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On the number of SNRs detectable in the TeV energy domain

MNRAS, 434, 2748-2760 (2013). On the number of SNRs detectable in the TeV energy domain. Cristofari et al 2013. (2014-07-01, reported by Zhang Xiao). Purpose: putting attention to the TeV energy domain, using the simulation to predict the number of Galactic SNRs with a given gamma-ray flux.

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On the number of SNRs detectable in the TeV energy domain

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  1. MNRAS, 434, 2748-2760 (2013) On the number of SNRs detectable in the TeV energy domain Cristofari et al 2013 (2014-07-01, reported by Zhang Xiao)

  2. Purpose: putting attention to the TeV energy domain, using the simulation to predict the number of Galactic SNRs with a given gamma-ray flux. Before simulation, something need to kown Dynamical evolution of SNRs (skip) CR acceleration at SNR shocks (skip) SNRs distribution in the Milky Way

  3. SNRs distribution in the Milky Way step 1. use MC to simulate the time of explosion step 2. according to the precription decribed in Faucher-Gigure & Kaspi (2006), determine the location (Faucher-Giguere & Kaspi 2006, ApJ, 643, 332)

  4. individual SNRs evolution and gamma-ray emission • 1. the ambient density • 2. SN type 3D distribution of HI and H2 given by Nakanishi & Sofue (2003, 2006)

  5. : the number ratio of e to p at relativistic energy regime : the index of particle momentum spectrum • Some parameters The flux sensitivity for deep observation with current CTA

  6. One zone without MFA red: ~13 black: ~21

  7. One zone without MFA One zone with MFA red: ~13 black: ~21 red: ~32 black: ~39 Two zone with MFA red: ~190 black: ~57

  8. comparison with observations Observation: HESS survey 35 TeV sources individual SNRs (3): RX J1713.7-3946, HESS J1731-347 and CTB 37B unidentified source (17) interacting SNRs (3): CTB 37A, HESS J1745-303, W28 other indetified source (12): AGNs, PWNe, ... The possible detected individual SNRs: 3 - 20

  9. red: ~7 black: ~5 red: ~22 black: ~17 number increase two-zone model with MFA 1. Steep spectra are consistent with observations. 2. Kep significantly larger than 0.01 is in conflict with observations.

  10. Discussion 1. the effect for different parameters: 2. SNR distribution 3. the effect of MCs Conclusions 1. Steep spectra are consistent with observations. 2. Kep significantly larger than 0.01 is in conflict with observations.

  11. escape GeV energy band interacting with MCs ...

  12. Thank You!

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