LEDAS  
Leicester Database and Archive Service
 
Mission
    Description
Products
    Databases
Raw Data
    Archive
Analysis Software
    Archive
Ginga Information
Ginga Gallery
Related Sites
Databases
GINGALAC
GINGABGD
GINGAFRF
GINGALOG
GINGAMODE
GINGARAW
View Ginga DBs
Line
Footer
e-mail

Description of the Ginga Mission

Ginga (the name means "galaxy" in Japanese) was the third Japanese X-ray astronomy satellite. It was launched on 5th February 1987 and re-entered the atmosphere on 1st November 1991 following the natural decay of the orbit. The main scientific instrument was the Large Area Proportional Counter (LAC; Turner et al. 1989) designed and built by a group in the UK led by Leicester University. The other instruments on board were the All-Sky Monitor and Gamma-ray Burst Detector. A full description of the satellite is given in Makino et al. (1987). During its lifetime Ginga performed over 1000 observations of approximately 350 different targets, covering all classes of cosmic X-ray sources then known.

The satellite was placed into an orbit with perigee of 510 km and apogee of 670 km and an inclination of 31°. Its orbital period was ~96 minutes. Ginga was approximately 1000 x 1000 x 1550 mm in size. It weighed about 420 kg. The Ginga configuration is shown in the figure above. The spacecraft was three-axis stabilised by a momentum wheel and a four-gyro inertial reference system, calibrated by two CCD star trackers. The spacecraft pointing manoeuvers were carried out with three-axis magnetic torquers.

The time required to move the Z-axis was slow and observation lengths of less than a day were not practical. Manoevers that rotated around the Z-axis were made quicker, but this required a suitable alignment of the sources carried out with three-axis torquers. The pointing accuracy was better than six arc minutes, while the attitude reconstruction had an accuracy of approximately one arc minute. The solar panels had to be held within 45 degrees of the sun direction in order to satisfy power constraints. This constraint limited the portion of the sky observable by the LAC at any given time of the year, to within a band of +/- 45 degrees wide along a great circle perpendicular to the sun vector. Data were transmitted at three different bit rates: 16384 bps (high rate), 2048 bps (medium rate) and 512 bps (low rate). An on-board bubble-memory data recorder with a capacity of 41.9 Mbits could store data for 42.7 minutes at the high data rate, 5.68 hours at the medium rate, and 22.73 hours at the low data rate. The stored date were played back during a ground contact at either 65,536 bps or 131,072 bps.

Large Area Proportional Counter

The LAC experiment, sensitive to X-rays with energy 1.5-37 keV, consisted of eight collimated co-aligned proportional counters with a total effective area of approximately 4000 cm² and energy resolution of 18%; at 6 keV, scaling as E throughout the full energy range. In each counter the anode structure was of a multi-layer and multi-cell design which provided both gain uniformity and low internal background through the use of anticoincidence. The high voltage supply was normally operated at ~ 1830 V, but was reduced occasionally to ~ 1745 V to achieve a larger energy range. Steel collimators restricted the field of view to 1.1 x 2.0 degrees (FWHM); the top and bottom 15 mm were coated with silver paint to prevent contamination through iron, nickel and chrome fluorescence lines. The fluorescence line of silver at 22.1 keV can be visible at high energy but is well away from lines of astrophysical importance and can be used for calibration.

The origin and behaviour of the LAC background is described in Hayashida et al. (1989). The main sources of background include the internal component generated after passage through the Earth's radiation belts, in particular the South Atlantic Anomaly, the high- and low-energy particles in the Earth's magnetosphere, and the diffuse Cosmic X-ray Background (CXB). The first two components generate a background which is a strong function of time and energy. Summed over the top- and mid-layer electrodes as well as over the full energy range (1.5-37 keV), this varies between 50 and 100 counts sec-1 . The CXB contributes approximately 18 counts sec-1 to the background, which varies as a function of position in the sky but is constant in time.

All-Sky Monitor (ASM)


The All-Sky Monitor (ASM) consisted of 2 identical gas proportional counters, and was sensitive to 1-20 keV. Each counter was equipped with a collimator which had 3 different fields of view (1° x 45° FWHM). The aim of the ASM was to create an all-sky survey every 1-2 days to look for transient events (to alert the LAC) and to collect a long-term record for X-ray sources.

Gamma-Ray Burst Detector (GBD)


The purpose of the Gamma-Ray Burst Detector (GBD) was to detect gamma-ray bursts in the energy range 1-500 keV with a time resolution of 31.3 msec and high-energy resolution. It was comprised of two sensors: a proportional counter (PC) and a scintillation spectrometer (SC). The GBD could also operate as a radiation belt monitor for high particle backgrounds which could harm the other 2 experiments.

 
HOME
SEARCH
SERVICES INFO SOFTWARE ViZieR BLASTA DSS
ARCHIVES ASCA CHANDRA GINGA ROSAT ARNIE