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Dru žice ESA INTEGRAL

Dru žice ESA INTEGRAL. IBWS Vlašim 2006 RH & ASU HEA team. 1. astro physics 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.

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Dru žice ESA INTEGRAL

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  1. Družice ESA INTEGRAL IBWS Vlašim 2006 RH & ASU HEA team 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.

  3. 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

  4. 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

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

  6. 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

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

  8. ESA INTEGRAL • Co-aligned onboard instruments: • gamma-ray imager IBIS (15 keV–10 MeV, • field 9 deg, 12 arc min FWHM) • gamma-ray spectrometer SPI (12 keV– • 8 MeV, field 16 deg) • X-ray monitor JEM-X (3–35 keV, field • 4.8 deg) • optical monitoring camera OMC • (Johnson V-filter, field 5 deg) • Simultaneous information in the optical, medium • X-ray, hard X-ray, and gamma spectral region (or • at least a suitable upper limit) for each CV in • each scan or field. • Modes of observation: • Regular (weekly) Galactic Plane Scans (GPS) • (-14o<bII<+14o) • (b) Pointed observations • (c) Targets of opportunity Fields of view of the individual instruments

  9. 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.

  10. The First Gamma-ray Burst observed by INTEGRAL

  11. 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

  12. Non-magnetic cataclysmic variable (CV) • Accretion disk – thermal • radiation (UV, optical, IR) Donor, lobe-filling star Bright spot (stream impact onto disk) • Opt. thick, geom. thin boundary • layer (therm. rad. - soft X-rays) • (high m) . Mass stream Non-mag. white dwarf • Opt. thin, geom. thick boundary • layer (bremsstrahlung – hard • X-rays) (low m) Accretion disk . Dominant source of luminosity: accretion process Intermediate polar – mildly magnetized white dwarf • Impact region near the • magnetic pole of the WD • (bremsstrahlung – hard • X-rays)

  13. Non-magnetic CVs Radial temperature profile of the disk Dwarf nova Z Cha Thermally unstable disk quiescence Increasing time- averaged mass accretion rate m (also increasing time- averaged luminosity) (Wood et al. 1986) . • flat temperature profile, disk • cool, optically thin Thermally stable disk (most time) outburst (Horne & Cook 1985) • steep temperature profile, • disk hot, optically thick

  14. Magnetic CVs (polars) ST LMi – orbital modulation in hard Xrays (1.9-8.5 keV) (EXOSAT) Mason (1985) hard X-ray sources • cyclotron emission from • accretion column (mainly • optical and UV) • bremsstrahlung from • shocks above impact • region on the WD (X-rays) IBIS AM Her – orbial modulation top – soft X-rays (40-120 A) bottom- hard X-rays (1.9-8.5 keV) (EXOSAT) AM Her (kTbrem~31 keV) (Rothschild et al. 1981) Typical high and low states found by Meinunger and Hudec, 1976 Heise et al. (1985)

  15. 15 – 25 keV 25 – 40 keV V1223 Sgr Field of the intermediate polarV1223 Sgr. Co-addedframes from IBIS. Start exp. JD 2452730.17 Integration time: 66 700 sec Size of the field: 9.1ox7.1o. North is up, East to the left. 40 – 60 keV

  16. GK Per INTEGRAL Interval between outbursts:D t = 973days IBIS obs.: start at ~42percent of this interval (measured since the previous outburst). Ishida’s et al. reference spectrum:Dt = 983days (start at ~29percent of this interval). Amount of matter arriving to the WD and the parameters of the X-ray emitting region on the WD remained almost the same during these phases of the quiescent intervals. Flux(15–40keV)= (2.7 +/- 1.2) x 10-4 photon/cm2/s L (15 – 40 keV) = 4.6 x 1032 erg/s IBIS Quiescent X-ray spectrum Parameters from Ishida et al. (1992) (kT = 32 keV, NH = 1022 cm-2, norm. factor: 0.0039+/-0.0002photon/cm2/s1/keV) IBIS (25–40 keV) image of GK Per(Integr. time: 79 980 sec Co-added images: 19 March 2003, 27 – 29 July 2003. Size of field:4.1ox3.0o. North is up, East to the left.

  17. First OMC image from space

  18. OMC Pointing Software OMC PS developed by V. Hudcova at AI Ondrejov 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

  19. Selection of objects in photometric shot

  20. 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

  21. Blazars & their powerful jets Jet (within ~10% AGN). Beam of energetic particles and magnetic field moving close to the speed of light Supermassive black hole with accretion disc • Effects of the jet: • Relativistic beaming • Superluminal motion • Featureless continuum • Gamma rays • Rapid variability • High luminosity Line of sight Blazar observer

  22. BLLac Violent optical variability of BL Lac on a long time time scale good candidate to be detected at flaring

  23. Historical optical light curve of NRAO530 The source exhibits rare but large amplitude optical flares (Dm~ 4 mag) Optical R band good tracer for the HE activity of blazars (CGRO experience, Collmar (2004)) - gamma flares can be expected

  24. INTEGRAL ToO Observation

  25. The target and the three additional AGNs in the IBIS FOV (30-60 keV)

  26. S5 0836+710 Markarian 6 single power law spectrum G~1.5 single power law spectrum G~1.3

  27. Hints for a break or cutoff in Markarian 3 Broken power law IBIS/ISGRI spectrum Power law with high energy cutoff

  28. INTEGRAL AO-3 ToO observation of 3C454 (z=0.859), preliminary results, L. Foschini et al. ATEL 2005, PI E. Pian @ large collaboration ToO triggered by high optical (T. Balonek, VSNET alert) and X-ray (BAT Swift) activity INTEGRAL observation started May 15, at 18:40 UT, exposure 200 ksec source clearly detected by IBIS/ISGRI in the 20-40 and 40-100 keV energy bands, with a significance of 20 and 15 sigma

  29. Integral observation Optical light curve of 3C454.3 (T. Balonek)

  30. INTEGRAL

  31. INTEGRAL IBIS/ISGRI images, 20-40 (left) and 100-200 keV (right)

  32. Secondary INTEGRAL Science and Data Centre, Ondřejov, Czech Republic • OSA installed and operated, public databases, ... • assistence can be provided to guest astronomers from Central Europe • intensive collaboration with ISDC in Versoix

  33. Our students at the 1st INTEGRAL Progress Meeting, Senohraby, October 2002 Hudec, Hrudková, Šmída, Hroch, Polcar, Bašta, Topinka, Jelínek, Štrobl, Stoklasová, Nekola, Kubánek

  34. 2nd INTEGRAL&BART Progress Meeting, Kostelní Střímelice, Oct 2003

  35. 3rd INTEGRAL/BART Workshop, Chocerady, Nov 1-3, 2004

  36. 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

  37. INTEGRAL future: • lifetime ~ 15 years, smooth operation • Czech Participation: Decision of ESA PECS Program Committee: prolongation approved for 4 years starting January 2005 • Continued ISDC participation, ISDC2 operations, OMC data analyses, science • Participation of young Czechs very much appreciated by ESA

  38. Acknowledgements: This study was supported by the projects ESAPRODEXINTEGRAL14527, ESA PECS INTEGRAL and partly by the grant 205/05/2167 of the Grant Agency of the Czech Republic. We have made use of the visual observations from the AFOEV database operated in Strasbourg, France. We acknowledge using the curve-fitting code HEC13 written by Dr. Harmanec. We thank F. Hroch for the preparation of a mosaic of V2400 Oph and P. Sobotka for a search in the OMC database. The WWZ code by G. Foster is available at URL: www.aavso.org/data/software/wwz.shtml. The code AVE for the period search, developed by the GEA society, is available at URL: www.astrogea.org/soft/ave/aveint.htm.

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