Get Proceedings of the the Third Workshop on Science with the PDF

By Alessandro DeAngelis,Oriana Mansutti

ISBN-10: 9812568131

ISBN-13: 9789812568137

The contributions during this quantity offer a image of the newest study and destiny plans for space-borne and ground-based experiments devoted to the remark of the gamma-ray sky. The articles are authored through either pro veterans of the 1st devoted gamma-ray missions, and younger scientists getting into the interesting box of gamma-ray astrophysics. With the appearance of gamma-ray instrumentation on spacecraft and massive and delicate ground-based detectors, new and unforeseen phenomena were stumbled on, reminiscent of gamma-ray bursts and gamma-ray emission from blazars. The sizeable energy of the sector within the present "post-EGRET period" is witnessed by means of the varied ongoing and approaching gamma-ray experiments documented right here, complementary to numerous cosmic-ray, neutrino, astroparticle and X-ray initiatives.

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XRT light curves The analysis of the following light curves, GRB011121, GRB050126, GRB050219A, GRB050315 and GRB050319, showed since the very beginning the main characteristics that have been described in a more organic way by Chincarini et al. [6] and by Nousek et al. [7]. Figure 1. Left: Cas A obtained by XMM on August 2001 with an integration of 7419 seconds. Right: Cas A observed by XRT on December 2004, during the activation phase, with an exposure of 10997 seconds. 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.

A dedicated procedure has been implemented to perform a threshold scan for each channel 54 §100 F Threshold scan 6014 200 225 250 th (DAC),ch 9 50 100 150 (a) 200 250 300 350 channel (b) Figure 7. (a) Example of a threshold scan on a channel; the horizontal axis is in arbitrary units, (b) Calibration signal amplitude computed from the threshold scans of each channel. EntrlM M**n RUS ecoo 6000 SO0O 4000 : /\ - MIS 1340 1 j 3000 2000 1000 - / L , . . I . . 161 L-, SCO (c) (d) Figure 8. Typical cosmic ray results: (a) beam profile; (b) signal to noise ratio for the strip with the maximum signal; (c) cluster pulse height; (d) number of strips per cluster.

I . 50 o 10 (a) . . i i . . 100 **" " * " i i . . 150 20 • . i — 200 250 \ , . 300 , , i , . 350 Channel (b) Figure 6. (a) Analog shape of one TAA1 channel. Both the axis are in arbitrary units. (b) Gain in ADC/mV of the three ASICs of one HDI. 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.

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Proceedings of the the Third Workshop on Science with the New Generation of High Energy Gamma-Ray Experiments: Cividale del Fiuli, Italy, 30 May - 1 June 2005 by Alessandro DeAngelis,Oriana Mansutti


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