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「すざく」による SN1006 の観測 Suzaku observations of SN1006

「すざく」による SN1006 の観測 Suzaku observations of SN1006. Aya BAMBA (ISAS/JAXA). Suzaku : Jp -US X-ray satellite. Successfully launched on 2005 July 10 th . XIS (X-ray Imaging Spectrometer) Improved X-ray CCD with high efficiency and good energy response Low and stable background

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「すざく」による SN1006 の観測 Suzaku observations of SN1006

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  1. 「すざく」によるSN1006の観測 Suzaku observations of SN1006 Aya BAMBA (ISAS/JAXA)

  2. Suzaku: Jp-US X-ray satellite Successfully launched on 2005 July 10th. XIS (X-ray Imaging Spectrometer) Improved X-ray CCD with high efficiency and good energy response Low and stable background Energy band : 0.2-12keV XRT (X-Ray Telescope) Large effective area 410cm2 @1.5keV HXD (Hard X-ray Detector) Wide energy band Si-PIN (10-70keV) & GSO Scinti. (40-600keV) Non-imaging detector, but low background XIS XRT HXD

  3. Previous SN1006 observations radio: faint continuum no information of MC X-ray: synchrotron X-rays ! (~10/265 SNRs) thermal X-rays Halpha: bright in NW rim proper motion is measured TeV: detected faint shells optical: detection of SN 1000yrs ago type Ia SN @NASA/HEASARC SN1006 is a milestone to understand the shock accelerationin SNRs

  4. What can Suzaku achieve ? - X-ray diagnostics of thermal emission density, temperature, …. -> topic 1 - parameters of synchrotron X-rays bending ?? -> topic 2

  5. Suzaku observations mapping of whole remnant FOV of XIS FOV of HXD/PIN src4pointing bg 2pointing total200ks

  6. Narrow band images of XIS-BI He-like Oline band 3 - 5 keV band Distributions of thermal plasma and non-thermal electron are different !

  7. Topic 1: X-ray diagnostics of thermal emission

  8. XIS thermal emission in SE region Plenty of emission lines strong H-like and He-like O lines the first detection of iron K line (Yamaguchi+08)

  9. thermal spectrum of whole SNR NH [cm-2] 6.8x1020 VNEI 1 (ejecta 1) kT [keV] 1.2 nOneV [cm-3] 4.19 (4.05-4.32)x1052 VNEI 2 (ejecta 2) kT [keV] 1.9 nOneV [cm-3] 3.82 (3.77-3.89)x1053 NEI (ISM) kT [keV] 0.45 nHneV [cm-3] 3.45 (3.43-3.48)x1056 ISM density: 0.03 cm-3 (SE of SNR) The density of acceleration site is very low ! (Yamaguchi+08) (Bamba+08)

  10. Proper motion of SN1006 NE shell filaments are moving in these 9 yrs ! v = 0.48”/yr ~ 5000 km/s ambient density ~ 0.085 cm-3 2000 - 2008 ISM density is very low ! (Katsuda+09)

  11. topic 2: Parameters of synchrotron X-rays

  12. Spectra of whole remnant: XIS+HXD PIN statistic err PIN systematic err excess: 1% of bgd The most tight upper-limit (2.7x10-5 ph/cm2/s in 10-15 keV)

  13. XIS spectra (1) emission lines + hard emission 3 kT plasma (Yamaguchi+08) + power-law model large residuals from power-law model XIS FI XIS BI

  14. synchrotron model with bending: srcut model cut-off ? -> Emax of e, B G electron distribution Sync. Emission From Power-lawelectrons N(E) exp. G-1 2 E (SRCUT model) Emax emission Sync. emission emission from an e n ncutoff ~ Emax2B n E2B We need spectra with good statistics -> Let’s see SN1006

  15. XIS spectra (2) sync. emission from electrons with PL + exp. cutoffdistribution spectral index at 1GHz: a=0.57 3 kT plasma + srcut model no residual ! XIS FI XIS BI non-thermal emission has significant cut-off ! ncutoff = 5.69 (5.67-5.71)x1016 Hz

  16. XIS spectrum of each rim NE rim SW rim cutloff freq. 6.66(6.58-6.69)x1016 Hz 4.68(4.64-4.73)x1016Hz cut-off freq. is larger in the NE rim

  17. What determine cutoff energy? 2 E 10TeV B 1microG cutoff freq. = 1.6x1016 [Hz] B: magnetic fieldE: max E of e (Reynolds 1998) assumption: B=40microG(10microG outside) (Bamba+ 2003) -> E = 9.4 TeV difference of cut-off in NEand SW rims difference of B and/or Emax ? -> difference of acc. efficiency ? E = 10 TeV @ NE E = 8.5 TeV @SW assump. B=40microG more detailed model is now needed to understand the cut-off Now we have TeV emission ! SED is available.

  18. nonthermal flux vs. thermal flux (Bamba+07, regected by J.Hughes) east inner thermal flux (ergs s-1cm-2arcmin-2 (0.5-2 keV)) north non-thermal flux (10-12ergs s-1cm-2arcmin-2 (2-10 keV)) even low density, it might affect CR acceleration

  19. Where is accelerated protons ? In the case of old SNR G359.1-0.5 … TeV gamma-rays! SNRs G359.0-0.9, G359.1-0.5 (Bamba+ 2000) Only thermal 6arcmin 0.5-2.0 keV (Suzaku) contour: HESS (Bamba+09)

  20. neutral iron map excess ! 6arcmin molecular cloud TeV emission is from accelerated protons ? past active GC (Bamba+09)

  21. Summary • SN1006 is a milestone to understand • CR acceleration on shocks of SNRs. • Suzaku capability to resolve thermal emission shows us that the ISM density around • SN1006 is very low. • Chandra detected proper motion of the NE rim. • We detected the bending of synchrotron emission. • Now we have TeV emission, we will be able to determine the Emax. • Older SNRs should be studied more • for proton acceleration study.

  22. 3rdSuzaku conference “the Energetic Cosmos: from Suzaku to Astro-H” June 29 – July 2, Otaru, Hokkaido, Japan Topics: - Particle acceleration in cosmic shocks and jets - X-ray diagnostics of cosmic hot plasma - High energy aspects of the Milky Way - Magnetic activity in stellar objects - Primary and reprocessed emission from accreting objects - X-ray vies of the evolution of the universe - Highlights from the Fermi Space Gamma-Ray Telescope - Status of the MAXI experiment - From Suzaku to ASTRO-H and other missions and further to IXO abstract deadline: Mar. 16 registration deadline: Apr. 13 Let us enjoy fresh topics and Sushi !

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