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A large XMM-Newton project on SN 1006

A large XMM-Newton project on SN 1006. Gilles Maurin (Sap – IRFU/CEA-Saclay) A. Decouchelle, G. Dubner, M. Miceli and the LP team. Why study SN 1006 ?. ATCA – 1.3 GHz. SN 1006 is a historical SNR: distance (2.2 kpc) and age are well-known The interstellar absorption towards it is low

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A large XMM-Newton project on SN 1006

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  1. A large XMM-Newton project on SN 1006 Gilles Maurin (Sap – IRFU/CEA-Saclay) A. Decouchelle, G. Dubner, M. Miceli and the LP team

  2. Why study SN 1006 ? ATCA – 1.3 GHz • SN 1006 is a historical SNR: distance (2.2 kpc) and age are well-known • The interstellar absorption towards it is low • Uniform ambient medium around the source: its morphology is relatively symmetrical • Synchrotron observed from radio to X-rays • + recently observed by H.E.S.S. in TeV γ-rays XMM – 2-4 keV H.E.S.S. - γ-rays • For all these reasons, SN1006 is a good target to study • particle acceleration

  3. The objectives of the large XMM-Newton project • Where are the ejecta and what are they made of ? • Where is the shocked interstellar medium ? • How efficient is the proton acceleration ? • How is the shock energy shared between the different species at shock ? • What is the intensity and post-shock evolution of the downstream magnetic field ? • What are the maximum energies of accelerated electrons and ions ? • What is the geometry of the ambient magnetic field ? • We asked for a deep 1 Ms XMM-Newton observation of the entire SN 1006 supernova remnant • We obtained 500 ks Outline of this présentation: Data; Analysis; Preliminary result: study of the thermal and non- thermal emission around the shock

  4. Status before the large project 7 observations between 2000 and 2005 = 106 ks

  5. The large project 6 new observations (2008-2009) = 549 ks Statistics are increased by a factor 5 in observed regions  Will allow us to study the spectra of the non-thermal filaments around the shock

  6. Standard method for background spectrum estimation Blank sky for PN instrument Blank skies are used to estimate: - astrophysical backgrounds (local and extra-galactic photons background) - particle background (CR and protons from solar) (linked to the solar activity) The rate of the particle background has strongly increased since 2005 (revolution 700). PN Counts per second MOS We have to take into account this effect, in particular for the new observations (2008-2009). Revolution 2005 2009

  7. Our method for background estimation Closed observations for PN instrument • Observations in closed mode are used to estimate the particle background • Double-substraction method are used to take into account the astrophysical background Before stacking observations in closed-mode (to have high statistics), we checked that the spectrum of particle background didn’t change significantly with time. Emission line 1.4 - 1.6 keV Continuum 2 – 3 keV Revolution = 500 Revolution = 1200 MOS count rate (s-1) PN PN MOS Total count rate (s-1)

  8. New images* of SN 1006 with MOS instruments *Background used = Closed observations Regions used for astrophisical background estimation 2 - 4 keV (dominated by non-thermal emission) 0.5 - 0.8 keV (oxygen band)  Spectrum extraction in 30 regions around the shock (like Miceli et al. 2009)

  9. Two samples of region Zone 29 In the SE region Zone 23 In the NE region PN PN MOS 1&2 MOS 1&2 Emission dominated by thermal emission Emission dominated by synchrotron emission 10 spectra for MOS 5 spectra for PN 10 spectra for MOS 4 spectra for PN

  10. Azimuthal behaviour Miceli et al. Our results Norm Models used: VPSHOCK + SRCUT VPSHOCK Thermal model The SRCUT normalization at 1 Ghz has been fixed by extracting the radio flux from the same region in the X-ray map: VLA observations (Petruk et al 2008) kt (keV) Comparison between the results from Miceli. et al. and our method with the same observations:  possible because the particle background is almost constant in these observations. α SRCUT Non Thermal model Very good agreement between the two results: - confirms the results of Miceli et al. - allows us to add new observations Log(νbreak)  High statistic allows us to reduce the size of the boxes

  11. Azimuthal behaviour in the NE region We divided each box in the NE region by 10. VPSHOCK Thermal model kt (keV) α SRCUT Non Thermal model Evidence of small scale azimuthal variations of the non-thermal emission Log(νbreak) Now we have to follow precisely the spectral variations along the filamentary structures

  12. Conclusion and outlook • We took into account properly the increase of particle background by using closed observations instead of blank sky. • We studied the azimuthal variations of the physical properties around the shock. • ⇒ Our results are compatible with the previous ones • In the NE region, we revealed variations at small scale of the non-thermal emission • The statistic of the large project will allow us to study the acceleration parameters at the size of non-thermal filaments NE - region ∼20’’ Statistics + angular resolution of XMM-Newton (∼8’’) ⇒ sufficient separation of the filaments Coming soon

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