1. Christoph Winkler, AWG #127, 18 January 2007, Page 2
INTEGRAL
Gamma-ray observatory
15 keV – 10 MeV
High resolution spectroscopy (SPI) and fine imaging (IBIS) within large FOV
Medium-size mission (ESA, Russia, NASA), launched in Oct 2002
Community involved via
AO programme (AO-4: 142 proposals, x 8 over-subscribed)
Public archive access
IUG, ISWT, TAC
AO-4: 65% of accepted proposals have PI’s from outside the h/w (PI) teams
Christoph Winkler, AWG #127, 18 January 2007, Page 2

2. INTEGRAL in perspective
SPI/INTEGRAL: THE unique spectrometer for nuclear-line astrophysics.
INTEGRAL science of nuclear lines is not done by any other current nor foreseeable instrument, with broadest application in astrophysics.
IBIS/INTEGRAL: THE best imager for high energy sources
Fine imaging and monitoring of large parts of the highly variable sky is crucial for high energy sources
Christoph Winkler, AWG #127, 18 January 2007, Page 3

3. Great science achieved: SPI
Annihilation of e- with e+ presents a unique view of the Galaxy (and big problem! Expected SNII which are disk!)
Reference
Topic
Citations
C. Böhm et al.
Phys. RevL 92, , 2004
MeV dark matter: has it been detected ? 93
P. Jean et al.
A&A 407, 55, 2003
511 keV line emission from 4th quadrant 82
J. Knödlseder et al.
A&A 411, 457, 2003
Constraints on the 511 keV line morphology 72
A&A 441, 513, 2005
511 keV all-sky distribution 46
Christoph Winkler, AWG #127, 18 January 2007, Page 4

4. Great science achieved: SPI
Radioactivity lines (26Al) yield direct measure of the Galactic supernova rate 1.91.1/century and rotation shows it’s the whole galaxy not nearby SN
Reference
Topic
Citations
R. Diehl et al.
Nature 439, , 2006
Radioactive 26Al from massive stars in the Galaxy 16
Christoph Winkler, AWG #127, 18 January 2007, Page 5

5. Great science achieved: IBIS
Cosmic X-ray background. First hard X-ray determination since HEAO-1: normalisation is 10% higher, better match with RXTE and Chandra. Need more obscured SMBH!
Reference
Topic
Citations
E. Churazov et al.
A&A, submitted, 2006
INTEGRAL observations of the cosmic X-ray background 2
Christoph Winkler, AWG #127, 18 January 2007, Page 6

6. Great science achieved: IBIS
Survey!
DISCOVERY: Accreting binaries within dense clouds (Why are they all slow spinning NS, not BH?)
DISCOVERY: hard tails in magnetars/AXPs (How does particle acceleration work?)
Reference
Topic
Citations
A. Bird et al.
ApJ 607, 33, 2004
The first IBIS source catalogue 63
M. Revnivtsev et al.
AstL 30, 382, 2004
Hard X-ray survey of the GC region 50
R. Walter et al.
A&A 411, L427, 2003
INTEGRAL discovery of IGR J 35
Christoph Winkler, AWG #127, 18 January 2007, Page 7

7. INTEGRAL science impact
Refereed papers since launch
240 refereed papers since launch using scientific data
In 2006: 98 refereed papers (2 papers per week )
409 non-refereed papers (conference proc., etc.) 
C. Winkler et al.
A&A 411, 1, 2003
The INTEGRAL mission
218
Christoph Winkler, AWG #127, 18 January 2007, Page 8

8. FUTURE: Key programmes (as suggested by AWG)
Observing programme AO-5,
Total per year: 24 Ms
Observing programme AO-6+,
typical for 2009+
Total per year: 24 Ms
TODAY
Very appropriate for INTEGRAL as long exposures needed
AO-4: KP lite on GC! 43 proposals (142 total) submitted for this
AO-5 for Key Programmes (Nov 2006): NOT including pointed AO
KP proposals over-subscribed by factor 8.7 for one year
10 out of 22 proposals asking for a multi-year programme
Christoph Winkler, AWG #127, 18 January 2007, Page 9

9. Deep 511 keV (all-sky) map and source of positrons
Emission fm disk 4.7σ
Initial evidence for contribution from “halo” around bulge or from disk component extended in latitude ?
Identify the primary source of positrons which is currently unknown
SN Ia ?
Micro-quasars ?
Light DM ?
Pulsar winds from ms pulsars ?
All-sky galactic projection - contours at 500ks intervals
3rd IBIS catalogue, exposure map, A. Bird et al., 2007
511 sky map, 1 year, J. Knödlseder et al., 2005
Christoph Winkler, AWG #127, 18 January 2007, Page 10

10. Christoph Winkler, AWG #127, 18 January 2007, Page 11
Mapping nuclear lines
M . Harris et al., A&A 433, L49, 2005
Σ 1173 and 1333 keV
69Ge bkgd
60Fe
Just now detecting 60Fe
Flux ratio 60Fe/26Al = 0.11±0.03, substantially below predictions for massive stars (≥ 0.40)
Nuclear physics ? (cross sections, β-decay rate for Fe ?)
Core-collapse SN not the primary 26Al-source ?
Need large additional source for 26Al acting prior to core collapse → massive winds during WR-phase
Future: mapping of 26Al and 60Fe lines. Might be different in different SFR depending on number of WR stars
Where is 44Ti (68, 78 keV) predicted by 60Fe and 26Al?
Christoph Winkler, AWG #127, 18 January 2007, Page 11

11. Diffuse Galactic continuum emission > 100 keV
RXTE
350o<l<10o
2o<|b|<10o
INTEGRAL
Comptel
Egret
Inverse Compton
Is the diffuse Galactic ridge emission truly diffuse ? Or
Can the emission from
the galactic ridge be
almost entirely
attributed to (unresolved) WD binaries ?
Requires (very) deep GP exposure (~ 5 Ms/y until 2014) e.g. outside the bulge/inner region (where point source population should drop off)
INTEGRAL will also observe high energy extension, unlike SWIFT
Extragal bgknd
A. Strong et al., A&A 444, 495, 2005
60 keV ~ proton
binding energy of white dwarf
R. Krivonos et al., A&A in press 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 12

12. Cosmic diffuse X-ray background (CXB)
Churazov et al., A&A in press, 2006
Initial CXB observations (2006) via Earth occultation were highly successful (test method, spectral normalisation)
Need long observations during solar maximum (away from GP) to verify robustness of Earth atmospheric emission and to obtain CXB spectrum in broader range
The CXB luminosity peaks at 30 keV – what produces this radiation ?
INTEGRAL’s AGN INITIAL survey results find that “Compton thick” AGN contribute only a few % to the CXB
Where are the super-massive BH’s ?
Not in the local (z=0.022) universe where (the surrounding gas/dust torus has been ‘’removed’’), or,
Within the local universe, but much more “hidden” than assumed
INTEGRAL will probe AGN population deeply not to just increase numbers of AGN, but to measure properties of the population at faint flux levels
Christoph Winkler, AWG #127, 18 January 2007, Page 13

13. INTEGRAL and TeV science: HESS, MAGIC
Continue INTEGRAL/HESS collaboration to correlate sky maps and create maps of combined detection significances
The keV to TeV connection: a new class of cosmic high energy accelerators
Nature of SNR, pulsars/PWN observed at TeV and at soft γ-rays ?
Same emitting region ? Same mechanism ?
IGR J = HESS J
Ubertini et al., 2005
VHE emission fm core or shell of SNR ?
Leptonic vs hadronic models
Funk et al., 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 14

14. Unidentified (very) high energy sources
INTEGRAL deep sky maps to allow detection of yet un-identified very high energy sources fm COS-B, EGRET, GLAST, AGILE, HESS…
Persistent = normal pulsars and ms radio pulsars
Variable = micro-quasar/pulsar binaries
Extragalactic sources (variability studies: gain ~ time, not sqrt(time) )
Need typically 10 Ms on plane
 Recent example: the Microquasar and TeV/EGRET/ COS-B source LSI seen by INTEGRAL
LSI
QSO
3EG J
3EG J
Hermsen et al., 2006
Egret contours
Christoph Winkler, AWG #127, 18 January 2007, Page 15

15. INTEGRAL and GeV science: GLAST, AGILE
GLAST, 20 MeV - >300 GeV, launch fall 2007, operational through 2010+
AGILE, 30 MeV – 30 GeV, launch spring 2007, operational through 2010+
Most AGN are highly variable and multi-wavelength studies are crucial to simultaneously observe from hard X-rays/soft gamma-rays up to very high energy gamma-rays (also including HERSCHEL,HESS/MAGIC)
 GLAST will tell INTEGRAL “when to look’’: both for extragalactic and for galactic sources
INTEGRAL
GLAST
Blazar 3C in outburst
E. Pian et al., A&A 449, L21, 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 16

16. The INTEGRAL large field of view
SPI
IBIS
XMM (30’)
HMXB
SNR
AXP
ms-pulsar
Diffuse emission (26Al, 60Fe)
from Gal plane
Many different source types – outside GC and bulge !
b [deg]
l [deg]
INTEGRAL/IBIS map of Cassiopeia region (20-50 keV)
Ms, 0.4 – 12 mCrab, den Hartog et al. 2005
Christoph Winkler, AWG #127, 18 January 2007, Page 17

17. The variable high-energy sky
3 deg
GC region, keV, time step = 3 days
The high energy sky is highly variable and ToO’s are important
35 ToO follow-up observations (~ 10 Ms, Jan 03 – Dec 06)
Monitoring the sky in this energy range is of fundamental importance (as are multi-λλ follow-ups)
Christoph Winkler, AWG #127, 18 January 2007, Page 18

18. Bright Galactic X-ray Novae
A , discovered by ARIEL in 1975
Nova Muscae 1991, discovered by GRANAT and Ginga 1991
5 bright novae since 1975, None occurred during 4 years of Integral operations
High quality spectra to study stellar-sized accreting BH’s
511 keV line emission (cf Nova Muscae) and h.e. tail ?
Compton backscatter line (170 keV) from accretion disk ?
Are novae significant contributors to e+ production in our Galaxy ?
Christoph Winkler, AWG #127, 18 January 2007, Page 19

19. The next Galactic Supernova
The ultimate goal for thermonuclear supernovae (SN Ia) is to understand
how much 56Ni is synthesized,
where - within the ejecta - it is produced, and
how fast the 56Ni and overlying ejecta expand.
This information will exclude many (!) of the possible models.
Historic SN
Year -
1006
Crab
1054
Tycho
1572
Kepler
1604
Cas A
± 1670
???
It’s time !
Christoph Winkler, AWG #127, 18 January 2007, Page 20

20. The next Galactic (or near-by) Supernova
SN Ia (WD thermonuclear explosion), rate: ~ 0.06 per 100 y in Galaxy (*) and ~ 1 per 5 years up to 5 Mpc (+)
Detect lines from 56Ni ->56Co ->56Fe (158, 812, 847, 1238, 2599 keV…)
Detect Compton-scattered continuum from these lines
Measure synthesized 56Ni mass and its distribution in ejecta
Measure ejection dynamics via line profile variations
Interactions between shock and circum-stellar medium
For galactic ‘’once in a lifetime’’ SN: 7Be, 59Fe, 22Na, 57Co, 60Co, 44Ti
SN II (massive star core collapse), lower 56Ni yield, higher mixing (obstruction) > lower flux, but higher rate: (1.9±1.1) per 100 y in Galaxy (#)
* S. Schanne et al., N. Gehrels et al., # Diehl et al., 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 21

21. Christoph Winkler, AWG #127, 18 January 2007, Page 22
INTEGRAL and SWIFT
Continue strong and excellent collaboration on important complementary observations on GRB’s, SGR’s, and follow-ups of new IGR/SWIFT sources
SWFIT/BAT telescope performs serendipitous sky survey during slews to/from GRB sites
50 – 150 keV
FOV: 1.4 sr (FWHM)
Higher bkgd (FOV), but larger detector area -> BAT performance comparable to ISGRI as survey instrument
INTEGRAL and SWIFT/BAT extragalactic surveys complement each other well thanks to programmed vs serendipitous pointing strategies.
Christoph Winkler, AWG #127, 18 January 2007, Page 22

22. Christoph Winkler, AWG #127, 18 January 2007, Page 23
Great science ahead
Nuclear gamma-ray lines in the Galaxy (2010+)
The primary positron sources
Radioactivity and galactic structure
The nature of the Galactic ‘diffuse’ continuum emission > 100 keV (2010+)
Cosmic diffuse background radiation and Compton-thick AGN (2010+)
Unidentified very high energy sources: GLAST/AGILE (2007+)
INTEGRAL and TeV astronomy: HESS/MAGIC (now+)
Unexpected new discoveries (now+)
Galactic SN, bright X-ray novae, ToO’s
Christoph Winkler, AWG #127, 18 January 2007, Page 23

23. Christoph Winkler, AWG #127, 18 January 2007, Page 24
Summary
INTEGRAL is a mature high-energy mission, works extremely well, and delivers the science it was built to do
The scientific output is high with increasing rate.
SPI/INTEGRAL: THE unique spectrometer for nuclear-line astrophysics.
INTEGRAL science of nuclear lines is not done by any other current nor foreseeable instrument, with broadest application in astrophysics.
IBIS/INTEGRAL: THE best imager for high energy sources
Fine imaging of and monitoring of large parts of the highly variable sky is crucial for high energy sources
Some overlap with SWIFT/Suzaku but enough science for all
Europe is now harvesting the reward for its substantial investment in INTEGRAL through ESA, and through the nationally funded instruments and data centre. We should continue to support these activities !
Christoph Winkler, AWG #127, 18 January 2007, Page 24