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HETE-II Catalogue

Burst statistics in. HETE-II Catalogue. Filip M ü nz, Elisabetta Maiorano and Graziella Pizzichini for HETE team. High Energy Transient Experiment – II. very small scale mission mass: 123 kg size: 89 x 66 cm (launch size).

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HETE-II Catalogue

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  1. Burst statistics in HETE-II Catalogue Filip Münz, Elisabetta Maiorano and Graziella Pizzichini for HETE team

  2. High Energy Transient Experiment – II very small scale mission mass: 123 kg size: 89 x 66 cm (launch size) • gamma-ray detectorFrench Gamma-ray Telescope (FREGATE): 5-400 keV; ~π FOVno localization • position sensitive instrumentsWide-Field X-ray Monitor (WXM): 2-25 keV; ~5’-10’ localizationsSoft X-ray Cameras (SXC): 2-10 keV; ~40” localizationssmall eff. surface / sensitivity • direct alert transmission through simple VHF stations along the equatorial trajectory Pisa, May 2009

  3. Detector response • FREGATE • large FoV implies high background (with Earth occultation of sources due to fixed pointing ) • WXM • extension to lower energies with complicated response matrix (1-D coded masks) • 1292 GCN alerts • 173 bursts • 143 localized • (110 within 1 hour) Pisa, May 2009

  4. GRB – SN connection (030329A) HETE Highlights first short burst OT (050709) HETE X-ray (Chandra) optical Pisa, May 2009

  5. Catalog content 284 bursts (some cancelled later) results of analysis of different groups more concerning position reconstruction Pisa, May 2009

  6. Checking the catalogue • correlation of different variables (160 entries) • looking for outliers Pisa, May 2009

  7. All links on one page to general catalogue to GCN notices to literature custom notes GRB entry Pisa, May 2009

  8. Band (X/gamma) Peak (times,fluence) GCN notices Afterglow measures Position info Catalogue structure Spectral fits • Database (mySQL) with object interface (and web replication ) • Numerical Python, Django, JQuery • light-curve profiles in ASCII/FITS • procedures to load and subtract background Burst (trigger info) Alert (time of distribution) Literature refer. Pisa, May 2009

  9. Afterglows • Many bursts have good coverage of optical afterglows • Combining with analysis of prompt lightcurves Pisa, May 2009

  10. Success of followups (until 2007) The anti-solar HETE pointing was friendly for ground observers and the frequency of GRB alerts was lower at the time of HETE detections. Pisa, May 2009

  11. HETE-2 Observations of GRB021211 Crew et al. (2003) first HETE localization after 33 sec., OT reported by Fox & Price (GCN 1731) after 53’17”. Pisa, May 2009

  12. GRB021211: Afterglow Light Curve Relative to Those of Other GRBs The optical afterglow of some bursts is much fainter (~ 3 mag) than those previously observed: without HETE’s prompt localization, this GRB would very likely have been listed as “dark”, instead of “dim”. But it proves that at t < 10 min even “dim” afterglows may be bright (m ~ 13). This was very promising for Swift. Pisa, May 2009

  13. Amati relation revisited Amati relation extended to X-Ray Rich GRBs and to X-Ray Flashes Amati relation extended to X-Ray Rich GRBs and to X-Ray Flashes Pisa, May 2009

  14. Lightcurve analysis • trying to extract information besides T90/fluence • developing methods for identification of peaks • need for sampling independent parameters Pisa, May 2009

  15. Lightcurve parade Pisa, May 2009

  16. Work in progress • make catalogue ready for public • checking outliers • linking the literature • polishing the interface • prompt emission studies • more detailed statistics • comparison with other datasets (BATSE, Swift) • need for robust peak-analysis technique • better pseudo-redshift indicator Pisa, May 2009

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