Transcript INTEGRAL AO-1: preliminary results

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 ewith e+ presents
a unique view of
the Galaxy (and
big problem!
Expected SNII
which are disk!)
Reference
Topic
C. Böhm et al.
MeV dark matter: has it been
detected ?
93
P. Jean et al.
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
J. Knödlseder et al.
511 keV all-sky distribution
46
Phys. RevL 92, 101301, 2004
A&A 407, 55, 2003
A&A 441, 513, 2005
Christoph Winkler, AWG #127, 18 January 2007, Page 4
Citations
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
R. Diehl et al.
Radioactive 26Al from massive
stars in the Galaxy
Nature 439, 45 92, 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 5
Citations
16
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
E. Churazov et al.
INTEGRAL observations of the
cosmic X-ray background
A&A, submitted, 2006
Christoph Winkler, AWG #127, 18 January 2007, Page 6
Citations
2
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
A. Bird et al.
The first IBIS source catalogue
63
M. Revnivtsev et al.
Hard X-ray survey of the GC
region
50
R. Walter et al.
INTEGRAL discovery of IGR
J16318-4848
35
ApJ 607, 33, 2004
AstL 30, 382, 2004
A&A 411, L427, 2003
Christoph Winkler, AWG #127, 18 January 2007, Page 7
Citations
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
Christoph Winkler, AWG #127, 18 January 2007, Page 8
218
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
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
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Emission fm disk now @ 4.7σ
Initial evidence for contribution from “halo” around bulge or from disk
component extended in latitude ?
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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
511 sky map, 1 year, J. Knödlseder et al., 2005
3rd IBIS catalogue, exposure map, A. Bird et al., 2007
Christoph Winkler, AWG #127, 18 January 2007, Page 10
Mapping nuclear lines
Σ 1173 and 1333 keV
60Fe
69Ge
bkgd
Just now detecting 60Fe
Flux ratio 60Fe/26Al = 0.11±0.03,
substantially below predictions for
massive stars (≥ 0.40)
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M . Harris et al., A&A 433, L49, 2005
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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
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
INTEGRAL
RXTE
350o<l<10o
2o<|b|<10o
Comptel
Egret
Inverse Compton
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)
 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

Churazov et al., A&A in press, 2006
 The CXB luminosity peaks at 30 keV – what produces this radiation ?
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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 ?
o
Not in the local (z=0.022) universe where (the surrounding gas/dust torus
has been ‘’removed’’), or,
o
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
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Nature of SNR, pulsars/PWN observed at TeV and at soft γ-rays ?
Same emitting region ? Same mechanism ?
IGR J18135-1751 = HESS J1813-178
VHE emission fm
core or shell of
SNR ?
Leptonic vs
hadronic models
Ubertini et al., 2005
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…
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Persistent = normal pulsars and ms
radio pulsars
Variable = micro-quasar/pulsar
binaries
Extragalactic sources (variability
studies: gain ~ time, not sqrt(time) )
Hermsen et al., 2006
QSO 0241 +622
 Need typically 10 Ms on plane
3EG J0229+6151
LSI +61 303
 Recent example: the Microquasar
3EG J0241+6103
and TeV/EGRET/ COS-B source LSI
+61 303 seen by INTEGRAL
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+
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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
Many different source types – outside GC and bulge !
b [deg]
SPI
IBIS
SNR
AXP
HMXB
ms-pulsar
XMM (30’)
Diffuse emission (26Al,
from Gal plane
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
60Fe)
l [deg]
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
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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
Year
The ultimate goal for thermonuclear
supernovae (SN Ia) is to understand
-
1006
Crab
1054
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Tycho
1572
Kepler
1604
Cas A
± 1670
???
???
It’s time !
Historic
SN
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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.
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 (+)
o Detect lines from 56Ni ->56Co ->56Fe (158, 812, 847,
1238, 2599 keV…)
o Detect Compton-scattered continuum from these lines
o Measure synthesized 56Ni mass and its distribution in
ejecta
o Measure ejection dynamics via line profile variations
o Interactions between shock and circum-stellar medium
o 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
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
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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
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
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