ESA INTEGRAL satellite

... and Czech Participation

3rd INTEGRAL/BART

Workshop Chocerady

2.11.20041. astrophysics ESA satellite with Czech participation

• 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.

The INTEGRAL The INTEGRAL MissionMission

INTEGRAL under Thermal Vacuum testing at ESTEC

Integral ISWGIntegral 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

Perigee: 9,000 km, Apogee: 150,000 km

4.1 tonnes

5 m high, 3.7 m diameter

16 m solar panels

INTEGRAL in a Nutshell

The INTEGRAL instruments

SPI – The gamma-ray Spectrometer on INTEGRAL. Excellent spectra, good images

Jem-X - The Joint European X-ray Monitor

IBIS – The gamma-ray Imager onboard the INTEGRAL satellite. Excellent Imaging, good spectra

OMC – Optical Monitor Camera.

Instrument Principal Investigators Collaboration

IBISP. Ubertini (I), F. Lebrun (F), G. Di Cocco (I)

Italy, France, Norway, Germany, Spain, USA, Poland, UK

SPIJ.-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 Data Centre

T. Courvoisier (CH)Switzerland, France, Germany, Italy, Denmark, UK, Belgium, USA, Czech Republic, Poland

The complex INTEGRAL instruments were built by large collaborations…

Imager on-board the INTEGRAL Imager on-board the INTEGRAL satellite (IBIS)satellite (IBIS)

IBIS detector unit being integrated onto the spacecraft in November 2001

• 15 keV – 10 MeV energy 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.

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)Spectrometer on INTEGRAL (SPI)

SPI detector plane (FM)

• 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 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-viewINTEGRAL 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

ISDC - members of the consortium

Integral multispectral imaging: BH candidate Cyg X-1

Integral exposure map with main sources labeled

IBIS team

Mosaic of 11 pointings (24200 sec), IBIS/ISGRI, 15-40 keV

GPS scan (29 Jan 2003) Dl = 270GPS scan (29 Jan 2003) Dl = 270oo – 337 – 337oo

4U 1630-47, BHC

First TOO follow-up observation (PI: J. Tomsick) on 1 & 2 Feb 2003, 300 ksec

IGR J16318-4848IGR J16318-4848

First new (transient) source detected by INTEGRAL (IBIS/ISGRI) during GPS First new (transient) source detected by INTEGRAL (IBIS/ISGRI) during GPS at Jan 29.271 UT (IAUC # 8063).at Jan 29.271 UT (IAUC # 8063).

LMX region

LMX X-3 and LMC X-4

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 X-3, 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

Fotometrický snímek (střed 10.12, 45.12, otočení 10.0)

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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 dataCore 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, astro-ph/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"

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

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 participationOMC 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

CVs can be sources of radio ... TeV gamma rays like blazars

Cataclysmic Variables/WD Binaries in Cataclysmic Variables/WD Binaries in the INTEGRAL Core Programmethe INTEGRAL Core Programme

Optical light curve

X-ray light curve

X-ray spectrum

GK Per

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

The field of the diskless intermediate polar The field of the diskless intermediate polar V 2400 OphV 2400 Oph and and the symbiotic star the symbiotic star V 2116 OphV 2116 Oph. Co-added frames obtained . Co-added frames obtained by by IBISIBIS (247000 sec exp. (247000 sec exp. (~69 hr (~69 hr) were used) were used.. The size of the The size of the field is 9.1field is 9.1oox7.1x7.1oo. North is up, East to the left. V 2400 Oph is . North is up, East to the left. V 2400 Oph is clearly detected only in the 15-40 keV passband.clearly detected only in the 15-40 keV passband.

1515 -- 40 keV40 keV 4040 -- 100 keV100 keV

The field of the intermediate polar The field of the intermediate polar V 1223 SgrV 1223 Sgr. Co-added . Co-added frames from the frames from the IBISIBIS instrument in the 15 instrument in the 15 -- 40 keV passband 40 keV passband (16481 sec exp.(16481 sec exp. (4 hr 35 min (4 hr 35 min)))) were used. The size of the were used. The size of the field is 9.1field is 9.1oox7.1x7.1oo. North is up, East to the left.. North is up, East to the left.

Optical photometry, V filter, with OMC

Blazars & AGN unification

BlazarQuasar

Radio galaxy

Seyfert 2

Seyfert 1

jet

obscuring torus

NLR

BLR

BH

AD

Blazars & their powerful jet I

Line of sight• Effects of the jet:• Relativistic beaming• Superluminal motion• Featureless continuum• Gamma rays• Rapid variability• High luminosityBlazar observer

Supermassive black holewith accretion disc

Jet (within ~10% AGN). Beam of energetic

particles and magnetic field moving close to the

speed of light

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 candidate1ES 2344+514 TeV gamma ray source, very close8C 0149+710 BL Lac candidate?4C 47.08 ”A secret object”87GB 02109+5130 poorly understood blazar, TeV candidateBL 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

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

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 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 EndThe End