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Morphological and spectral studies of the shell-type supernova remnants

Morphological and spectral studies of the shell-type supernova remnants RX J1713.7-3946 & RX J0852.0-4622 by H.E.S.S. M. Lemoine-Goumard, F. Aharonian, D. Berge, B. Degrange, D. Hauser, N. Komin, O. Reimer, U. Schwanke for the H.E.S.S. Collaboration.

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Morphological and spectral studies of the shell-type supernova remnants

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  1. Morphological and spectral studies of the shell-type supernova remnants RX J1713.7-3946 & RX J0852.0-4622 by H.E.S.S. M. Lemoine-Goumard, F. Aharonian, D. Berge, B. Degrange, D. Hauser, N. Komin, O. Reimer, U. Schwanke for the H.E.S.S. Collaboration

  2. RX J1713.7-3946Multi-Wavelength Observations RA RA Fukui et al. (2003) Discovery: ROSAT All-Sky Survey (1996) X-ray emission mostly non-thermal Distance reestimated at 1kpc (Cassam-Chenai et al. and Fukui et al., 2004) CANGAROO observed TeV excess from western rim (Enomoto et al., 2000) Detection by H.E.S.S. in 2004 (Aharonian et al., 2004) ROSAT (0.1-2 keV) XMM-Newton (2-10 keV) XMM + NANTEN David Berge, HDGS July 2004

  3. H.E.S.S. Observations in 2004 Angular resolution < 0.1° → morphology resolved Observations with the full array of 4 telescopes 33 hours livetime ON source Zenith angles from 15 to 60 degrees Standard cuts are applied Shell of the remnant resolved

  4. RX J1713.7-3946 Spectrum Extension of the spectrum up to 40 TeV → Particles accelerated up to ~100 TeV Spectrum obtained with the 2004 dataset compatible with the one from 2003 Photon index of the remnant : -2.26 ± 0.02 ± 0.15 Flux ~ 1 Crab Deviation from a pure power-law at high energy

  5. XMM-Newton Cassam-Chenai et al. Spatially resolved spectra No significant change of the spectral shape from one region to another in TeV Significant changes of the spectral index observed in X-rays H.E.S.S.

  6. Energy dependence of the Morphology As opposed to X-rays, TeV morphology doesn’t change significantly with energy 1.4 TeV < E E < 0.6 TeV 0.6 < E < 1.4 TeV David Berge, DPG Tagung, März 2005

  7. Correlation with X-rays Correlation coefficient between ASCA & HESS ~ 80%

  8. Primary population: electrons ? B = 6 µG B = 6 µG B = 8 µG B = 8 µG B = 10 µG B = 10 µG • Need about 8 µG B field to match flux ratios • Simplest electronic models don’t work well Simple one-zone model Electrons & protons injected with the same spectral shape Energy losses + escape of particles out of the shell taken into account Power-law index = 2.4 at injection level Power-law index = 2.2 at injection level

  9. Primary population: protons ? Spectral shape at the injection level: power-law + exponentional cut-off Ecut = 120 TeV et index = 2.0 Energy injected = 1050 ergs Electron/proton ratio = 5× 10-4 Magnetic field = 35 µG & Density = 1.5 cm-3

  10. RX J0852.0-4622Multi-Wavelength Observations Discovery: ROSAT All-Sky Survey (1998) X-ray emission mostly non-thermal Distance still uncertain 200 pc - 1kpc Detected with H.E.S.S. in 2004 ASCA + CANGAROO contours ROSAT all Sky Survey

  11. H.E.S.S. Observations in 2004 Angular resolution < 0.1° → morphology resolved Observations from December 2004 to May 2005 20 hours livetime ON source Zenith angles between 20° and 50° Energy threshold : 250 GeV Results confirmed by an independent analysis

  12. RX J0852.0-4622 Spectrum Extension of the spectrum up to 20 TeV → Particles accelerated up to ~100 TeV Spectrum ranges from: 300 GeV up to 20 TeV Spectral index: 2.24 ± 0.05stat ± 0.15 syst I (> 1TeV) = (15.2±0.7stat±3.20syst)×10-12 cm-2s-1 Flux and spectral index compatible with the results published in A&A Indication of deviation at high energy

  13. ASCA 2 1 3 6 4 5 HESS ROSAT ASCA Correlation with X-rays Correlation coefficient between X-rays and HESS ~ 70%

  14. Primary population: electrons ? Leptonic process => Magnetic field ~ 7 µG Nearby case (D ~ 200 pc) Distant case (D ~ 1 kpc) => Difficulty to confine electrons in the very thin shell resolved by HESS

  15. Primary population: protons ? Hadronic process => Magnetic field > 40 µG to fit the X-ray data and suppress the IC-scattering component Nearby case (D ~ 200 pc) Distant case (D ~ 1 kpc) Density ~ 2.2 cm-3 => Bubble mechanism needed to explain the absence of thermal X-rays (n < 0.1 cm-3Slane et al.) => Electron/proton ratio ~ 4 × 10-6

  16. Morphological comparison between the 2 sources Morphology completely different Much thicker shell for RX J1713.7-3946 Widthshell ~ 55% Rremnant Widthshell < 22.5% Rremnant RX J1713.7-3946 RX J0852.0-4622

  17. Spectral comparison between the 2 sources Almost the same flux Almost the same spectral index Indication of curvature at high energy

  18. Conclusions 2 shell-type supernova remnants established as γ-ray emitter and resolved for the first time in TeV X-ray morphology very similar to the γ-ray morphology observed with HESS First time ever spatially resolved spectral study of a gamma-ray source (RX J1713.7-3946) Flux ~ 1 Crab & Photon index ~ 2.2 Question of electron or hadron accelerator remains difficult to answer (=> solution should be given by HESS II & GLAST)

  19. Column density in RX J0852.0-4622 fov D ~ 1 kpc D ~ 500 pc D ~ 1.5 kpc D ~ 2 kpc

  20. Correlation between CO and γ-rays in RX J0852.0-4622 fov

  21. Thickness of the whidth of RX J1713.7-3946 & RX J0852.0-4622 RX J1713.7-3946 width < 22.5 % RX J1713.7-3946 width ~ 55%

  22. Correlation between CO and γ-rays in RX J1713.7-3946 fov Azimuthal profile

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