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The hard X-ray spectrum of Pulsar Wind Nebulae

Data-models comparison in the Simbol-X era F. Bocchino, INAF Osservatorio Astronomico di Palermo with contributions of R. Bandiera (INAF-OAA), L. Del Zanna (UNIFI), D. Volpi (UNIFI), G. Cusumano (INAF-IASF Pa). The hard X-ray spectrum of Pulsar Wind Nebulae. Introduction. What is a PWN.

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The hard X-ray spectrum of Pulsar Wind Nebulae

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  1. Data-models comparison in the Simbol-X era F. Bocchino, INAF Osservatorio Astronomico di Palermo with contributions of R. Bandiera (INAF-OAA), L. Del Zanna (UNIFI), D. Volpi (UNIFI), G. Cusumano (INAF-IASF Pa) The hard X-ray spectrum of Pulsar Wind Nebulae

  2. Introduction What is a PWN...

  3. Introduction The mechanism which bring particles and fields to the outer edge of the nebulae is still under investigation “It's like finding the transmission lines between the power plant and the light bulb.” (J. Hester, Arizona Univ.)

  4. Examples of PWNe The Crab Nebula • SN1054 • LX=2.4 1037 erg/s • Distance 2 kpc • Calib. source 1’

  5. Examples of PWNe The Vela PWN • Age 11 kyr • LX=6 1033 erg s • D = 0.2 kpc 1’

  6. Symbol-X and PWNe • Doing Chandra-like imaging is hopeless • Low bkg will make Symbol-X extremely competitive w.r.t. current non-imaging hard X-ray instruments • Easy detection of PWNe above 10 keV in reasonable single-pointing exposure time • Recent advances in theoretical modeling of PWNe have pointed out the importance of the study of the shape of PWN integrated X-ray spectrum

  7. Spectra of PWNe • Zero order approximation • Synchrotron aging of a constantly injected power-law population (Ginzburg & Syrovatskii 1965)

  8. Spectra of PWNe • Modern approaches based on inhomogeneous models • MHD simulations, calculations of synchrotron emissivities (Del Zanna et al. 2006)

  9. Spectra of PWNe • Alternative views • Diffusive synchrotron radiation from PWNe (Fleishman & Bietenholtz 2007) Aimed to overcome difficulties of “classical” approaches to “non-Crab like” PWNe

  10. X-ray spectra of PWNe • XMM-Newton 30 ks • INTEGRAL/IBIS, 439 SCWs in 2003-2004, 1 Ms • fX = 0.4 mCrab • Single power-law • NH=2.5+/-0.1 1022 cm-2 • g = 1.74 +/- 0.06

  11. Data sensitivity to spectral breaks in hard X-ray

  12. Data sensitivity to spectral breaks in hard X-ray • VELA: Mangano et al (2006), BeppoSAX MECS+PDS • CRAB1: de Jager et al. (1996), balloon-borne experiments • CRAB2: Massaro et al. (2000) BeppoSAX NFI+HP+PDS

  13. Data sensitivity to spectral breaks in hard X-ray Black: XMM 30 ks + ISGRI 1 Ms • VELA: Mangano et al (2006), BeppoSAX MECS+PDS • CRAB1: de Jager et al. (1996), balloon-borne experiments • CRAB2: Massaro et al. (2000) BeppoSAX NFI+HP+PDS

  14. Data sensitivity to spectral breaks in hard X-ray Black: XMM 30 ks + ISGRI 1 Ms RED: Suzaku 300 ks std. bkg • VELA: Mangano et al (2006), BeppoSAX MECS+PDS • CRAB1: de Jager et al. (1996), balloon-borne experiments • CRAB2: Massaro et al. (2000) BeppoSAX NFI+HP+PDS

  15. Data sensitivity to spectral breaks in hard X-ray Black: XMM 30 ks + ISGRI 1 Ms RED: Suzaku 300 ks std. Bkg Green: Simbol-X 100 ks • VELA: Mangano et al (2006), BeppoSAX MECS+PDS • CRAB1: de Jager et al. (1996), balloon-borne experiments • CRAB2: Massaro et al. (2000) BeppoSAX NFI+HP+PDS

  16. Data-model comparison in the Simbol-X era • Simulated synchrotron emission from PWNe (Del Zanna et al. 2006) pole equator pole run A: s=0.025, nearly ideal case for Crab run B: s=0.1 large equatorial unmagnetized region

  17. Data-model comparison in the Simbol-X era: the Crab Only the nebular emission is considered VELA: Mangano et al 06 (obs) CRAB1: de Jager et al. 1996 (obs) CRAB2: Massaro et al 2000 (obs) LDZ06: Del Zanna et al 2006 (models)

  18. Data-model comparison in the Simbol-X era: the Crab • Only the nebular emission is considered • VELA: Mangano et al 06 (obs) • CRAB1: de Jager et al. 1996 (obs) • CRAB2: Massaro et al 2000 (obs) • LDZ06: Del Zanna et al 2006 (model) Black: Simbol-X 100 ks simulated spectrum

  19. Data-model comparison in the Simbol-X era: 3C 58 • Prototype of “non-Crab like” PWNe • Diffusive synchrotron radiation from PWNe (Fleishmann & Bietenholtz 2007) seems to overcome the difficulty of low frequency and large change of slope of the break in the radio band • What about in the X-ray band?

  20. Data-model comparison in the Simbol-X era: 3C 58 DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum

  21. Data-model comparison in the Simbol-X era: 3C 58 DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum Black solid: XMM 30 ks

  22. Data-model comparison in the Simbol-X era: 3C 58 DSR 3c58: Diffusive synchrotron radiation model of Fleishmann & Bietenholz (2007) tailored to 3c58 broad band spectrum Black solid: XMM 30 ks Red solid: Simbol-X 100 ks

  23. Conclusions The shape of the hard X-ray spectrum of Pulsar Wind Nebulae is directly related to the distribution of B and e- in the source Current measurements are just enough to provide some diagnostics for the brightest objects (Crab and Vela) Simbol-X may provide an order of magnitude improvement in the comparison between model and observations for these bright sources Other bright PWNe (G21.5-0.9, 3C58) are hardly detected by non-imaging hard X-ray instruments. Simbol-X will provide THE unique opportunity to study the spectrum above 5-10 keV.

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