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Tony Dean School of Physics and Astronomy University of Southampton

KeV to Tev The Non-Thermal Universe. Tony Dean School of Physics and Astronomy University of Southampton. INTEGRAL Studies of PWN Systems. The Source list of PWN: Selection based on the Mallory Roberts The Pulsar Wind Nebula Catalogue http://www.physics.mcgill.ca/~pulsar/pwncat.html

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Tony Dean School of Physics and Astronomy University of Southampton

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  1. KeV to Tev The Non-Thermal Universe Tony Dean School of Physics and Astronomy University of Southampton

  2. INTEGRAL Studies of PWN Systems • The Source list of PWN: • Selection based on the Mallory Roberts The Pulsar Wind Nebula Catalogue • http://www.physics.mcgill.ca/~pulsar/pwncat.html • Interest heightened by the association with a number of HESS Sources • Three types of PWN for IBIS/ISGRI: • Seen by IBIS - some discussed here ~ 10 (16%) • Pulsar seen in radio but not seen by IBIS ~ 25 (42%) • No radio pulsar ~ 25 (42%) – Possibly one seen by IBIS

  3. PWN - Where do the soft gamma-rays come from ? For the Crab, the INTEGRAL spectrum has photon index of ~2.23 i.e similar to Jet/Counterjet Spin-down energy loss, Ė = 4.6  1038 erg s-1 L(20-100) ~ 7  1036 erg s-1 ~1.5% Ė L1-10TeV ~ 3.4 1033 erg s-1 ~10-2 % Ė Mori et al 2004 HESS spectrum has ~2.39 Centroid shown PSF ~0.14

  4. Klein-Nishina cross-section for linearly polarized photons: j – azimuth angle between incident photon polarisation direction and scattered photon direction.  = azimuthal scatter angle  = elevation angle  Simulated modulation due to Compton scattering

  5. PSR J1811 -1925 : The Turtle Chandra Spectral Images • “Classic” SNR/PWN/Pulsar configuration • 4’5 diameter SNR has thermal kT ~ 0.6 keV • 65ms Pulsar has  ~ 0.97 • Bilateral elongated PWN has  ~ 1.8 • Blobs move along jet with ~ 1.4c and 0.8c • IBIS/ISGRI :  = 1.8 like Chandra PWN • L (20-100) ~ 0.66% Ė @ 5 kpc Roberts et al 2003

  6. PSR J1811 -1925 : INTEGRAL/IBIS 0.2-2.0 keV 4.0-8.0 keV • SNR spectrum is thermal, kT~ 0.6 keV • Good fit between INTEGRAL and Chandra PSR + ”jet” Where do the gamma-rays come from? • INTEGRAL error circle lies within SNR

  7. PSR J1846-0258 : Kes75 Chandra Spectral Images • Very young (~700y) system @ 19kpc • P = 324 ms • dP/dt = 7.1  10 -12 ss -1 • PWN/PSR close to centre of composite SNR • SNR, thermal, kT ~ 2.9 keV • Pulsar has  ~ 1.39 • Axisymmetric elongated PWN has  ~ 1.92 • Hot spots along axis on either side of pulsar • Exceptional timing properties : P & dP/dt > 10 Crab • Result of extreme B value of 4.8 1013 G ? Helfand et al 2003 Youngest with longest period

  8. PSR J1846-0258 : Kes75 Chandra-IBIS McBride et al (2007) • IBIS “coincident” with Pulsar/PWN complex • IBIS/ISGRI :  = 2.0 includes PWN + Pulsar • Ė = 8.4  1036 erg s-1 • L (20-100) = 1.3  1036 erg s-1 @ 19kpc • Extraordinary L (20-100) ~ 15% Ė !!! – But some concerns over 19 kpc • With D ~ 6 kpc, L (20-100) ~ 1.5% Ė • L(1-10TeV) ~ 0.1% Ė

  9. J1846-0258 a new keV to TeV emitter

  10. PSR J1617 -5055 - HESS J1616-508 INTEGRAL image HESS image • HESS extended and one sided, source size decreases with E • INTEGRAL, point like, coincident with 69ms PSR • Soft γ-ray emission Γ = 1.91 • L(20-100) = 7.4  1034 erg s-1 ~0.4% Ė • LTeV ~ 0.5% Ė • Mechanisms: • X/soft -rays: synchrotron, Ee ~ 1013 -1014 eV,  ~ 500y • TeV: IC on (partly) CMB, Ee ~ 1012 -1013 eV,  ~ 3-5000y • 10Gauss field

  11. PSR J0835-4510 - Vela Aharonian et al 2006 Pulsar Rosat (White) INTEGRAL Image • Youngish Vela Pulsar(89 ms, 290pc, Ė = 7x1036ergs-1,  ~ 11ky) • HESS extended source south of pulsar (B0833-45) • Rosat/ASCA Vela X jet like feature corresponds to aone-sided PWN • No IBIS excess from extended PWN, • No HESS excess from pulsar • L(20-100) ~ 1.6 10-2 % Ė • L(1-10TeV) ~ 0.6 10-2 % Ė

  12. PSR J1513-5906 MSH 15-52 • PSR J1509-58, (5kpc, ~1500y, 150ms, Ė = 1.8x1037ergs-1, B=1.5 1013G) • Chandra shows torus and & jet with pulsar + • HESS Elliptically around pulsar (1st extendedPWN jet seen in VHE) INTEGRAL Spectrum • IBIS/ISGRI :  = 1.89 • Fits Chandra Pulsar/PWN combo • L(20-100) ~ 2.44% Ė • L(1-10TeV) ~ 0.26% Ė

  13. Crab Inner Jet • J0540-6919 (LMC) PWN/”jet” • J0835-4519 (Vela) PWN/”jet” • J1302-6350 (Be) ? Be accretor • J1513-5906 (MSH 15-52) PWN/”jet” • J1617-5055 near pulsar (X-PWN? – No jet) • J1811-1925 (Turtle) PWN/”jet” • J1833-1034 Somewhere in outer PWN – No jet • J1846-0258 (Kes 75) PWN/”jet” Where do the soft gamma-rays come from ? • Positional location : Tantalisingly close to pulsar, within PWN? • IBIS Site must be close to electron accelerator • Synchrotron lifetime of soft -ray producing electrons in PWN fields is  ~ 10 - 100y • NOTE that  67% of the soft -emitting systems have “jets”

  14. Correlations with the pulsar characteristics - 20-100 keV Luminosity INTEGRAL NOTE: They are all young, short period (~ 100ms), energetic pulsars, spin down ages in range 700  τ 20,000 y L(20-100) 20-100 keV -rays (INTEGRAL/IBIS) 1% Ė 1036 erg/s L(20-100) %Ė) X-rays (Possenti et al 2002) J0835-4519 (Vela) @ 0.02%

  15. Γ Ė erg/s Correlations with the pulsar characteristics INTEGRAL X-rays Weighted mean 20-100 keV photon spectral index:  = 2.13 ± 0.15

  16. Some general characteristics of INTEGRAL PWN • A young energetic pulsar is needed • L(20-100) ~ 1% Ė, & L(20-100keV) L(1-10TeV) • A jet-like feature is generally present • The soft gamma-ray photon index is  ~ 2 • INTEGRAL source is “coincident” with the pulsar/PWN & INTEGRAL X-rayPWN • When accompanied by a TeV source, Synchrotron for soft gammas and Inverse Compton for TeV works well. • NOTE the energies of the soft gamma producing electrons is ~ 10× TeV producing electrons

  17. High-energy spectrum of PSR J1846-0258 NOTE: As the energy increases the pulsar provides more of the output.

  18. Emitted Power How do the Soft gammas and TeV Emissions Compare? Spectral Indices

  19. Why are some not there? e.g. G292.0+1.8 – PSR J1124-5916 • Age ~ 1600 y • Distance ~ 5.4 kpc • Ė ~1.2 1037 erg/s • P = 135 ms, • dP/dt = 7.47 10-13 s/s •  ~3 ky • L(20-100)Min ~ 0.5% Ė @ 5

  20. Those that are not there Is the Ė /D2too faint? NO

  21. Those that are not there Note: a comparison with Ė is not correct  Integrate Ė over electron lifetimes Some still should be there!

  22. Microquasars LSI +61 303, : “OFF” (phase 0.8 – 1.3) “ON” (phase 0.3 – 0.8) 20 – 95 keV > 400 GeV

  23. The distant blazar Swift J1656.3-3302 Data analysis of spectroscopy collected with the ESO-3.6m telescope plus EFOSC2 on June 2007 allowed us to identify the hard X-ray source Swift J1656.3-3302 as a powerful gamma-ray loud blazar atz = 2.40. This is, up to now, the farthest optically-identified object of any INTEGRAL survey, and the fourth farthest of all objects detected with INTEGRAL. Masetti et al. (in prep.) Lyα Z = 2.40 CIV CIII] SIV SWIFT J1656.3-3302

  24. IGR J16479-4514, the 9th SFXT Optical counterpart recently identified as supergiant(Chaty 2007,astroph 0710.0292) SFXT with the highest duty cycle(Sguera et al. 2007 to be submitted) ISGRI light curve (18-60 keV) from Feb 2003 to Apr 2006 bin time 2000 s

  25. The obscured source IGR J16318-4848 NOTE: 25% of INTEGRAL sources are still unidentified.

  26. Hello, Non-Thermal Universe keV to TeV

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