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By Alessandro DeAngelis,Oriana Mansutti
The contributions during this quantity offer a picture of the newest study and destiny plans for space-borne and ground-based experiments devoted to the commentary of the gamma-ray sky. The articles are authored by means of either pro veterans of the 1st committed gamma-ray missions, and younger scientists getting into the interesting box of gamma-ray astrophysics. With the arrival of gamma-ray instrumentation on spacecraft and massive and delicate ground-based detectors, new and unforeseen phenomena were stumbled on, corresponding to gamma-ray bursts and gamma-ray emission from blazars. The substantial power of the sector within the present "post-EGRET period" is witnessed by way of the varied ongoing and coming near near gamma-ray experiments documented the following, complementary to numerous cosmic-ray, neutrino, astroparticle and X-ray initiatives.
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OK ^ * * % ft " * JOOOMOOWfr Figure 1. 0-4622 obtained from the C A N G A R G O I I I stereo observations (preliminary). 5. Other sources We took fair amount of stereo data on the pulsar PSR 1706-44 and the supernova remnant SN1006 which we claimed to be TeV gamma-ray sources 28 with CANGAROO-I. Preliminary analysis of both objects did not show any peaks in the 62 distribution [21]. ) Further analysis is underway so that we can check the possible extended emission. 6. Summary We have been carrying out stereo observations of sub-TeV gamma-rays with four telescopes since March 2004.
It is clear from Figure 2 that the basic morphology is given, soon after the prompt emission, by a fast decay of the afterglow, see also Tagliaferri et al. [8], followed by a milder decay steeping down after a while. This will define the type 1 light curve. In one case, GRB050319 in Figure 2, the initial slope is much higher (about -6) but that is almost certainly due to an erroneous BAT trigger. Counting the time (to) from the beginning of the second BAT burst (in this GRB the prompt emission is composed by two bursts separated by about 137 seconds) the light curve of GRB050319 is exactly superimposed to the light curve of GRB050315.
In order to send a given signal to one channel at a time. Using the hold signal, the output amplitude can be sampled at different times from the signal generation thus obatining the shape of the analog signal (fig. 6a) of each channel. This procedure has been applied to all channels with 3 different input signal in order to calibrate the ASICs response. A shorter procedure has been performed on each ASIC after each following assembly step. Fig. 6b shows the gain of three ASICs of one HDI as computed using the calibration procedure.