Jos Mara Castro Cern1 Alberto J' CastroTirado2,3 Jan Soldn4 Ren Hudec4 Martin Bernas5 Petr Pta5 Toms

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ESA INTEGRAL satellite
... and Czech Participation 3rd
INTEGRAL/BART Workshop Chocerady 2.11.2004
1. astrophysics ESA satellite with Czech
participation
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The INTEGRAL Mission

• Gamma-ray observatory with concurrent X-ray and
  optical monitoring.
• INTEGRAL is the ESA Science Programmes mission
  launched on October 17, 2002.
• ESAs 2nd ?-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
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Integral ISWG
The INTEGRAL FM and the ISWT _at_ ESTEC, 26 March
2002
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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
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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
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The INTEGRAL instruments
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The complex INTEGRAL instruments were built by
large collaborations
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Imager on-board the INTEGRAL satellite (IBIS)

• 15 keV 10 MeV energy range
• 16384 CdTe (ISGRI) and 4096 CsI (PICsIT)
  detectors. E/?E 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.

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.
IBIS detector unit being integrated onto the
spacecraft in November 2001
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Spectrometer on INTEGRAL (SPI)

• Fine spectroscopy of narrow lines and the study
  of diffuse emission on gt degree scales.
• 20 keV to 8 MeV energy range
• 19 cooled (90o K) Ge detectors. E/?E 500.
• 16 degree fully coded FOV with 2.5 degree FWHM
  imaging resolution. Location accuracy lt1.3
  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.
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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
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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

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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
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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

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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
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Integral multispectral imaging BH candidate Cyg
X-1
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Integral exposure map with main sources labeled
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GPS scan (29 Jan 2003) Dl 270o 337o
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LMX region LMX X-3 and LMC X-4 JEM-X image
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Cyg region by ISGRI/IBIS 15-40 keV
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The First Gamma-ray Burst observed by INTEGRAL
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1905105, microquasar and BH candidate, time
variability by Jem X, AO-1 pointing
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Pulses of Crab pulsar in various energy ranges,
IBIS
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Multi instrument spectra of Cyg X-3, JEM X,
ISGRI, SPI
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First OMC image from space
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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
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Selection of objects in photometric shot
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First OMC image from space .... after running the
OMC Pointing Software developed by Vera Hudcová
with help of Filip Hroch and Jirí Polcar at HEA
Group, Astronomical Institute Ondrejov
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Cyg X-1 optical image by OMC
Test variable star testing performance of OMC
and s/w
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Eclipsing binary Y Sex , OMC LC
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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
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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.
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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
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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 gt 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.
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• 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

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Galactic Scans Data source of the Core
Programme CVs, blazars
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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
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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.
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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,
astro-ph/0401643). However, the high energy image
shows that only GX 33700 (a black hole
candidate) emits above 100 keV. GX 33700 shows
many chararacteristics of galactic microquasars
(radio jets, QPO, and X-ray behaviour).
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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.
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GRB030501 "Labor Day GRB" 1st "Czech" lead
analyse GRB observed by INTEGRAL (according to
negotiated rotation of responsibilities of
instrumental teams)
SPI image
Real-time localization by IBIS and IBAS alert
response
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• 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

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• 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

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Secondary INTEGRAL Science and Data Centre,
Ondrejov
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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

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Cataclysmic Variables/WD Binaries in the INTEGRAL
Core Programme
CVs can be sources of radio ... TeV gamma rays
like blazars
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Optical light curve
GK Per
X-ray spectrum
X-ray light curve
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• 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

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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_at_asu.cas.cz
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• 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

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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.
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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.
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Optical photometry, V filter, with OMC
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Blazars AGN unification
Blazar
Quasar
Radio galaxy
obscuring torus
BLR
Seyfert 2
AD
BH
NLR
Seyfert 1
jet
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Blazars their powerful jet I
Supermassive black hole with accretion disc
Jet (within 10 AGN). Beam of energetic
particles and magnetic field moving close to the
speed of light

• Effects of the jet
• Relativistic beaming
• Superluminal motion
• Featureless continuum
• Gamma rays
• Rapid variability
• High luminosity

Line of sight
Blazar observer
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Blazars Integral
Seven blazars identified in galactic scans of
Integral 1ES 0647250 A secret object PKS
0823-223 no gamma from EGRET, grav. lensing
candidate 1ES 2344514 TeV gamma ray source, very
close 8C 0149710 BL Lac candidate? 4C 47.08 A
secret object 87GB 021095130 poorly understood
blazar, TeV candidate BL Lac The prototype ?
Working Group in construction Hudec, Munz,
Sillanpaa, Basta, Hroch, Kurtanidze, ...
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Blazar NRAO530 in outburst ... end of Feb
2004 discovered by INTEGRAL, IBIS telescope,
during GPS another blazar in GPS but V19.5
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The Czech Integral Team Astronomical
Institute of the Academy of Sciences of the Czech
Republic Ondrejov Hudec, Poláek, imon, Nekola,
Jelínek, Hudcová, trobl, Hroch, Polcar, Topinka,
Bata, Kubánek plus spolupracující studenti,
Michnovic, véda, 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
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• Czech Integral Team
• groups at ASÚ AV CR, MU Brno, FEL CVUT Praha
• CV team imon, trobl, Hudec, 19 from
  abroad...international team lead from Ondrejov
• GRB team Topinka, Hroch, Polcar, Hudec, ....
  part of larger international team
• AGN team Bata, Munz, Sillanpaa ..... part of
  larger international team, focus on blazars
• BART and BOOTES team Jelínek BART team,
  Nekola, Bernas, Páta, Vítek, Kubánek, véda,
  Michnovic, Sobotka, Poláek...
• ISDC team Soldán, Hroch, Munz, Jelínek - ISDC2
• software team Hudcová, Hroch, Polcar, Páta,
  Nekola, Bernas, Vítek, Krolupper

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Our students at the 1st INTEGRAL Progress
Meeting, Senohraby, October 2002 Hudec, Hrudková,
mída, Hroch, Polcar, Bata, Topinka, Jelínek,
trobl, Stoklasová, Nekola, Kubánek
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2nd INTEGRALBART Progress Meeting, Kostelní
Strímelice, Oct 2003
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• 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 co-operation on XEUS and other missions!"

INTEGRAL Day 2003, Prague, Academy of Sciences of
the Czech Republic, May 27
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• 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

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The End