-NS mergers
High energy neutrino signals from NS-NS mergers He Gao 高鹤 University of Nevada Las Vegas Collaborators: Bing Zhang, Xue-Feng Wu & Zi-Gao Dai 2013-05-08 Multi-Messenger Workshop @ KIAA EM signals for a
More informationThe Plasma Physics and Cosmological Impact of TeV Blazars
The Plasma Physics and Cosmological Impact of TeV Blazars Philip Chang (UW-Milwaukee) Avery Broderick (Waterloo/Perimeter) Astrid Lamberts (UW-Milwaukee) Christoph Pfrommer (HITS-Heidelberg) Ewald Puchwein
More informationPoS(EXTRA-RADSUR2015)063
Constraining magnetic fields and particle acceleration processes in galaxy clusters: a joint VLA/LOFAR view on Coma and SKA perspectives Hamburger Sternwarte,Universität Hamburg, Gojenbergsweg 112,21029
More informationPERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
More informationNonthermal Emission in Starburst Galaxies
Nonthermal Emission in Starburst Galaxies! Yoel Rephaeli!!! Tel Aviv University & UC San Diego Cosmic Ray Origin! San Vito, March 20, 2014 General Background * Stellar-related nonthermal phenomena * Particle
More informationParticle acceleration in Supernova Remnants
Particle acceleration in Supernova Remnants Anne Decourchelle Service d Astrophysique, CEA Saclay Collaborators: J. Ballet, G. Cassam-Chenai, D. Ellison I- Efficiency of particle acceleration at the forward
More informationKathrin Egberts Max-Planck-Institut für Kernphysik, Heidelberg for the H.E.S.S. Collaboration
Kathrin Egberts Max-Planck-Institut für Kernphysik, Heidelberg for the H.E.S.S. Collaboration Outline The H.E.S.S. Experiment The H.E.S.S. Electron Measurement Gamma-Ray Background Hadronic Background
More informationarxiv:astro-ph/ v1 19 Mar 2007
Galaxy Clusters in the Radio: Relativistic Plasma and ICM/Radio Galaxy Interaction Processes arxiv:astro-ph/0703494v1 19 Mar 2007 Luigina Feretti 1 and Gabriele Giovannini 1,2 1 Istituto di Radioastronomia
More informationConstraining primordial magnetic fields with observations
Constraining primordial magnetic fields with observations Kerstin Kunze (University of Salamanca and IUFFyM) KK PRD 83 (2011) 023006; PRD 85 (2012) 083004; PRD 87 (2013) 103005; PRD 89 (2014) 103016, arxiv:1703.03650
More informationMULTIMESSENGER APPROACH:Using the Different Messengers
MULTIMESSENGER APPROACH:Using the Different Messengers PROTONS p NUCLEI (A,Z) NEUTRINOS νµ PHOTONS LECTURE PLAN: 1) COSMIC RAYS- proton interactions with photons, composition, nuclei interactions with
More informationTurbulence & particle acceleration in galaxy clusters. Gianfranco Brunetti
Turbulence & particle acceleration in galaxy clusters Gianfranco Brunetti Mergers & CR-acceleration Cluster-cluster mergers are the most energetic events in the present Universe (10 64 erg/gyr). They can
More informationEnrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3
Enrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3 Craig Sarazin Dept. of Astronomy University of Virginia A85 Chandra (X-ray) Cluster Merger Simulation Cool Cores in Clusters Central
More informationThe Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events
More information80 2 Observational Cosmology L and the mean energy
80 2 Observational Cosmology fluctuations, short-wavelength modes have amplitudes that are suppressed because these modes oscillated as acoustic waves during the radiation epoch whereas the amplitude of
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 information> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!
> News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May
More informationShocks in the ICM and the IPM
Shocks in the ICM and the IPM Tom Jones (University of Minnesota) 1 Outline Setting the stage for following talks The Interplanetary and Intracluster Media as Collisionless Plasmas Basic Introduction to
More informationMagnetic Fields (and Turbulence) in Galaxy Clusters
Magnetic Fields (and Turbulence) in Galaxy Clusters Dongsu Ryu (UNIST, Ulsan National Institute of Science and Technology, Korea) with Hyesung Kang (Pusan Nat. U, Korea), Jungyeon Cho (Chungnam Nat. U.),
More informationRecent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
More informationVHE emission from radio galaxies
VHE emission from radio galaxies Martin Hardcastle The future of gamma-ray astronomy and the CTA Leicester, October 2010 Outline Recap: radio galaxy physics Inverse-Compton emission Locations of high-energy
More informationCosmic Ray Electrons and GC Observations with H.E.S.S.
Cosmic Ray Electrons and GC Observations with H.E.S.S. Christopher van Eldik (for the H.E.S.S. Collaboration) MPI für Kernphysik, Heidelberg, Germany TeVPA '09, SLAC, July 2009 The Centre of the Milky
More informationMulti-Messenger Astonomy with Cen A?
Multi-Messenger Astonomy with Cen A? Michael Kachelrieß NTNU, Trondheim [] Outline of the talk 1 Introduction 2 Dawn of charged particle astronomy? Expectations vs. Auger data Effects of cluster fields
More information99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR
More informationVERITAS Observations of Starburst Galaxies. The Discovery of VHE Gamma Rays from a Starburst Galaxy
VERITAS Observations of Starburst Galaxies The Discovery of VHE Gamma Rays from a Starburst Galaxy Wystan Benbow for the VERITAS Collaboration 1 Harvard-Smithsonian Center for Astrophysics 1 see R.A. Ong
More informationSupernova Remnants and GLAST
SLAC-PUB-14797 Supernova Remnants and GLAST Patrick Slane Harvard-Smithsonian Center for Astrophysics Abstract. It has long been speculated that supernova remnants represent a major source of cosmic rays
More informationRelativistic jets from XRBs with LOFAR. Stéphane Corbel (University Paris 7 & CEA Saclay)
Relativistic jets from XRBs with LOFAR. Stéphane Corbel (University Paris 7 & CEA Saclay) Outline Introduction: X-ray binaries and flavors of relativistic jets LOFAR Contributions Conclusions Introduction:
More informationShell supernova remnants as cosmic accelerators: II
Shell supernova remnants as cosmic accelerators: II Stephen Reynolds, North Carolina State University I. Observational tools II. Radio inferences III. X ray synchrotron emission IV. MeV GeV observations
More informationCosmic Rays, Photons and Neutrinos
Cosmic Rays, Photons and Neutrinos Michael Kachelrieß NTNU, Trondheim [] Introduction Outline Plan of the lectures: Cosmic rays Galactic cosmic rays Basic observations Acceleration Supernova remnants Problems
More informationFermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars
Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Marie-Hélène Grondin CENBG, Bordeaux (France) on behalf of the Fermi-LAT Collaboration and the Pulsar Timing
More informationNeutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002
Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays
More informationGamma-ray emission from nova outbursts
Gamma-ray emission from nova outbursts Margarita Hernanz Institute of Space Sciences - ICE (CSIC-IEEC) Bellaterra (Barcelona), Spain Stella Novae: Past and Future Decades, Cape Town, 4-8/2/2013 M. Hernanz
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 informationEXCESS OF VHE COSMIC RAYS IN THE CENTRAL 100 PC OF THE MILKY WAY. Léa Jouvin, A. Lemière and R. Terrier
1 EXCESS OF VHE COSMIC RAYS IN THE CENTRAL 100 PC OF THE MILKY WAY Léa Jouvin, A. Lemière and R. Terrier 2 Excess of VHE cosmic rays (CRs) γ-ray count map Matter traced by CS 150 pc After subtracting the
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More informationEBL Studies with the Fermi Gamma-ray Space Telescope
EBL Studies with the Fermi Gamma-ray Space Telescope Luis C. Reyes KICP The Extragalactic Background Light (EBL) What is it? Accumulation of all energy releases in the form of electromagnetic radiation.
More informationA pulsar wind nebula associated with PSR J as the powering source of TeV J
A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130 Javier Moldón Netherlands Institute for Radio Astronomy Extreme Astrophysics in an Ever-Changing Universe Crete,
More informationCross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
More informationSpatial Profile of the Emission from Pulsar Wind Nebulae with steady-state 1D Modeling
Spatial Profile of the Emission from Pulsar Wind Nebulae with steady-state 1D Modeling Wataru Ishizaki ( Department of Physics, Graduate School of Science, The University of Tokyo ) Abstract The pulsar
More informationOn the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere
On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere for the HAWC collaboration E-mail: miguel@psu.edu Observations of high energy gamma rays are an
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 informationX-ray Hotspot Flares and Implications for Cosmic Ray Acceleration and magnetic field amplification in Supernova Remnants
X-ray Hotspot Flares and Implications for Cosmic Ray Acceleration and magnetic field amplification in Supernova Remnants Yousaf Butt, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
More informationThe Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths
More informationGAMMA-RAY ASTRONOMY: IMAGING ATMOSPHERIC CHERENKOV TECHNIQUE FABIO ZANDANEL - SESIONES CCD
GAMMA-RAY ASTRONOMY: IMAGING ATMOSPHERIC CHERENKOV TECHNIQUE COSMIC RAYS Discovered in 1912 by Victor Hess (Nobel Prize) Messengers from the non-thermal part of the Universe E < 15 ev: galactic E > 17
More informationThe Cosmological Impact of Blazars: from Plasma Instabilities to Structure Formation
The Cosmological Impact of Blazars: from Plasma Instabilities to Structure Formation 1 in collaboration with Avery E. Broderick 2, Phil Chang 2, Ewald Puchwein 1, Volker Springel 1 1 Heidelberg Institute
More informationAstronomy. Astrophysics. Radio halos in future surveys in the radio continuum
DOI: 10.1051/0004-6361/201220018 c ESO 2012 Astronomy & Astrophysics Radio halos in future surveys in the radio continuum R. Cassano 1,G.Brunetti 1, R. P. Norris 3,H.J.A.Röttgering 4, M. Johnston-Hollitt
More information