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Early Results from the Low-Energy Concentrator Spectrometer on-board BeppoSAX

Published online by Cambridge University Press:  25 May 2016

A.N. Parmar ,
M. Bavdaz ,
F. Favata ,
T. Oosterbroek ,
A. Orr ,
A. Owens ,
U. Lammers  and
D. Martin
A.N. Parmar
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
M. Bavdaz
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
F. Favata
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
T. Oosterbroek
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
A. Orr
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
A. Owens
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
U. Lammers
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands
D. Martin
Affiliation:
Astrophysics Division, Space Science Department of ESA ESTEC, 2200 AG Noordwijk, The Netherlands

Extract

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SAX, an acronym for “Satellite Italiano per Astronomia a raggi X”, now renamed “BeppoSAX” in honor of Giuseppe Occhialini, is the first X-ray mission sensitive in the very broad energy range between 0.1 and 300 keV (Boella et al. 1997a). The Narrow Field Instruments (NFI) have approximately 1° fields of view and consist of the imaging low- and medium-energy concentrator spectrometers (LECS, 0.1-10 keV, Parmar et al. 1997; and MECS, 1-10 keV, Boella et al. 1997b), and the non-imaging high pressure gas scintillation proportional counter (HPGSPC, 3-120 keV, Manzo et al. 1997) and Phoswich detector system (PDS, 15-300 keV, Frontera et al. 1997). All the NFI are coaligned and are normally operated simultaneously. In addition, the payload includes two wide field cameras (WFC, 2-30 keV; Jager et al. 1997) which observe in directions perpendicular to the NFI. These allow the detection of X-ray transient phenomena, as well as long-term variability studies.

Type
Session 2: Future Space Programs
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 71 - 74
Copyright
Copyright © Kluwer 1998 

References

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