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C H A P T E R 8

C H A P T E R 8. RESPIRATORY REGULATION DURING EXERCISE. w Discover how your respiratory system regulates your breathing and gas exchange. (continued). Learning Objectives.

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C H A P T E R 8

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  1. INTEGRAL衛星の初期成果 海老沢　研 INTEGRAL Science Data Center Versoix, Switzerland

  2. Contents • Introduction of the satellite • Introduction of the instruments • Status and performance of the instruments • Early scientific results • Current problems • Prospects for future

  3. INTEGRAL satellite • Launched on Oct 17, 2002 by Russian Proton rocket • Covers 3 keV to ~10 MeV with three coded mask instruments • Hard X-ray/gamm-ray imaging • Gamma-ray spectroscopy

  4. INTEGRAL Orbit • High eccentric orbit, 72 hour period • Inclination 51.6° • Perigee ~9,000 km, apogee ~150,000 km • Two ground stations • Goldstone (California) • Redu (Belgium) • REAL TIME OPERATION • Gamma-ray burst monitor!

  5. INTEGRAL Detectors JEMX masks IBIS mask SPI IBIS detector JEMXdetectors

  6. ISGRI (CdTe) PICSIT(CsI) IBIS(Imager on Board the Integral Satellite) • Full imaging capability • FWHM~12 arcmin Centroid accuracy ~arcmin • ISGRI (20-200 keV) 128x128 CdTe pixels Moderate energy resolution (~9%@100 keV) • PICSIT (100-6000 keV) 64x64 CsI pixels

  7. Anti Coincidence Sensor (ACS) GBD minotor! Spectrometer SPI • Coded mask and 19 Ge detectors • Stirling cryocooler • Limited imaging capability(19 “pixels”) • BGO anti-coincidence detectors • High energy resolution ~2.2 keV@662 keV • Energy range 15 keV to 8 MeV

  8. X-ray monitor JEMX • Two identical detectors • Imaging micro-strip gas chambers(90% Xenon + 10 % Methane) • Energy range 3-35 keV • ~30’’ angular resolution

  9. INTEGRAL prelaunch movie

  10. IBIS on-board sensitivity 3s, 105 sec exposure Ubertini et al.(2003) ISGRI PICSIT Based on measured BGD, only statistical errors taken into account “Ultimate sensitivity” ~1mCrab @ 20-100 keV PICIST sources:Crab and Cyg X-1, GRB only?

  11. SPI on-board sensitivity Roques et al. (2003) 10 mcrab 3s, 106 sec 1 mcrab SPI point source sensitivity is limited by confusion (~0.5 deg)

  12. JEMX on-board sensitivity Brandt et al. (2003) Sensitivity limited by systematics Ultimate sensitivity ~1mCrab

  13. Detectable sources “INTEGRAL reference catalog” Ebisawa et al. (2003) ~1000 known sources, ever brighter 1mCrab above 2 keV.

  14. Detectable sources • INTEGRAL has a large FOV • Eventually, all the sky will be fully covered • 105 sec exposure over the sky • ~700 sources with JEMX • ~400 sources with ISGRI Ebisawa et al. (2003)

  15. Exposure map from Oct 2002 to Nov 2003 Green> 106 sec Blue >105 sec 3C273 Vela Cyg GC Crab LMC

  16. 2003 2004 AO2 AO1

  17. Projects and targets • Core program • Galactic Center Deep Exposure (GCDE) • Galactic Plane Scan (GPS) • Vela region • TOO observations for transient sources

  18. Projects and targets • Accepted general programs (A and B categories, besides TOO and GRB) AO1AO2 • AGN 16 12 • Galaxy 2 1 • Clusters 1 2 • Galactic diffuse 3 9 • G.C. 2 1 • SNR 3 2 • Binary 10 11 • Pulsar 1 1 • Stars 2 2 • Gamma-ray sources 6 5 • Most AO1 observations completed, data are sent to PIs • Calibration and analysis software getting better…

  19. Early results • Discovery of new sources (from GCDE, GPS) • IAUC, Astronomer’s Telegram • GRB detection • GRB Coordinates Network (GCN) • A&A special issue, 2003, vol 411, no1 • 75 letter papers (28 astrophysical papers) • 5th INTEGRAL meeting in Feb 2004 (Munich) • 244 abstracts submitted (including non-INTEGRAL papers) • Some other publications…

  20. INTEGRAL Sources (http://isdc.unige.ch/~rodrigue/html/igrsources.html) 15 sources till Dec 2003 All transient sources!

  21. IGR J16318-4848(observed @50mCrab with INTEGRAL) Revnivtsev et al. (2003) Walter et al. (2003) ASCA 1994~1mCrab XMM and ISGRI Iron line dominate! Heavily absorbed X-ray binary transients! (probably high mass binaries like GX301-2)

  22. SPI energy spectrum of Cyg X-1 High energy imaging/spectra of binary sources 308 -605 keV 20-50 keV 84 -308 keV SPI image of the Cyg region Moderate resolution (~0.5 deg) imageup to ~600 keV! Bouchet et al. (2003)

  23. Cyg X-1 PCA HEXTE JEMX ISGRI SPI High quality spectra of bright sources from 3 keV to ~1 MeV! Pottschmidt et al. (2003)

  24. Bright X-ray binaries near GC b b l l l b ISGRI 20-40 keV ISGRI 40-60 keV High resolution (~10 arcmin) imaging up to ~100 keV Paizis et al. (2003)

  25. Early results – Gamma-ray bursts • 7 GRBs in the IBIS FOV (till Dec 2003) • Detected with INTEGRAL Burst Alert System (IBAS) • Alerts sent all over the world within ~10 sec • Position accuracy depends on the brightness, down to ~30” • SPI Anti-coincidence Sensor (ACS) alert (no position) ~1/day • sent to GRB Coordinates Network (GCN)

  26. GRBs detected with IBAS 4.4’ in 30sec! Error region and delay Mereghetti et al (2003)

  27. GRB detected with ACS Light curves von Kienlin et al. (2003) Expected from BATSE Duration histogram

  28. GRB energy spectra Malaguti et al. (2003) PICSIT ISGRI Good GRB energy spectra from 20 keV to 500 keV! GRB021125 GRB030501 ISGRI SPI SPI spectrum Spectral variation Beckman et al. (2003)

  29. Extragalactic sources • Many other bright AGNs detected (confirmed with real time Quick Look) Publication? • 3C111 – radio galaxy at z=0.048 (~34 mCrab in the 20-40 keV band in August 2003 (Favre et al.) • Strong flares expected! (e.g. Blazers) • Normal galaxy? Clusters of Galaxies? 3C273 detected, expected spectrum(Courvoisier et al. 2003)

  30. Galactic center Belanger et al. (2003) 40 - 100 keV 20 - 40 keV Hard X-ray point source coincides with Sgr A* Sgr A*? X-ray binary?

  31. Strong et al. (2003) Galactic diffuse emission • Preliminery results • Consitent with previous XTE, OSSE observation • A rumor says… • Contrubution of point sources at ~100 keV dominant than previousestimates? • Not so much Galactic “diffuse” emission at ~100 keV? GC=33deg L=33deg

  32. Galactic center 511 keV line Knodlseder et al. (2003) Symmetric diffuse distribution around GC Annihilation fountain (claimed by OSSE)not confirmed Russian data!

  33. Current problems • Calibration • Background estimation, subtraction • Spectral response • Analysis technique • Currently, deconvolution is made for each pointing (~30 min), deconvolved images and spectra combined • Photons have to be accumulated for longer periods! • Deconvolution at once from many (~1000) pointings • Memory and CPU serious problems… • Data structure, software issues • Unique data structure, incompatibility with widely-used analysis system, difficult to handle “event” data • No good portability of data/software

  34. Future prospects • Detection of more gamma-ray lines expected • SNR, Point sources • Annihilation line from point sources? • Dim sources down to 1 mCrab at >50 keV? • High quality spectra of dim sources up to ~1 MeV • Short transients? • Gamma-ray/X-ray “flush” events • Fast pulsars? • Hard X-ray study of millisecond pulsars

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