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

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% ĖL1-10TeV ~ 3.4 1033 erg s-1 ~10-2 % Ė

HESS spectrum has

~2.39

Centroid shown

PSF ~0.14

Mori et al 2004

22

'

''20 θcos2sin

EE

EE

EE

2r

dΩdσ

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

“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

INTEGRAL error circle lies within SNR

0.2-2.0 keV 4.0-8.0 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”

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 ?

Chandra Spectral Images

Helfand et al 2003

Youngest with longest period

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

Chandra-IBISMcBride et al (2007)

50”

ChandraIBIS-ISGRI

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

HESS imageINTEGRAL image

Mechanisms: X/soft -rays: synchrotron, Ee ~ 1013 -1014 eV, ~ 500y TeV: IC on (partly) CMB, Ee ~ 1012 -1013 eV, ~ 3-5000y 10 Gauss field

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 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

INTEGRALImage

Pulsar

Rosat (White)

Aharonian et al 2006

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 = 1.8x1037ergs-1, B=1.5 1013G)

Chandra shows torus and & jet with pulsar +

HESS Elliptically around pulsar (1st extended PWN jet seen in VHE)

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” J1833-1034 Somewhere 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”

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 1036 erg/s

L(20-100)

J0835-4519 (Vela) @ 0.02%

L(20-100) %Ė)

1%

20-100 keV -rays(INTEGRAL/IBIS)

INTEGRAL X-rays

Weighted mean 20-100 keVphoton spectral index: = 2.13 ± 0.15

Spectral Index vs Edot

0.1

1

10

1E+35 1E+36 1E+37 1E+38 1E+39

Edot erg/s

Ph

oto

n I

nd

ex

Spectral Index

Γ

Ė erg/s

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

High-energy spectrum of PSR J1846-0258

NOTE: As the energy increases the pulsar provides more of the output.

TeV spectral indices

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 2.8 3 More

Spectral Index

Num

ber

per

bin

Frequency

Spectral Indices

LSG/LTeV vs Age

0.1

1

10

100

1000

0.1 1 10 100

Age ky

LS

G/L

TeV

Series1

Emitted Power

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 kyL(20-100)Min ~ 0.5% Ė @ 5

L(20-100)/Edot, no resevoir

0

0.5

1

1.5

2

2.50.0

1

0.0

3

0.0

3

0.0

5

0.0

5

0.1

0.2

5

0.5 1

2.5 5 10

25

50

100

250

500

L(20-100)%Edot

Nu

mb

er

per

Bin

+gamma

Lmin(20-100)/Edot, no resevoir

0

1

2

3

4

5

6

Lmin(20-100)%Edot

Nu

mb

er p

er B

in

-gamma

Is the Ė /D2 too faint?

NO

L Sum EdotT No Gamma

0

1

2

3

4

5

6

0.01

0.02

50.

05 0.1

0.25 0.

5 12.

5 5 10 25 50 100

250

500

1000

Lmin(20-100)/L(T)

Nu

mb

er

pe

r B

in

L(SumEdot for T) Gamma PWN

00.5

11.5

22.5

33.5

L(20-100)/L(T)

Num

ber

per

Bin

Note:

a comparison with Ė is not correct

Integrate Ė over electron lifetimes

Some still should be there!

LSI +61 303, :

“OFF” (phase 0.8 – 1.3) “ON” (phase 0.3 – 0.8)

20 – 95 keV

> 400 GeV

The distant blazar Swift J1656.3-The distant blazar Swift J1656.3-33023302

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 = 2.40z = 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 = 2.40Lyα

CIVCIII]

SIV

IGR J16479-4514, the 9th SFXTOptical 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

The obscured source IGR J16318-4848

NOTE: 25% of INTEGRAL sources are still unidentified.