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

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

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, 101301, 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

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, 45 92, 2006 Radioactive 26Al from massive stars in the Galaxy 16 Christoph Winkler, AWG #127, 18 January 2007, Page 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

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 J16318-4848 35 Christoph Winkler, AWG #127, 18 January 2007, Page 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

FUTURE: Key programmes (as suggested by AWG) Observing programme AO-5, 2007-2008 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

Deep 511 keV (all-sky) map and source of positrons Emission fm disk now @ 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

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

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 Cutoff @ 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

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

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 J18135-1751 = HESS J1813-178 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

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 +61 303 seen by INTEGRAL LSI +61 303 QSO 0241 +622 3EG J0241+6103 3EG J0229+6151 Hermsen et al., 2006 Egret contours Christoph Winkler, AWG #127, 18 January 2007, Page 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 454.3 in outburst E. Pian et al., A&A 449, L21, 2006 Christoph Winkler, AWG #127, 18 January 2007, Page 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) 0.7-1.6 Ms, 0.4 – 12 mCrab, den Hartog et al. 2005 Christoph Winkler, AWG #127, 18 January 2007, Page 17

The variable high-energy sky 3 deg GC region, 17-60 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

Bright Galactic X-ray Novae A 0620-00, 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

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

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., 2006 + N. Gehrels et al., 1987 # Diehl et al., 2006 Christoph Winkler, AWG #127, 18 January 2007, Page 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

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

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