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Diffuse Gamma-Ray Emission Su Yang 2010.1.19. Telescopes Examples Our work.

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Presentation on theme: "Diffuse Gamma-Ray Emission Su Yang 2010.1.19. Telescopes Examples Our work."— Presentation transcript:

1 Diffuse Gamma-Ray Emission Su Yang 2010.1.19

2 Telescopes Examples Our work

3 angular resolution: 0.1d@1TeV, 0.14d@200 GeV (68% containment radius) energy range: 100 GeV to >30 TeV energy resolution: 15% at 1 TeV source location accuracy: 50’’ VERITAS (Very Energetic Radiation Imaging Telescope Array System): 4*12*345 http://veritas.sao.arizona.edu/

4 energy resolution: 15% (Index~0.1; Flux~20%) energy range: 0.1-10 TeV PSF: 0.03/0.06d FOV: 5d H.E.S.S. (High Energy Stereoscopic System): 4*13*382 http://www.mpi-hd.mpg.de/hfm/HESS/

5 CR density (M82)~500*CR density (our Galaxy): SNe & Winds from massive stars Chandra; Spitzer; Hubble; VERITAS Telescopes Help Solve 100-Year-Old Mystery ; The Origin of CRs, Nature, 2009 Web Source

6 Fermi (PSR J2229+6114) 3EG J2227+6122 CO (-6, -4 km/s) Radio SNR G106.3+2.7 (60*24’; D~0.8kpc; Boomerang) 0.4d Acciari et al. 2009, arXiv0911.4695

7 Fermi OH CO (-20,20km/s) PWN Radio Magic IC443: 1.5kpc, 45’; CXOU J061705.3+222127; (VER J0616.9+2230 ~ Magic J0616+225 ~ Milagro; 0FGL J0617.4+2234 ~ 3EG J0617+2238; ) EGRET Acciari et al. 2009, ApJ, 698:L133-L137

8 IC: L(0.3-2.0TeV)~4E32 erg/s E (rotation)~1-50E36 erg/s Synchrotron cooling: Time (E)~ 1.3E7 (B/uG) -2 (E/GeV) -1 kyr E(electron)~20TeV, B~5uG  Time~30 kyr (Abdo et al., 2010, B(Cas A)>=0.1mG) Hadronic CRs Particles were accelerated prior to the shock hitting the MC ? Or an energy-dependent rate of diffusion of CRs out of the MC ? Acciari et al. 2009, ApJ, 698:L133-L137

9 VERITAS HESS EGRET+GLAST VERITAS (Northern Sky) AGN, BIN, PWN, starburst galaxy, SNR, UNID Ong et al. 2009, arxiv0912.5355 +Web Source

10 Fermi (GLAST: Gamma-ray Large Area Space Telescope): 2008-06-11 >9000 sources 271 sources

11 Web Source

12 1-10GeV excess? Dark Matter? Variations of the Galaxy’s CR spectra? Unresolved point sources? Instrumental effects? Abdo et al. 2009, arXiv0912.0973

13 10-15% The DGE (diffuse Galactic emission): CRs (protons, electrons)  the ISM (Pi0-decay + bremsstrahlung), and radiation field (IC); Abdo et al. 2009, arXiv0912.0973

14 (Abdo et al., 2010, arXiv:1001.1419; B(Cas A)>=0.1mG)

15 Leptonic modelHadronic model (Abdo et al., 2010, arXiv:1001.1419; B(Cas A)>=0.1mG)

16 1, The Fermi Gamma-Ray Space Telescope Discovers the Pulsar in the Young Galactic Supernova Remnant CTA 1. Science, 2008, 322, 1218 2, Discovery of Pulsed gamma-Rays from the Young Radio Pulsar PSR J1028–5819 with the Fermi Large Area Telescope. ApJ, 2009, 695, L72 3, Fermi Large Area Telescope Observations of the Vela Pulsar. ApJ, 2009, 696, 1084 4, Measurement of the Cosmic Ray e++e- Spectrum from 20GeV to 1TeV with the Fermi Large Area Telescope. PRL, 2009, 102, 1101 5, Pulsed Gamma Rays from the Millisecond Pulsar J0030+0451 with the Fermi Large Area Telescope. ApJ, 2009, 699, 1171 6, Discovery of Pulsations from the Pulsar J0205+6449 in SNR 3C 58 with the Fermi Gamma-Ray Space Telescope. ApJ, 2009, 699, L102 7, Pulsed Gamma-rays from PSR J2021+3651 with the Fermi Large Area Telescope. ApJ, 2009, 700, 1059 8, Detection of 16 Gamma-Ray Pulsars Through Blind Frequency Searches Using the Fermi LAT. Science, 2009, 325, 840 9, Pulsed Gamma-rays from PSR J2021+3651 with the Fermi Large Area Telescope. ApJ, 2009, 700, 1059 10, Fermi LAT Observation of Diffuse Gamma Rays Produced Through Interactions Between Local Interstellar Matter and High-energy Cosmic Rays. ApJ, 2009, 703, 1249 Some GLAST results: Just For the Milk Way

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