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

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Presentation transcript:

HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 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 Helios 2, Pioneer Venus Orbiter, International Sun-Earth Explorer, Venera 11, Venera 12, the Earth orbiter Prognoz 7

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

Observational properties GRB light curves

Durations

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

GRB energy spectra Range: 1keV-18GeV

The Band function E peak is the energy of the peak of Spectrum.

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

X-ray rich GRB : E peak < 50keV XRF : E peak at a few keV

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

French Gamma Telescope

Wide Field X-ray Monitor

Soft X-ray Camera

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.

Spectrum

The constrained Band function method Result: Best-fit value E peak = 2.7 keV 1.1 keV < E peak < 3.6keV with 68% probability E peak < 5.0 keV with 99.7% probability

Discussion XRF is an XRF and not a type I X-ray burst The observes spectrum of XRF were not the redshifted spectrum of a typical GRB. The properties of XRF are consistent with the relation between S 7-30 and S 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.

Thank you