With seven different instruments onboard, Granat was designed to observe the Universe at energies ranging from X-ray to Gamma-Ray. Specific instruments were meant to study Gamma-Ray bursts and other transient X-Ray sources while others were intended to image X-Ray sources near the Galactic Center. One instrument (WATCH) was designed to monitor the sky continuously and alert the other instruments to new or interesting X-Ray sources.
The ART-P and ART-S instruments were both the responsibility of the IKI in Moscow. The ART-P instrument covered the energy range 4-60 keV for imaging and 4-100 keV for spectroscopy and timing. There were 4 identical modules of the ART-P telescope. Each consisted of a position sensitive Multi-Wire Proportional Counter (MWPC) together with a URA coded mask. Each module had an effective area of ~600 cm2. The field of view was 1.8° x 1.8°. The angular resolution was 5 arcmin. The instrument could achieve a 1mCrab sensitivity in an 8 hour exposure. The maximum time resolution was 4 ms. The ART-S instrument covered the energy range 3-100 keV. The field of view was 2° x 2°. The instrument consisted of 4 detectors based on spectroscopic MWPCs. The effective area was 2400 cm2 at 10 keV, 800 cm2 at 100 keV. The time resolution was 200 microseconds.
The PHEBUS experiment was designed by CESR (Toulouse) to record high energy transient events in the range 100 keV - 100 MeV. It consisted of 2 independent detectors with their associated electronics. Each detector consisted of a BGO crystal 78 mm in diameter by 120 mm thick, surrounded by a plastic anti-coincidence jacket. The 2 detectors were arranged on the spacecraft so as to observe ~4-pi steradians. The burst mode was triggered when the count rate in the 0.1-1.5 MeV energy range exceeded the background level by 8 sigma in either 0.25 or 1.0 seconds. There were 116 energy channels.
Four WATCH instruments, designed by the Danish Space Research Institute, were in operation on the Granat observatory starting in January 1990. The instruments could localize bright sources in the 6-180 keV range to within 0.5° using a Rotation Modulation Collimator. Taken together, the 3 fields of view of the instruments covered ~75% of the sky. The energy resolution was 30% FWHM at 60 keV. During quiet periods, count rates in 2 energy bands (6-15 keV, 15-180 keV) were accumulated for 4, 8, or 16 s, depending on memory filling. During a burst or transient event, count rates were accumulated with a time resolution of 1 second into 36 energy channels.
The KONUS-B instrument, designed by the Ioffe Physical-Technical Institute in St. Petersburg, consisted of 7 detectors distributed around the spacecraft. They responded to 10 keV - 8 MeV photons. They consisted of NaI(Tl) scintillator crystals 200 mm in diameter x 50 mm thick, with a Be entrance window. The side surfaces were protected by a 5 mm thick lead layer. The burst detection threshold was 5 x 10-8 - 5 x 10-7 erg/cm2, depending on the burst spectrum and rise time. Spectra were taken in two 31 channel PHAs. The first 8 spectra were measured with 1/16 s time resolution. The remaining spectra had adaptive time resolutions depending on the count rate. The range of resolutions was 0.25 s - 8 s. The KONUS-B instrument operated from 11 December 1989 until 20 February 1990. Over that period, the "on" time for the experiment was 27 days. Some 60 solar flares and 19 cosmic gamma-ray bursts were detected.
The French TOURNESOL instrument consisted of 4 proportional counters and 2 optical detectors. The proportional counters detected 2 keV - 20 MeV photons in a 6° x 6° field of view. The visible detectors had a field of view of 5° x 5°. The instrument was designed to look for optical counterparts of high-energy burst sources, as well as performing spectral analysis of the high-energy events.