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ESA INTEGRAL satellite

ESA INTEGRAL satellite. ... and Czech Participation 3rd INTEGRAL/BART Workshop Chocerady 2.11.2004. 1. astro physics ESA satellite with Czech participation. The INTEGRAL Mission. Gamma-ray observatory with concurrent X-ray and optical monitoring.

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ESA INTEGRAL satellite

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

  2. 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

  3. Integral ISWG The INTEGRAL FM and the ISWT @ ESTEC, 26 March 2002

  4. 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

  5. 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

  6. 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 INTEGRAL instruments

  7. The complex INTEGRAL instruments were built by large collaborations…

  8. Imager on-board the INTEGRAL satellite (IBIS) • 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. IBIS detector unit being integrated onto the spacecraft in November 2001

  9. 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.

  10. 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

  11. 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

  12. 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) : 2106 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

  13. 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

  14. 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

  15. Integral multispectral imaging: BH candidate Cyg X-1

  16. Integral exposure map with main sources labeled

  17. Mosaic of 11 pointings (24200 sec), IBIS/ISGRI, 15-40 keV 4U 1630-47, BHC First TOO follow-up observation (PI: J. Tomsick) on 1 & 2 Feb 2003, 300 ksec IBIS team IGR J16318-4848First new (transient) source detected by INTEGRAL (IBIS/ISGRI) during GPS at Jan 29.271 UT (IAUC # 8063). GPS scan (29 Jan 2003) Dl = 270o – 337o

  18. LMX region LMX X-3 and LMC X-4 JEM-X image

  19. Cyg region by ISGRI/IBIS 15-40 keV

  20. The First Gamma-ray Burst observed by INTEGRAL

  21. 1905+105, microquasar and BH candidate, time variability by Jem X, AO-1 pointing

  22. Pulses of Crab pulsar in various energy ranges, IBIS

  23. Multi instrument spectra of Cyg X-3, JEM X, ISGRI, SPI

  24. First OMC image from space

  25. 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

  26. Selection of objects in photometric shot

  27. 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

  28. Cyg X-1 optical image by OMC Test variable star: testing performance of OMC and s/w

  29. Eclipsing binary Y Sex , OMC LC

  30. 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

  31. 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.

  32. 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

  33. 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.

  34. 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

  35. Galactic Scans Data source of the Core Programme CVs, blazars

  36. 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

  37. 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.

  38. 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).

  39. 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.

  40. 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

  41. 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

  42. 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

  43. Secondary INTEGRAL Science and Data Centre, Ondřejov

  44. 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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