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ESTREMO/WFXRT Field Monitor Thinkshop Summary

This summary from the August Thinkshop in Rome discusses the minimum requirements and additional needs for the Wide Field Monitor (WFI) localizator in studying GRBs. The presentation covers hardware constraints, proposed designs for the WFI, and two options for configurations. Option (a) focuses on prompt emission and hard X-ray transients, while option (b) offers cost-effective solutions for prompt emission studies. The workshop also outlines the specifications for each option, including pixel sizes, energy ranges, geometric areas, sensitivities, and power requirements. This summary emphasizes the importance of meeting the scientific requirements for accurate and efficient monitoring of GRBs.

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ESTREMO/WFXRT Field Monitor Thinkshop Summary

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  1. The Wide Field Monitorfor ESTREMO/WFXRT: A Summary of the 2-3 August Thinkshop Marco Feroci IASF/INAF – Rome ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  2. (Very) Minimum (baseline) requirements for WFI(*) Requirements for the localizator are: • Flux: rather bright events (>1 Crab) • Energy range: need to go down to at least 4 keV. Upper range: not a driver for localization (but see below), 40 keV should be good enough. • FOV > 3-4 sr • Localization (driven by NFI): better than 3 arcmin • Need to have at least the temporal signature in the hard X-ray range (>100 keV) to identify a GRB (*) Presentation by L. Piro ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  3. Additional Requirements for WFI: Study of the prompt emission of GRBs See L. Amati ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  4. Gross Hardware Constraints(*) Mass: 150 kg, including cont.y Power: 120 W, including cont.y Volume: 70 cm height, Vega fairing (220 cm) symmetric Telemetry: few Mbit/s (X-band) (*) Presentation by L.Piro ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  5. Designs Proposed for WFM • ISGRI/BAT-like configuration, with optical design and detector technology to be assessed (+open field det.) • Improved SuperAGILE technology, plus “classical” open-field spectroscopy detector Both options satisfy the baseline scientific requirements. Option (a) offers better performance for the study of the prompt emission of GRBs and (Hard) X-ray transients, simultaneously over half sky: probably unprecedented. high quality ASM science Option (b) requires smaller budgets (factor of 2-3) but provides coarser spectral info on prompt emission. Soft X-rays (~1-5 keV) probably require SDD in both options. Fine determination of spectral parameters requires area or small FOV for the spectroscopy detector. ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  6. Option (a) (baseline) • 2D pixellated detector – pixel size 2-3 mm • Energy range: 1/10 – 200 keV, depending on technology • Detector options: CZT, CdTe, SDD+CsI • Geometric Area: 3700-5000 cm2, depending on solution • Eff. Area: 350 (flat) or 700-2500 cm2(min/max), dep. on solution • 2D Coded Mask • Mask-Detector distance: 400-700 cm, depending on solution • FOV: 3-6 sr, to be optimized • Angular Resolution: 30-40 arcmin • Point Source Location Accuracy: 2-3 arcmin • Sensitivity (1s): 0.5-5 Crab, to be optimized • Weight: 150 kg • Power: 120 W ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  7. Option (b) (back-up) • Detector: 1D microstrip – pixel size 120 m • Energy range: 3-5 – 50 keV, depending on ASIC technology • Detector options: Silicon,1-2 mm thick, single/double-sided • Geometric Area: 5000 cm2 • Eff. Area: 100/200 cm2 (any direction), dep. on solution • 1D/2D Coded Mask • Mask-Detector distance: 15 cm • FOV: 6 sr, to be optimized • Angular Resolution: 6 arcmin • Point Source Location Accuracy: 1-2 arcmin • Sensitivity (1s): 1 Crab, to be optimized • Weight: 30-50 kg • Power: 50 W ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  8. Summary of Solutions ESTREMO/WFXRT Workshop Rome 12-13 September 2006

  9. Summary of Summaries • Arcmin Localization of bright bursts (say, 50 events/year) in 10-100 keV “easily” reachable • Good low energy (<5-7 keV) sensitivity requires R&D or dedicated detector • Good high energy (>200 keV) spectral sensitivity may require dedicated detector • Good spectral response on wide energy range (fine determination of spectral parameters) may require trade-off on the area/FOV. Different optimization wrt point (1) Need A Clear Assessment of Scientific Requirements ESTREMO/WFXRT Workshop Rome 12-13 September 2006

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