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HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903

HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903. Liang Jau-shian Institute of Physics, NTHU. Introduction The Vela satellites. The discovery of GRB was published in the year 1973. IPN (Interplanetary Network). 1980s

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HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903

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  1. HETE- 2OBSERVATIONS OF THE EXTREMELYSOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU

  2. Introduction The Vela satellites • The discovery of GRB was published in the year 1973.

  3. IPN (Interplanetary Network) • 1980s • Helios 2, Pioneer Venus Orbiter, International Sun-Earth Explorer, Venera 11, Venera 12, the Earth orbiter Prognoz 7

  4. The Compton Gamma-Ray Observatory • April 1991 • The Burst and Transient Source Experiment (BATSE) (10keV ~ MeV)

  5. Observational properties • GRB light curves

  6. Durations

  7. Classes of Bursts duration/fluence/spectrum • Long/bright/soft bursts (59%) • Short/faint/hard bursts (23%) • Intermediate (2-5 s)/intermediate/soft busts (18%)

  8. GRB energy spectra • Range: 1keV-18GeV

  9. The Band function Epeak is the energy of the peak of Spectrum.

  10. XRF • no gamma ray counterpart • The XRF spectra are also well described by the Band function.

  11. X-ray rich GRB : Epeak < 50keV • XRF : Epeak at a few keV

  12. XRF 020903 Observations • HETE-2 • the French Gamma Telescope (FREGATE) • the wide-field X-ray monitor (WXM) • the soft X-ray cameras (SXC)

  13. French Gamma Telescope

  14. Wide Field X-ray Monitor

  15. Soft X-ray Camera

  16. Temporal properties • Two peaks: 2-5 and 5-10 keV • No significant flux above 10 keV • The duration of the burst is longer in the lower energy band.  this trend is similar to long bright GRBs.

  17. Spectrum

  18. The constrained Band function method Result: • Best-fit value Epeak = 2.7 keV • 1.1 keV < Epeak < 3.6keV with 68% probability • Epeak < 5.0 keV with 99.7% probability

  19. Discussion • XRF 020903 is an XRF and not a type I X-ray burst • The observes spectrum of XRF 020903 were not the redshifted spectrum of a typical GRB. • The properties of XRF 020903 are consistent with the relation between S7-30 and S30-400 found by Barraud et al.(2003) • Figures 6-8 provide evidence that XRFs, X-ray rich GRBs, and GRBs from a continuum and are therefore the same phenomenon.

  20. Thank you

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