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Proceedings Paper

Design and development of the SIMBOL-X hard x-ray optics
Author(s): G. Pareschi; P. Attinà; S. Basso; G. Borghi; W. Burkert; R. Buzzi; O. Citterio; M. Civitani; P. Conconi; V. Cotroneo; G. Cusumano; E. Dell'Orto; M. Freyberg; G. D. Hartner; P. Gorenstein; E. Mattaini; F. Mazzoleni; G. Parodi; S. Romaine; D. Spiga; G. Tagliaferri; R. Valtolina; G. Valsecchi; D. Vernani
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Paper Abstract

The SIMBOL-X formation-flight X-ray mission will be operated by ASI and CNES in 2014, with a large participation of the French and Italian high energy astrophysics scientific community. Also German and US Institutions are contributing in the implementation of the scientific payload. Thanks to the formation-flight architecture, it will be possible to operate a long (20 m) focal length grazing incidence mirror module, formed by 100 confocal multilayer-coated Wolter I shells. This system will allow us to focus X-rays over a very broad energy band, from 0.5 keV up to 80 keV and beyond, with more than two orders of magnitude improvement in angular resolution (20 arcsec HEW) and sensitivity (0.5 µCrab on axis @30 keV) compared to non focusing detectors used so far. The X-ray mirrors will be realized by Ni electroforming replication, already successfully used for BeppoSAX, XMM-Newton, and JET-X/SWIFT; the thickness trend will be about two times less than for XMM, in order to save mass. Multilayer reflecting coatings will be implemented, in order to improve the reflectivity beyond 10 keV and to increase the field of view 812 arcmin at 30 keV). In this paper, the SIMBOL-X optics design, technology and implementation challenges will be discussed; it will be also reported on recent results obtained in the context of the SIMBOL-X optics development activities.

Paper Details

Date Published: 15 July 2008
PDF: 12 pages
Proc. SPIE 7011, Space Telescopes and Instrumentation 2008: Ultraviolet to Gamma Ray, 70110N (15 July 2008); doi: 10.1117/12.790336
Show Author Affiliations
G. Pareschi, INAF, Osservatorio Astronomico di Brera (Italy)
P. Attinà, ThalesAleniaSpace (Italy)
S. Basso, INAF, Osservatorio Astronomico di Brera (Italy)
G. Borghi, Media-Lario Technology (Italy)
W. Burkert, Max-Planck-Institut für extraterrestrische Physik, PANTER (Germany)
R. Buzzi, BCV Progetti (Italy)
O. Citterio, INAF, Osservatorio Astronomico di Brera (Italy)
Media-Lario Technology (Italy)
M. Civitani, INAF, Osservatorio Astronomico di Brera (Italy)
ThalesAleniaSpace (Italy)
P. Conconi, INAF, Osservatorio Astronomico di Brera (Italy)
V. Cotroneo, INAF, Osservatorio Astronomico di Brera (Italy)
Media-Lario Technology (Italy)
G. Cusumano, INAF-Istituto di Astrofisica Spaziale e Fisica Spaziale (Italy)
E. Dell'Orto, INAF, Osservatorio Astronomico di Brera (Italy)
M. Freyberg, Max-Planck-Institut für extraterrestrische Physik, PANTER (Germany)
G. D. Hartner, Max-Planck-Institut für extraterrestrische Physik, PANTER (Germany)
P. Gorenstein, Harvard-Smithsonian Ctr. for Astrophysics (United States)
E. Mattaini, INAF-Istituto di Astrofisica Spaziale e Fisica Spaziale (Italy)
F. Mazzoleni, INAF, Osservatorio Astronomico di Brera (Italy)
G. Parodi, BCV Progetti (Italy)
S. Romaine, Harvard-Smithsonian Ctr. for Astrophysics (United States)
D. Spiga, INAF, Osservatorio Astronomico di Brera (Italy)
G. Tagliaferri, INAF, Osservatorio Astronomico di Brera (Italy)
R. Valtolina, INAF, Osservatorio Astronomico di Brera (Italy)
G. Valsecchi, Media-Lario Technology (Italy)
D. Vernani, INAF, Osservatorio Astronomico di Brera (Italy)
Media-Lario Technology (Italy)


Published in SPIE Proceedings Vol. 7011:
Space Telescopes and Instrumentation 2008: Ultraviolet to Gamma Ray
Martin J. L. Turner; Kathryn A. Flanagan, Editor(s)

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