ESA INTEGRAL
satellite
... and Czech Participation
3rd INTEGRAL/BART
Workshop Chocerady
2.11.2004
1. astrophysics ESA satellite with Czech participation
The INTEGRAL
Mission
•
Gamma-ray observatory with concurrent
X-ray and optical monitoring.
•
INTEGRAL is the ESA Science
Programme’s mission launched on
October 17, 2002.
•
ESA’s 2nd γ-ray mission (COS-B, 1975),
will join XMM-Newton in orbit.
•
ESA led mission in collaboration with
Russia, United States, Czech Rep. and
Poland
•
•
•
Lifetime of at least 5 years.
Highly eccentric 72 hour orbit.
Observing programme includes 65-75%
open time.
INTEGRAL under Thermal Vacuum
testing at ESTEC
Integral ISWG
The INTEGRAL FM and the ISWT @ ESTEC, 26 March 2002
Images from the Bajkonur cosmodrome: Integral ready for launch with Proton
rocket on Oct 17 at 4.41 UT
Integral launch event: ESA MOC, Darmstadt,
October 17 from 3.30 UT
TV also via Astra satellite
INTEGRAL in a Nutshell
Perigee: 9,000
km, Apogee:
150,000 km
4.1 tonnes
5 m high, 3.7 m
diameter
16 m solar
panels
The INTEGRAL instruments
IBIS – The gamma-ray
Imager onboard the
INTEGRAL satellite.
Excellent Imaging, good
spectra
Jem-X - The Joint
European X-ray
Monitor
OMC – Optical
Monitor Camera.
SPI – The gamma-ray
Spectrometer on
INTEGRAL. Excellent
spectra, good images
The complex INTEGRAL instruments were built by
large collaborations…
Instrument
Principal Investigators
Collaboration
IBIS
P. Ubertini (I), F. Lebrun
(F), G. Di Cocco (I)
Italy, France, Norway, Germany, Spain, USA,
Poland, UK
SPI
J.-P. Roques (F),
V. Schönfelder (D)
France, Germany, Italy, Spain, Belgium, UK,
USA
JEM-X
N. Lund (Dk)
Denmark, Finland, Spain, Italy, USA, Sweden,
UK, Poland, Russia
OMC
M. Mas-Hesse (ES)
Spain, Ireland, Belgium, UK, Czech Republic
Science
T. Courvoisier (CH)
Data Centre
Switzerland, France, Germany, Italy, Denmark,
UK, Belgium, USA, Czech Republic, Poland
Imager on-board the INTEGRAL
(IBIS)
• 15 keV – 10 MeV energysatellite
range
• 16384 CdTe (ISGRI) and 4096 CsI (PICsIT) detectors.
E/ΔE ~10.
• 9 x 9 degree fully coded FOV. 12 arcmin FWHM
angular resolution. 30 arcsec location accuracy.
• 630 kg
• Accurate point source imaging and location. Broad
lines and continuum.
IBIS detector unit
being integrated
onto the spacecraft
in November 2001
Image of a bronze statue which was
placed above the ISGRI detector and
illuminated by a 57Co 122 keV X-ray
source at CEA in July 2001. “Gaps”
between the modules will be much
smaller than in this test.
Spectrometer on INTEGRAL (SPI)
• Fine spectroscopy of narrow lines and the study of diffuse
emission on > degree scales.
• 20 keV to 8 MeV energy range
• 19 cooled (90o K) Ge detectors. E/ΔE ~500.
• 16 degree fully coded FOV with 2.5 degree FWHM imaging
resolution. Location accuracy <1.3 degree
• 1300 kg
SPI detector
plane (FM)
SPI science calibration image of two 60Co 1.1 MeV -ray
sources separated by 2 degrees showing that they are
well resolved.
Joint European X-ray Monitor (JEM-X)
• 3 –35 keV X-ray monitoring
• 2 identical Microstrip Xe gas detectors and coded
masks.
• Source identification and monitoring in X-rays
• 5 degree diameter FOVs with 3 arcmin FWHM
spatial resolution. 30 arcsec location accuracy.
• Energy resolution of 15% at 10 keV
• 65 kg
The coded mask viewed
during testing with a
flight detector
Optical Monitoring Camera (OMC)
• 500 – 600 nm wavelength range
• CCD (2048 x 1024 pixels)
• 5 x 5 degree FOV, 20” imaging
• Optical monitoring of high-energy
sources
• 17 kg
• Sensitivity: 18.2 mag in 1000 s
• Czech participation: onboard
software, ISOC and ISDC software,
simulators, test camera, tests,
science
INTEGRAL Observing Programme
Core program (35-25%)
• Galactic centre deep exposure (GCDE) : 4 106 s
• Weekly galactic plane scans (GPS) : 2 106 s
• Transient events (TOO) : 2 106 s
• Vela region deep exposure : 106 s
Open time (65-75%)
• Compact objects (Galaxy and Magellanic Clouds) : 8 106 s
• AGN : 4 106 s
• Diffuse emission (continuum and lines) : 5 106 s
• Supernova nucleosynthesis : 3.5 106 s
• Transient events (TOO) : 2 106 s (effective time)
GCDE Pointing Pattern
INTEGRAL fields-of-view
Fully coded fields of
view :
• OMC : 5°
• SPI : 16°
• JEM-X : 4.8°
• IBIS
: 9°
Dithering patterns:
• staring
• 7 point hexagonal
• 5  5 rectangular
The INTEGRAL Science and Data Centre ISDC
• It is the task of the INTEGRAL Science
Data Centre in Versoix, Switzerland to
make the data from all the instruments
available to the scientific community.
• Not only are the instruments built by
large collaborations…
• Czech participation: consortium
member, Co-I, direct participation to the
team, science
ISDC - members of the consortium
ISDC
Integral multispectral imaging: BH candidate Cyg X-1
Integral exposure map with main sources labeled
GPS scan (29 Jan 2003) Dl = 270o – 337o
Mosaic of 11 pointings
(24200
sec), IBIS/ISGRI,
4U 1630-47, BHC
15-40 keV
First TOO follow-up
observation (PI: J. Tomsick)
on 1 & 2 Feb 2003, 300 ksec
IGR J16318-4848
IBIS team
First new (transient) source detected by INTEGRAL (IBIS/ISGRI) during GPS at
Jan 29.271 UT (IAUC # 8063).
LMX region
LMX X-3
and LMC X4
JEM-X image
Cyg region by ISGRI/IBIS 15-40 keV
The First Gamma-ray Burst observed by INTEGRAL
1905+105, microquasar and BH candidate, time variability by Jem X, AO-1
pointing
Pulses of Crab pulsar in various energy ranges, IBIS
Multi instrument
spectra of Cyg X3, JEM X, ISGRI,
SPI
First OMC image from space
OMC Pointing Software OMC PS
Part of ISOC - Integral Science Operation Centre
Generates telecommands sent to the satellite
Controlls the OMC
Selects objects observed
Transfer of up to 100 objects
Selection of objects in photometric shot
0.05
0.05
48.0
0.04
0.04
47.0
0.03
0.03
46.0
0.02
0.02
0.01
0.01
45.0
0.00
44.0
-0.05
-0.04
-0.03
-0.02
-0.01 0.00
-0.01
43.0
0.01
0.02
0.03
0.04
0.05
-0.02
42.0
6.0
7.0
8.0
9.0 10.0 11.0 12.0 13.0 14.0
Rektascenze
0.00
-0.0 -0.0 -0.0 -0.0 -0.0
-0.010.00 0.01 0.02 0.03 0.04 0.05
5
4
3
2
1
-0.02
-0.03
-0.03
-0.04
-0.04
-0.05
-0.05
CCD souřadnice
CCD souřadnice
Magnitudy vybraných objektů
1000 4
800
800
600
400
600
1
400
200
200
y
0
0
200
400
600
x
800
1000
12.0
8
10
11.0
5
9
Magnituda
1000
y
Deklinace
Gnom onická projekce - otočení
Gnom onická projekce
Fotom etrický sním ek (střed 10.12, 45.12,
otočení 10.0)
10.0
9.0
3
7
0
20
200
400
6
600
x
8.0
800
1000
7.0
1
2
3
4
5
6
7
8
9
10
First OMC image from space .... after running the OMC Pointing Software
developed by Věra Hudcová with help of Filip Hroch and Jiří Polcar at HEA
Group, Astronomical Institute Ondřejov
Cyg X-1 optical
image by OMC
Test variable star:
testing performance
of OMC and s/w
Eclipsing binary Y Sex , OMC LC
INTEGRAL News
- all working OK including Czech deliveries
- fuel supply for 15 years
- the mission officially for 2.2 years lifetime, will be extended on
4 year term basis, recently until end of 2008
AO-3
Evaluations in progress at the ISOC for the
INTEGRAL AO-3 proposals.
This will cover observations between 18 February 2005
and 17 August 2006.
The AO - 3 proposals were due by 29 October 2004.
We and AO-3: 1 our proposal Simon et al. (CV ToO), 2
collaborative proposals - blazars ToO and GRBs.
Integral scientific data
Core Programme - Galactic Scans, Vela, Galactic
Center ... we have data rights. Huge scatter in number
of data points. Short exposures of order of 1ksec, low
sensitivity, long term studies, CVs only in flaring state,
so far only 3 CVs detected by IBIS, but: cumulative
exposures will improve with time
AO pointings - objects inside the FOV ... the data
rights has the corresponding PI, work in collaboration
with him. Long exposures 10ksec and more, better
sensitivity, but limited long-term studies
Access to INTEGRAL data
Hardware Teams:
Core Programme (CP): Galactic Plane Survey (GPS), Galactic Center
Deep Exposure (GCDE), Vela Deep Exposure, ToO
All:
by proposal submisions for AO-1, AO-2, ... (open time pointings)
All:
all data public after 12 months (at moment > 12 months)
Tools:
OSA (off-line analysis software package) provided by ISDC
Main ISDC in Versoix, Switzerland
Secondary centers in Moscow, Russia, and Ondrejov, Czech Rep.
Core Programme
•CP is divided according to the scientific topics
•Each scientific topic has a responsible scientist delegated by the
INTEGRAL ISWT (R_Sci)
•The R_Sci has data rights for the corresponding scientific topics
•Each R_Sci has a right to organize a working group with members
also outside the hardware teams
•The R_Sci for the topic 5.5 WD Binaries including CVs is Rene
Hudec. The WG Cataclysmic Variables has bee established
Galactic
Scans
Data source
of the Core
Programme
CVs, blazars
The image shows the results of the first year of
processingof the IBIS Survey. This is a
composite significance image ofthe whole
galactic plane. It has been made from all
surveypointings in revolutions 46 to 120 in the
30-50keV energyband for a total exposure of
approximately 5 Ms. Around 120sources can be
found in the all-sky image; more detairevealed in
the inset zoomed images for two re
JEM-X 2 mosaic image of the Galaxy in the 2-5 keV energy band. The image includes all Galactic Plane Scans (GPS) and all Galactic Center
Deep Exposures (GCDE) taken during roughly the first year of INTEGRAL's mission. The four pannels are, from top to bottom, the intensity
image, the variance map, the significance image and the exposure map.
These two images show a deep
exposure (~700 ks obtained from
Galactic
Center Deep Exposure observations) of the
Norma spiral arm tangent
region. The images show the IBIS/ISGRI
image in the 20-100 keV range
(top) with EGRET contours superimposed and
the 100-250 keV image
(bottom). In the case of 3EG J1639-4702 the
possible dust-enshrouded
source IGR J16313-4643 has been proposed
as a counterpart (Malizia et
al. 2004, Atel 227; Combi et al. 2004, astroph/0401643). However, the
high energy image shows that only GX
337+00 (a black hole candidate)
emits above 100 keV. GX 337+00 shows
many chararacteristics of
galactic microquasars (radio jets, QPO, and
X-ray behaviour).
The IBIS/ISGRI image (top; 18-60
keV) shows the inner 3.5 degree by
2.5 degree region of the center of the
Galaxy. Contours represent
signal-to-noise levels starting at S/N
= 5 and increasing with a
factor 1.4. The image has a total
effective exposure time of 2.3 Ms.
The bottom image is the same
INTEGRAL image, however, now
with
the brightness distribution of the 6.4
keV iron line as determined by
ASCA/GIS, overplotted as contours.
GRB030501 "Labor Day
GRB"
SPI image
Real-time
localization by
IBIS and IBAS
alert response
1st "Czech" lead analyse
GRB observed by
INTEGRAL (according to
negotiated rotation of
responsibilities of
instrumental teams)
Observations of CVs by INTEGRAL
• in galactic plane survey GPS +- 13 degrees from the galactic
plane
• possibly: ToO - transients-outbursts-flares: polars, possible MeV
gamma-ray CVs (VV Pup, E1405-45), CVs with VHE emission
(AO Psc, EXO 033319-2554.2), AM Her, Aql X-1, AE Aqr
• in the FOV of pointed observations (for other sources) within the
AO-1,2 programme
•for good science, we aim to add additional data and clever ideas
TeV and GAMMA-RAY EMISSION FROM
CATACLYSMIC VARIABLES
…. Suitable candidates for the INTEGRAL Core Programme
• largely unexplored field - some positively detected CVs
• AE Aqr - intermediate polar; occasional flares Meintjes et al.
(1992) - correlated pulsed optical and very high energy emission
(VHE) (2.4 TeV, 1.5x1032 ergs/s)
• possible detection of VHE from another 7 CVs (Meintjes et al.
1992) (e.g. AO Psc, EXO 033319-2554.2)
• AM Her - gamma-ray emission (prototype polar)
• VV Pup, E1405-45 - possible MeV gamma-ray CVs
Secondary INTEGRAL Science and Data Centre, Ondřejov
Czech participation
OMC Optical Monitoring Camera (consortium members, Co-I)
•onboard s/w, centering algorithm, compression,...
•simulator
•test device = BART WF camera and related s/w
•OMC Pointing Software, tests, astrometry, interactive s/w
•science
ISDC Integral Science and Data Centre (consortium members, co-I)
•OPUS, GRBs alert, OMC ISDC s/w
•science
Ground segment
•BART, BOOTES
Cataclysmic Variables/WD Binaries in
the INTEGRAL Core Programme
CVs can be sources of radio ... TeV
gamma rays like blazars
Optical light curve
GK Per
X-ray
spectrum
X-ray light curve
CVs in INTEGRAL Core Programme
•investigation of gamma-ray component in CVs emission (mostly
flares)
•investigation of X-ray and hard X-ray component (mostly flares)
•multispectral observations and analyses
•focus on selected objects and types with high energy emission
•complex analyses supported by ground based data
•long term evolution analyses (galactic scans)
•study of related physical processes
Members of INTEGRAL CP CVs WG
USA
5
Japan
1
Czech Republic 4
Great Britain
1
Slovakia
3
Germany
1
Russia
3
India
1
Ukraine
2
Spain
2
South Africa
1
France
1
Australia
1
Strengths: access to large telescopes,
access to XMM data, access to
databases (Compton, ...), access to
robotic telescopes, theory &
observations
New members welcome,
rhudec@asu.cas.cz
What we do/plan to do in CVs
•Analyses of CVs in the CP (GPS): OMC, JEM X, IBIS
•Analyses of CVs in the AO FOVs
•AO-3 proposal ToO of CVs in outburst
•complex analyses: INTEGRAL & other data
15 - 40 keV
40 - 100 keV
The field of the diskless intermediate polar V 2400 Oph and
the symbiotic star V 2116 Oph. Co-added frames obtained
by IBIS (247000 sec exp. (~69 hr) were used. The size of the
field is 9.1ox7.1o. North is up, East to the left. V 2400 Oph is
clearly detected only in the 15-40 keV passband.
The field of the intermediate polar V 1223 Sgr. Co-added
frames from the IBIS instrument in the 15 - 40 keV passband
(16481 sec exp. (4 hr 35 min)) were used. The size of the
field is 9.1ox7.1o. North is up, East to the left.
Optical photometry, V filter,
with OMC
Blazars & AGN unification
Blazar
Quasar
Radio galaxy
obscuring
torus
BLR
Seyfert 2
AD
BH
NLR
Seyfert 1
jet
Blazars & their powerful jet
Jet (within ~10% AGN).
Beam of energetic
particles and magnetic
field moving close to the
speed of light
I
Supermassive black hole
with accretion disc
Line of sight
• Effects of the jet:
• Relativistic beaming
Blazar observer
• Superluminal motion
• Featureless continuum
• Gamma rays
• Rapid variability
• High luminosity
Blazars & Integral
Seven blazars identified in galactic scans of
Integral
1ES 0647+250 ”A secret object”
PKS 0823-223 no gamma from EGRET, grav. lensing candidate
1ES 2344+514 TeV gamma ray source, very close
8C 0149+710 BL Lac candidate?
4C 47.08 ”A secret object”
87GB 02109+5130 poorly understood blazar, TeV candidate
BL Lac The prototype 
Working Group in construction: Hudec,
Munz, Sillanpaa, Basta, Hroch,
Kurtanidze, ...
Blazar NRAO530
in outburst ... end
of Feb 2004
discovered by
INTEGRAL, IBIS
telescope, during
GPS
another blazar in
GPS but V=19.5
The Czech Integral Team
Astronomical Institute of the Academy of Sciences of the Czech
Republic Ondrejov Hudec, Polášek, Šimon, Nekola, Jelínek,
Hudcová, Štrobl, Hroch, Polcar, Topinka, Bašta, Kubánek plus
spolupracující studenti, Michnovic, Švéda, Krolupper Czech
Technical University, Faculty of Electronic Engineering Praha:
Bernas, Páta, Vítek plus studenti, Masaryk University Brno
Hroch, Polcar, Munz, Sobotka, Sixtová
Interdisciplinary project, extended student participation,
collaboration with Universities
Czech Integral Team:
•groups at ASÚ AV ČR, MU Brno, FEL ČVUT Praha
•CV team: Šimon, Štrobl, Hudec, 19 from abroad...international team lead from
Ondrejov
•GRB team: Topinka, Hroch, Polcar, Hudec, .... part of larger international team
•AGN team: Bašta, Munz, Sillanpaa ..... part of larger international team, focus on
blazars
•BART and BOOTES team: Jelínek & BART team, Nekola, Bernas, Páta, Vítek,
Kubánek, Švéda, Michnovič, Sobotka, Polášek...
•ISDC team: Soldán, Hroch, Munz, Jelínek - ISDC2
•software team: Hudcová, Hroch, Polcar, Páta, Nekola, Bernas, Vítek, Krolupper
Our students at the 1st INTEGRAL Progress Meeting, Senohraby,
October 2002
Hudec, Hrudková, Šmída, Hroch, Polcar, Bašta, Topinka, Jelínek,
Štrobl, Stoklasová, Nekola, Kubánek
2nd INTEGRAL&BART Progress Meeting, Kostelní
Střímelice, Oct 2003
Prof. A. Parmar, ESA: "The contributions
from scientists in the Czech Republic to the
OMC and ISDC consortia has been very
successful and is much appreciated by
ESA. We look forward to similar cooperation on XEUS and other missions!"
INTEGRAL Day 2003, Prague, Academy of Sciences of
the Czech Republic, May 27
INTEGRAL future:
•lifetime ~ 15 years, smooth operation
•Czech Participation: Decision of ESA PECS Program
Commitee: prolongation approved for 4 years starting
January 2005 - final approval by the Czech Ministry of
Education still needed
•Continued ISDC participation, ISDC2 operations, OMC
data analyses, science
The End