1. The INTEGRAL Galactic Sky
Synergy with AGILE
P. Ubertini,
A. Bazzano, A. Tarana on behalf of the IBIS Survey Team 1

2. OUTLINE IBIS and its capabilty
The IBIS view of the Galactic Gamma–ray Sky
The IBIS AGILE Galactic source OK 2

3. INTEGRAL overview IBIS and SPI are main instruments
IBIS optimised for imaging (17keV-10MeV)
SPI optimised for spectra
(20keV-8MeV)
IBIS is the primary survey instrument
Wide FOV (30x30 degrees)
ISGRI detector mainly operates keV
Sensitivity <0.5mCrab for deep exposures
JEM-X and
Credit: ESA
IBIS
SPI
Coded aperture mask - multiplex advantage - monitoring of many sources while simultaneously searching for other new ones.

4. IBIS: hunting new γ-ray sources
Takes advantage of the large FOV (~1000sq deg) for source detection
Unbiased search of the IBIS datasets: 6+ years of operations
Looking for weak persistent sources only visible on long timescales: spans a duration of > 1600 days100Ms (with no basic systematic errors! i.e. 4.5sigma limit averall)
Looking for transient sources on various timescales (s to y)
Follow-up of new and unidentified sources in other waveband
Overall analysis of all the sources: Spectra, timing, states
Go through this quickly – all demonstrated later 4

5. The soft gamma-ray sky according to IBIS…
421 sources from 3rd catalog
139 others (more recent IGR and known sources)
Around 400 more ‘under inspection’
More than 700 !!!
4th catalog almost ready
18-60 keV band

6. Source populations CAT 3 – E>17 keV6

7. Source populations above 100 keV7

8. IBIS GALACTIC Sources MAGNETARs (4+3) PSRs and PWN (13) OK,AGILE
NSs and BHCs in LMXB (59+14)
NSs and BHCs in HMXB (49+4) OK,AGILE
CVs
? still under ispection
AGNs in cat3, OK, AGILE

9. The AGILE SKY. From Pittori et al.2009
LSI
Cyg X-3
PSR J
PSR J
Eta Car
Vela PSR
Crab
PSR J

10. PSR/PWN

11. The light curve of the Crab emission as seen by INTEGRAL/SPI non-scattered events. The 0.1–1 MeV gamma-ray events used for the polarization analysis were selected from within the phase interval 0.5–0.8 of the pulsar period (shaded).
The gamma-ray polarization vector superimposed on a composite image of the Crab from Chandra (X-ray/blue) and HST (optical/red). The vector is drawn so as to pass through the position of the pulsar. The limits on the direction of the vector are indicated by the shading. The direction of the polarization vector shows a remarkable alignment with the inner jet structure.
Image credits NASA/CXC/ASU/J. Hester et al. (2002) Ap. J 577, L49 (X-ray) and NASA/HST/ASU/J. Hester et al. (2002) Ap. J 577, L49 (Optical)
The data are consistent with a linearly polarized beam with the electric vector at an angle of 123°±11° closely aligned with the pulsar spin orientation angle which has been estimated to be 124°.0±0°.1. The polarization is 46%±10%. The errors are dominated by non-statistical effects. The angle is measured from North, anti-clockwise on the sky.

12. Young Pulsars
Three young pulsars (< 10 kyr) so far studied at hard X-rays/soft g-rays: PSR B (Crab) PSR B PSR B
Different lightcurve shapes
HE-spectra of Crab and B0540 similar
Maximum Lg below 30 MeV
Lx/Lg GeV larger than for older pulsars
INTEGRAL profile:
Slowikowska et al. 2007

13. PSR B in MSH (G )
Pulse profile consistent with e.g. BATSE, RXTE,
but, INTEGRAL timing plus imaging gives results on the PWN,
see Forot et al. 2006
ISGRI 20 – 300 keV
power law with a= −2.12 up to 160 keV
Possible break at this energy

14. The emerging population of pulsar wind nebulae in soft-γ rays
PSRB as a test case (Campana et al. 2008)
synchrotron
Key range!
Up to know very little was known about PWN above 20 keV, yet soft gamma-rays are important diagnostic as they probe the end part of the synchrotron emission and show that particle acceleration is taking place near the pulsar
Results on other PWN
Name Dominance (IBIS range)
Crab PWN
PSR B PWN
Vela PWN
PSR J PWN
AXJ PSR
PSR J PWN
PSR J PWN
Archival X-ray data allowed to separate the pulsar and PWN emission in a number of systems including PSR B
The result is that the INTEGRAL emission is often dominated by PWN (Dean et al. 2009)

15. Middle age Pulsar: Vela
INTEGRAL 2.1 Msec
IBIS / ISGRI
PSR P1 P2
INTEGRAL
TOTAL
γ = 1.86 ± 0.03
6.2 σ
(ZN2)
IBIS, 5.1 Msec
PWN
PWN, EGRET
PSR

16. the second middle age Pulsar : PSRJ1420-6049
INTEGRAL mosaic in the energy range keV
a faint signal of 5 sigma is detected consistent with the position of PSR J This pulsar belongs to the middle aged class where the PWN interacts with the reverse shock of the Supernova Remnant. Interestingly, NO INTEGRAL counterpart to the Rabbit PWN candidate, Horns et al., ASS 309,215,2007

17. The PWN KeV to TeV connection
..and now GeV!!!
AGILE
AGILE
AGILE
AGILE
From Mattana et al. 2009, Dean et al., 2009

18. Microqsos LSI +61 303 a Be in a HMXB
20 – 95 keV: “OFF” (phase 0.8 – 1.3) “ON” (phase 0.3 – 0.8)
Microqsos

19. LSI +61 303, “ON” (phase 0.3 – 0.8) 45 – 95 keV 45 – 205 keV

20. AGL J2032+4102 ?=CYG X-3 Transition from the ultra-soft to the Hard state observed with INTEGRAL
Apparently, the ultrasoft state precedes the emission of a jet, which is apparent in the radio and hard X-ray domain
Beckman et al, 2008 A&A
During the ultrasoft state, the soft X-ray spectrum is well-described by an absorbed (NH = 1.5 × 1022 cm−2) black body model, whereas the X-ray spectrum above 20 keV appears to be extremely low and hard (≃ 1.7). During the transition, the radio flux rises to a level of > 1 Jy, and the soft X-ray emission drops by a factor of ∼ 3, while the hard X-ray emission rises by a factor of ~14 and becomes steeper (up to Ѓ= 4).

21. Hard X-ray emission from Eta Carinae
Tavani M. et al, ApJ accepted
From Leyder et al., 2008

22. NSs in HMXBs: Examples of important unexpected INTEGRAL discoveries and possible association with Gamma ray source
the highly absorbed (mostly transient) binary systems as a new class of HMXB: slow pulsar ( s period) in a giant cocoon (Nh often >23)
the super-giant fast transients: a new (sub) class of super-giant HMXB (wind accretion in blobs?)
V. Sguera et al., ApJ 646,
IGR J
2 hr flare
R. Walter et al., A&A 411, L427, 2003
XMM
INTEGRAL/IBIS
IGR J
See Vito Sguera talk