the integral galactic sky synergy with agile
DESCRIPTION
The INTEGRAL Galactic Sky Synergy with AGILE. P. Ubertini, A. Bazzano, A. Tarana on behalf of the IBIS Survey Team. OUTLINE IBIS and its capabilty The IBIS view of the Galactic Gamma–ray Sky The IBIS AGILE Galactic source. INTEGRAL overview. IBIS. SPI. Credit: ESA. - PowerPoint PPT PresentationTRANSCRIPT
The INTEGRAL Galactic SkySynergy with AGILE
P. Ubertini, A. Bazzano, A. Tarana on behalf of the IBIS Survey Team
OUTLINE
•IBIS and its capabilty
•The IBIS view of the Galactic Gamma–ray Sky
•The IBIS AGILE Galactic source
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 17-600 keV
Sensitivity <0.5mCrab for deep exposures
JEM-X and
Credit: ESA
IBISIBIS
SPISPI
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 days100Ms (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
The soft gamma-ray sky according to IBIS…
18-60 keV band
421 sources from 3rd catalog139 others (more recent IGR and known sources)Around 400 more ‘under inspection’
More than 700 !!! 4th catalog almost ready
Source populations CAT 3 – E>17 keV
Source populations above 100 keV
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 21
? still under ispection AGNs 136 in cat3, OK, AGILE
LSI +61303 Cyg X-3
PSR J1826-1334 PSR J1509-5850
Eta Car
Vela PSRCrab
PSR J1420-6048
The AGILE SKY. From Pittori et al.2009
PSR/PWN
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.
Young Pulsars
Three young pulsars (< 10 kyr) so far studied at hard X-rays/soft -rays:
PSR B0531+21 (Crab)
PSR B1509-58
PSR B0540-69
Different lightcurve shapes HE-spectra of Crab and B0540 similar
Maximum L below 30 MeV
Lx/L GeV larger than for older pulsarsINTEGRAL profile:Slowikowska et al. 2007
PSR B1509-58 in MSH 15-52 (G320-1.2)
ISGRI 20 – 300 keV Pulse profile consistent with e.g. BATSE, RXTE, but, INTEGRAL timing plus imaging gives results on the PWN, see Forot et al. 2006
power law with a= −2.12 up to 160 keVPossible break at this energy
The emerging population of pulsar wind nebulae in soft-γ rays
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 pulsarArchival X-ray data allowed to separate the pulsar and PWN emission in a number of systems including PSR B0540-69The result is that the INTEGRAL emission is often dominated by PWN (Dean et al. 2009)
Results on other PWNName Dominance (IBIS range)Crab PWNPSR B0540-69 PWNVela PWN PSR J1811-1925 PWNAXJ 1838-0655 PSRPSR J1833-1034 PWNPSR J1846-0258 PWN
synchrotron
PSRB 0540-69 as a test case (Campana et al. 2008)
Key range!
Middle age Pulsar: Vela
INTEGRAL 2.1 MsecIBIS / ISGRI
6.2 σ
(ZN
2)
P1 P2
PSR
INTEGRAL TOTALγ = 1.86 ± 0.03
PWN, EGRET
PSR
PWN
IBIS, 5.1 Msec
the second middle age Pulsar : PSRJ1420-6049
INTEGRAL mosaic in the energy range 20-40 keVa faint signal of 5 sigma is detected consistent with the position of PSR J1420-6048. 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
The PWN KeV to TeV connection ..and now GeV!!!
From Mattana et al. 2009, Dean et al., 2009
AGILE
AGILE
AGILE
AGILE
LSI +61 303 a Be in a HMXB 20 – 95 keV:
“OFF” (phase 0.8 – 1.3) “ON” (phase 0.3 – 0.8)
Microqsos
LSI +61 303, “ON” (phase 0.3 – 0.8)
45 – 95 keV 45 – 205 keV
AGL J2032+4102 ?=CYG X-3 Transition from the ultra-soft to the Hard state
observed with INTEGRAL
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).
Apparently, the ultrasoft state precedes the emission of a jet, which is apparent in the radio and hard X-ray domain
Hard X-ray emission from Eta Carinae
From Leyder et al., 2008
Tavani M. et al, ApJ accepted
NSs in HMXBs: Examples of important unexpected INTEGRAL discoveries
and possible association with Gamma ray source1. the highly absorbed (mostly transient) binary
systems as a new class of HMXB: slow pulsar (100-1000s period) in a giant cocoon (Nh often >23)
2. the super-giant fast transients: a new (sub) class of super-giant HMXB (wind accretion in blobs?)
R. Walter et al., A&A 411, L427, 2003
XMM
INTEGRAL/IBIS
IGR J16318-4848
V. Sguera et al., ApJ 646, 453 2006
IGR J174544-2619 2 hr flare
See Vito Sguera talk