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

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

HETE- 2 OBSERVATIONS OF THE EXTREMELY

SOFT X-RAY FLASH XRF 020903

Liang Jau-shianInstitute of Physics, NTHU

Page 2: 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.

Page 3: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

IPN (Interplanetary Network)

• 1980s• Helios 2, Pioneer Venus Orbiter, Intern

ational Sun-Earth Explorer, Venera 11, Venera 12, the Earth orbiter Prognoz 7

Page 4: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

The Compton Gamma-Ray Observatory

• April 1991• The Burst and Transient Source Exper

iment (BATSE) (10keV ~ MeV)

Page 5: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 6: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Observational properties

• GRB light curves

Page 7: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Durations

Page 8: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Classes of Bursts

duration/fluence/spectrum• Long/bright/soft bursts (59%)• Short/faint/hard bursts (23%)• Intermediate (2-5 s)/intermediate/soft

busts (18%)

Page 9: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

GRB energy spectra

• Range: 1keV-18GeV

Page 10: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

The Band function

),exp()100

()(0E

E

keV

EAENE

,)100

)(exp(100

)( 0

keV

E

keV

EA

breakEEE 0)(

breakEEE 0)(

1~

)2( 0

EEpeak Epeak is the energy of the peak ofSpectrum.

F

Page 11: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 12: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

XRF

• no gamma ray counterpart• The XRF spectra are also well

described by the Band function.

Page 13: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

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

Page 14: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

XRF 020903

Observations• HETE-2• the French Gamma Telescope (

FREGATE) • the wide-field X-ray monitor (WXM) • the soft X-ray cameras (SXC)

Page 15: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

French Gamma Telescope

Page 16: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Wide Field X-ray Monitor

Page 17: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Soft X-ray Camera

Page 18: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 19: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Temporal properties

• Two peaks: 2-5 and 5-10 keV• No significant flux above 10 keV• The duration of the burst is longer in t

he lower energy band. this trend is similar to long bright G

RBs.

Page 20: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 21: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 22: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Spectrum

Page 23: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 24: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 25: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 26: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

The constrained Band function method

Result:• Best-fit value Epeak = 2.7 keV• 1.1 keV < Epeak < 3.6keV with 68% prob

ability• Epeak < 5.0 keV with 99.7% probability

Page 27: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 28: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
Page 29: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Discussion• XRF 020903 is an XRF and not a type I X-ray b

urst• 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.

Page 30: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.
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Page 33: HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF 020903 Liang Jau-shian Institute of Physics, NTHU.

Thank you


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