Tony Dean

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

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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, E 4.6 ?
1038 erg s-1 L(20-100) 7 ? 1036 erg s-1 1.5
E L1-10TeV 3.4 ? 1033 erg s-1 10-2 E
Mori et al 2004
HESS spectrum has ?2.39 Centroid shown PSF
0.14?
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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
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PSR J1811 -1925 The Turtle
Chandra Spectral Images

• Classic SNR/PWN/Pulsar configuration
• 45 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 E _at_ 5 kpc

Roberts et al 2003
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PSR J1811 -1925
Where do the gamma-rays come from?

• INTEGRAL error circle lies within SNR

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PSR J1846-0258 Kes75
Chandra Spectral Images

• Very young (700y) system _at_ 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 gt 10
  Crab
• Result of extreme B value of 4.8 1013 G ?

Helfand et al 2003
Youngest with longest period
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PSR J1846-0258 Kes75
Chandra-IBIS McBride et al (2007)

• IBIS coincident with Pulsar/PWN complex
• IBIS/ISGRI ? 2.0 ? includes PWN Pulsar
• E 8.4 ? 1036 erg s-1
• L (20-100) 1.3 ? 1036 erg s-1 _at_ 19kpc
• Extraordinary L (20-100) 15 E !!! But some
  concerns over 19 kpc
• With D 6 kpc, L (20-100) 1.5 E
• L(1-10TeV) 0.1 E

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J1846-0258 a new keV to TeV emitter
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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 ?-ray emission G 1.91
• L(20-100) 7.4 ? 1034 erg s-1 0.4 E
• LTeV 0.5 E

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

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PSR J0835-4510 - Vela
Aharonian et al 2006
Pulsar
Rosat (White)
INTEGRAL Image

• Youngish Vela Pulsar (89 ms, 290pc, E
  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 E
• L(1-10TeV) 0.6 10-2 E

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PSR J1513-5906 MSH 15-52
INTEGRAL Spectrum

• PSR J1509-58, (5kpc, 1500y, 150ms, E
  1.8x1037ergs-1, B1.5 1013G)
• Chandra shows torus and jet with pulsar
• HESS Elliptically around pulsar (1st extended
  PWN jet seen in VHE)

• IBIS/ISGRI ? 1.89
• Fits Chandra Pulsar/PWN combo
• L(20-100) 2.44 E
• L(1-10TeV) 0.26 E

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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

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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 ? t ? 20,000 y
L(20-100)
20-100 keV ?-rays (INTEGRAL/IBIS)
1
E ?1036 erg/s
L(20-100) E)
X-rays (Possenti et al 2002)
J0835-4519 (Vela) _at_ 0.02
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Correlations with the pulsar characteristics
INTEGRAL
X-rays
Weighted mean 20-100 keV photon spectral index
? 2.13 0.15
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Some general characteristics of INTEGRAL PWN

• A young energetic pulsar is needed
• L(20-100) 1 E, 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

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High-energy spectrum of PSR J1846-0258
NOTE As the energy increases the pulsar provides
more of the output.
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How do the Soft gammas and TeV Emissions Compare?
Spectral Indices
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Why are some not there?
e.g. G292.01.8 PSR J1124-5916

• Age 1600 y
• Distance 5.4 kpc
• E 1.2 1037 erg/s
• P 135 ms,
• dP/dt 7.47 10-13 s/s
• ? 3 ky
• L(20-100)Min 0.5 E _at_ 5?

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Those that are not there
Is the E /D2 too faint?
NO
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Those that are not there
Note a comparison with E is not correct ?
Integrate E over electron lifetimes
Some still should be there!
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LSI 61 303, OFF (phase 0.8 1.3)
ON (phase 0.3 0.8)
Microquasars
20 95 keV
gt 400 GeV
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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 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.)
Z 2.40
Lya
CIV
CIII
SIV
SWIFT J1656.3-3302
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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
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The obscured source IGR J16318-4848
NOTE 25 of INTEGRAL sources are still
unidentified.
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Hello, Non-Thermal Universe keV to TeV