2. 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 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

3. 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  10 38 erg s -1 L (20-100) ~ 7  10 36 erg s -1 ~1.5% Ė L 1-10TeV ~ 3.4  10 33 erg s -1 ~10 -2 % Ė HESS spectrum has  ~2.39 Centroid shown PSF ~0.14  Mori et al 2004

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

5.  “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 Chandra Spectral Images  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.  INTEGRAL error circle lies within SNR 0.2-2.0 keV4.0-8.0 keV INTEGRAL/IBIS Where do the gamma-rays come from?  SNR spectrum is thermal, kT~ 0.6 keV  Good fit between INTEGRAL and Chandra PSR + ”jet”

7.  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 10 13 G ? Chandra Spectral Images Helfand et al 2003 Youngest with longest period

8.  IBIS “coincident” with Pulsar/PWN complex  IBIS/ISGRI :  = 2.0  includes PWN + Pulsar  Ė = 8.4  10 36 erg s -1  L (20-100) = 1.3  10 36 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 Chandra-IBIS McBride et al (2007)

10.  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  10 34 erg s-1 ~0.4% Ė  L TeV ~ 0.5% Ė HESS image INTEGRAL image Mechanisms:  X/soft  -rays: synchrotron, E e ~ 10 13 -10 14 eV,  ~ 500y  TeV: IC on (partly) CMB, E e ~ 10 12 -10 13 eV,  ~ 3-5000y  10  Gauss field

11.  Youngish Vela Pulsar (89 ms, 290pc, Ė = 7x10 36 ergs -1,  ~ 11ky)  HESS extended source south of pulsar (B0833-45)  Rosat/ASCA Vela X jet like feature corresponds to a one-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 INTEGRAL Image Pulsar Rosat (White ) Aharonian et al 2006

12.  IBIS/ISGRI :  = 1.89  Fits Chandra Pulsar/PWN combo  L (20-100) ~ 2.44% Ė  L (1-10TeV) ~ 0.26% Ė INTEGRAL Spectrum  PSR J1509-58, (5kpc, ~1500y, 150ms, Ė = 1.8x10 37 ergs -1, B=1.5 10 13 G)  Chandra shows torus and & jet with pulsar +  HESS Elliptically around pulsar (1st extended PWN jet seen in VHE)

13.  Positional location : Tantalisingly close to pulsar, within PWN?  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”  J1833-1034Somewhere in outer PWN – No jet  J1846-0258 (Kes 75)PWN/”jet”  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. INTEGRAL NOTE: They are all young, short period (~ 100ms), energetic pulsars, spin down ages in range 700  τ  20,000 y X-rays (Possenti et al 2002) Ė  10 36 erg/s L(20-100) J0835-4519 (Vela) @ 0.02% L (20-100) %Ė) 1% 20-100 keV  -rays (INTEGRAL/IBIS)

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

16.  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. Spectral Indices Emitted Power

19. e.g. G292.0+1.8 – PSR J1124-5916  Age ~ 1600 y  Distance ~ 5.4 kpc  Ė ~1.2 10 37 erg/s  P = 135 ms,  dP/dt = 7.47 10 -13 s/s   ~3 ky  L (20-100)Min ~ 0.5% Ė @ 5 

20. Is the Ė /D 2 too faint? NO

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

22. 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 z = 2.40 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 at z = 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.) SWIFT J1656.3-3302 Z = 2.40 Ly α CIV CIII] SIV

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.