The wide field monitor for estremo wfxrt a summary of the 2 3 august thinkshop
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The Wide Field Monitor for ESTREMO/WFXRT: A Summary of the 2-3 August Thinkshop. Marco Feroci IASF/ INAF – Rome. (Very) Minimum (baseline) requirements for WFI (*). Requirements for the localizator are: Flux: rather bright events (>1 Crab)

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The Wide Field Monitor for ESTREMO/WFXRT: A Summary of the 2-3 August Thinkshop

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The wide field monitor for estremo wfxrt a summary of the 2 3 august thinkshop

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


Very minimum baseline requirements for wfi

(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


Additional requirements for wfi study of the prompt emission of grbs

Additional Requirements for WFI: Study of the prompt emission of GRBs

See L. Amati

ESTREMO/WFXRT Workshop

Rome 12-13 September 2006


Gross hardware constraints

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


Designs proposed for wfm

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


Option a baseline

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


Option b back up

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


Summary of solutions

Summary of Solutions

ESTREMO/WFXRT Workshop

Rome 12-13 September 2006


Summary of summaries

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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