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A CdTe Position Sensitive Detector for a Hard X-and Gamma-Ray Wide Field Camera

Published online by Cambridge University Press:  10 February 2011

E. Caroli ,
G. Bertuccio ,
G. De Cesare ,
A. Donati ,
W. Dusi ,
G. Landini ,
F. Perotti ,
M. Sampietro  and
J. B. Stephen
E. Caroli
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
G. Bertuccio
Affiliation:
Dip. di Elettronica ed Informatica, Politecnico, Piazza L. Da Vinci 32, 20133 Milano, Italy
G. De Cesare
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
A. Donati
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
W. Dusi
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
G. Landini
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
F. Perotti
Affiliation:
IFCTR/CNR, Via Bassini 13, 20133 Milano, Italy
M. Sampietro
Affiliation:
Dip. di Elettronica ed Informatica, Politecnico, Piazza L. Da Vinci 32, 20133 Milano, Italy
J. B. Stephen
Affiliation:
Istituto TESRE/CNR, Via Gobetti 101, 40129 Bologna, Italy, caroli@tesre.bo.cnr.it
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Abstract

An important region of the electromagnetic spectrum for astrophysics is the hard X- and gamma ray band between 10 keV and a few MeV, where several processes occur in a wide variety of objects and with different spatial distribution and time scales. In order to fulfill the observational requirements in this energy range and taking into account the opportunities given by small/medium size missions (e.g. on the ISS), we have proposed a compact, wide field camera based on a thick (1 cm) position sensitive CdTe detector (PSD). The detector is made of an array of 128×96 CdTe microspectrometers with a pixel size of 2×2 mm2. The basic element of the PSD is the linear module that is an independent detection unit with 32 CdTe crystals and monolithic front-electronics (ASIC) supported by a thin (300 μm) ceramic layer. The expected performance of the PSD over the operative energy range and some of the required ASIC functionality are presented and discussed.

Type
Research Article
Information
MRS Online Proceedings Library (OPL) , Volume 487: Symposium I – Semiconductors for Room-Temperature Radiation II , 1997 , 275
Copyright
Copyright © Materials Research Society 1998

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References

1. Gehrels, N. et al., SPIE Proceedings, 2806, p. 12 (1996).Google Scholar
2. McConnell, M. et al., SPIE Proceedings, 2806, p. 349 (1996).Google Scholar
3. Tümer, T.O. et al., Conference Record of the 1996 IEEE Nucl. Sci. Symp., 1, p. 84 (1997).Google Scholar
4. Caroli, E. et al., Proposal 043-I-SCI in response to ESA A.O. SP-1201 Dec. 1996 (1997).Google Scholar
5. Caroli, E. et al., in Photon Detectors for Space Instruments, ESA SP–356, p. 27 (1992).Google Scholar
6. Lund, J. et al., IEEE Trans. Nucl. Sci., NS–43, p. 1411 (1996).Google Scholar
7. Skinner, G.K., and Grindlay, J. E., Astronomy & Astrophysics, 276, p. 673 (1993).Google Scholar
8. Doty, F.P. et al., Nucl. Instr. And Meth., A353, p. 356 (1994).Google Scholar
9. Casali, F. et al., IEEE Trans. Nucl. Sci., NS–39, p. 598 (1992).Google Scholar
10. Caroli, E. et al., Imaging in High Energy Astronomy, edited by Bassani, L. and Cocco, G. Di (Kluwer Academic Publ. 1995), p. 345.Google Scholar
11. Gehrels, N., Nuclear Instr. and Meth., A313, p. 513 (1992).Google Scholar
12. Parsons, A., et al., SPIE Proceedings, 2806, p. 432 (1996).Google Scholar