The Konus-FG experiment for gamma-ray burst studies in GAMMA-400

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The Konus-FG experiment for gamma-ray burst
studies in GAMMA-400

• M.V. Ulanov, R.L. Aptekar, D.D. Frederiks,
• S.V. Golenetskii, E.P. Mazets, and V.D. Palshin

Ioffe Physical-Technical Institute, St.
Petersburg, Russia
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Historical remarks

• GRB research experiments
• KONUS / Venera 1114 (19791983)
• KONUS-WIND (1994present time)
• CORONAS-I, CORONAS-F, CORONAS-PHOTON (20012009)
• Autonomous localization
• GRANAT (1989)
• KONUS-A / Cosmos-2326, 2367, 2421 (19952008)

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Joint Russian-American Konus-Wind experiment
WIND orbit
WIND 1994present time
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Konus-Wind GRB Experiment

• Two detectors S1 and S2 (NaI(Tl) 13cm diameter,
  7.5cm height, Be entrance window). Placed on
  opposite faces of the spacecraft, observing the
  south and north ecliptic hemispheres of the sky.
• Background mode G1 (2080 keV), G2 (80300 keV),
  G3 (3001200 keV) with time resolution 1.472.94
  sec.
• Burst mode time resolution 2ms256ms, energy
  spectra (20keV15MeV).

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Scientific goals of the Konus-FG experiment

• Detection and prompt (12 sec) localization of
  GRB sources in 10 keV 3 MeV energy range with
  accuracy of 0.53.
• Localization information can be used for
  GAMMA-400 pointing to burst source or for further
  data analysis.
• Study of temporal and spectral properties in 10
  keV 15 MeV range with two high-sensitive
  spectrometers.

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Schematic diagram of the Konus-FG instrument
Localization array of four detectors with
anisotropic sensitivity
Spectrometers
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Konus-FG-DN localization units
 
 

• The localization subsystem is formed by four
  identical detectors Konus-FG-DN, registering
  photons in 10700 keV range.
• The detectors anisotropic angular sensitivity
  is proportional to the cosine of the angle of
  incidence and is formed in the soft part of
  spectrum 40160 keV.
• The axes of the DNs are offset from the symmetry
  axis by 30 and separated in azimuth by 90.
• Field of view of each detector (2p sr) should
  not be occulted by construction details of the
  telescope.
• The system provides burst localization in upper
  hemisphere within detectors field of view (75
  of 2p sr) that exceeds the effective angular
  aperture of the telescope.

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Konus-FG-DS spectrometry units

• The spectrometric subsystem includes two
  identical wide directional spectrometry detectors
  Konus-FG-DS operating in 10keV15MeV energy
  range.
• The axis of the detectors should be pointed
  parallel to the main spacecraft axis that
  provides the survey of the whole celestial sphere
  4p sr.
• DS detectors obtain detailed information about
  energy spectra and time history of bursts.
• Konus-FG-DS will be a valuable part of
  triangulation network (IPN), which will improve
  the reliability and accuracy of automatic
  localization.

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Location of Konus-FG units (preliminary)
Konus-FG-DN
Konus-FG-DS
Konus-FG-DN
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The Konus-FG-DS detector unit
The main parts of the detector 1 NaI(Tl)
crystal 5 in diameter by 3 in height, 2
beryllium entrance window, 4 lead glass, 6
photomultiplier, 12, 13, 14 electronic boards.
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The Konus-FG-DN detector unit
The main parts of the detector 1 NaI(Tl)
crystal 5 in diameter by 1 in height, 2
beryllium entrance window, 3 lead shield, 4
lead glass, 6 photomultiplier, 12, 13, 14
electronic boards.
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Konus-A / Cosmos 2326, 2367Localization detector
prototype

• Each detector had 130 mm in diameter and 30 mm in
  height with the passive shielding on lateral
  side.
• The axes of detectors are offset from symmetry
  axis by 30 and separated in azimuth by 90 .
• The accuracy of localization is of 0.5 to 23
  angular degrees depending on the burst intensity.
  

R.L.Aptekar et al. ApJ 1998, 493, 404-407
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Unsolved problems

• Arrangement the optimal location of Konus-FG
  detectors on the GAMMA-400 spacecraft.

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Broadband observations of the naked-eye
gamma-ray burst GRB080319B
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The ultra-luminous GRB110918A
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Konus-Wind and Helicon (CORONAS-F) simultaneous
observations of giant flare from SGR1806-20 on
December 27, 2004
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Konus-Wind and Helicon (CORONAS-F) simultaneous
observations of giant flare from SGR1806-20 on
December 27, 2004
The full isotropic energy release Q2,3?1046 erg
and the peak luminosity L3,5?1047 ??? ?-1
(Frederiks et al., Astronomy Lett., 2007)