Share Email Print
cover

Proceedings Paper

A large area detector proposed for the Large Observatory for X-ray Timing (LOFT)
Author(s): S. Zane; D. Walton; T. Kennedy; M. Feroci; J.-W. Den Herder; M. Ahangarianabhari; A. Argan; P. Azzarello; G. Baldazzi; D. Barret; G. Bertuccio; P. Bodin; E. Bozzo; F Cadoux; P. Cais; R. Campana; J. Coker; A. Cros; E. Del Monte; Alessandra De Rosa; S. Di Cosimo; I. Donnarumma; Y. Evangelista; Y. Favre; C. Feldman; G. Fraser; F. Fuschino; M. Grassi; M. R. Hailey; R. Hudec; C. Labanti; D. Macera; P. Malcovati; M. Marisaldi; A. Martindale; T. Mineo; F. Muleri; M. Nowak; M. Orlandini; L. Pacciani; E. Perinati; V. Petracek; M. Pohl; A. Rachevski; P. Smith; A. Santangelo; J.-Y. Seyler; C. Schmid; P. Soffitta; S. Suchy; C. Tenzer; P. Uttley; A. Vacchi; G. Zampa; N. Zampa; J. Wilms; B. Winter
Format Member Price Non-Member Price
PDF $14.40 $18.00

Paper Abstract

The Large Observatory for X-ray Timing (LOFT) is one of the four candidate ESA M3 missions considered for launch in the 2022 timeframe. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. The LOFT scientific payload is composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a 10 m2-class pointed instrument with 20 times the collecting area of the best past timing missions (such as RXTE) over the 2-30 keV range, which holds the capability to revolutionize studies of X-ray variability down to the millisecond time scales. Its ground-breaking characteristic is a low mass per unit surface, enabling an effective area of ~10 m2 (@10 keV) at a reasonable weight. The development of such large but light experiment, with low mass and power per unit area, is now made possible by the recent advancements in the field of large-area silicon detectors - able to time tag an X-ray photon with an accuracy <10 μs and an energy resolution of ~260 eV at 6 keV - and capillary-plate X-ray collimators. In this paper, we will summarize the characteristics of the LAD instrument and give an overview of its capabilities.

Paper Details

Date Published: 17 September 2012
PDF: 15 pages
Proc. SPIE 8443, Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray, 84432F (17 September 2012); doi: 10.1117/12.925156
Show Author Affiliations
S. Zane, Mullard Space Science Lab., Univ. College London (United Kingdom)
D. Walton, Mullard Space Science Lab., Univ. College London (United Kingdom)
T. Kennedy, Mullard Space Science Lab., Univ. College London (United Kingdom)
M. Feroci, INAF/IAPS Roma (Italy)
J.-W. Den Herder, SRON Netherlands Institute for Space Research (Netherlands)
M. Ahangarianabhari, Politecnico di Milano (Italy)
A. Argan, INAF HQ (Italy)
P. Azzarello, ISDC, Science Data Ctr. for Astrophysics (Switzerland)
G. Baldazzi, Univ. of Bologna (Italy)
D. Barret, Institut de Recherche en Astrophysique et Planetologie (France)
G. Bertuccio, Politecnico di Milano (Italy)
P. Bodin, CNES, Ctr. Spatial de Toulouse (France)
E. Bozzo, ISDC, Science Data Ctr. for Astrophysics (Switzerland)
F Cadoux, Geneva Univ. (Switzerland)
P. Cais, Lab. d'Astrophysique de Bordeaux, CNRS, Univ. Bordeaux (France)
R. Campana, INAF/IAPS Roma (Italy)
J. Coker, Mullard Space Science Lab., Univ. College London (United Kingdom)
A. Cros, Institut de Recherche en Astrophysique et Planetologie (France)
E. Del Monte, INAF/IAPS Roma (Italy)
Alessandra De Rosa, INAF/IAPS Roma (Italy)
S. Di Cosimo, INAF/IAPS Roma (Italy)
I. Donnarumma, INAF/IAPS Roma (Italy)
Y. Evangelista, INAF/IAPS Roma (Italy)
Y. Favre, Geneva Univ. (Switzerland)
C. Feldman, Univ. of Leicester (United Kingdom)
G. Fraser, Univ. of Leicester (United Kingdom)
F. Fuschino, INAF/IASF Bologna (Italy)
M. Grassi, Univ. of Pavia (Italy)
M. R. Hailey, Mullard Space Science Lab., Univ. College London (United Kingdom)
R. Hudec, Czech Technical Univ. in Prague (Czech Republic)
C. Labanti, INAF/IASF Bologna (Italy)
D. Macera, Politecnico di Milano (Italy)
P. Malcovati, Univ. of Pavia (Italy)
M. Marisaldi, INAF/IASF Bologna (Italy)
A. Martindale, Univ. of Leicester (United Kingdom)
T. Mineo, INAF/IASF Palermo (Italy)
F. Muleri, INAF/IAPS Roma (Italy)
M. Nowak, Massachusetts Institute of Technology (United States)
M. Orlandini, INAF/IASF Bologna (Italy)
L. Pacciani, INAF/IAPS Roma (Italy)
E. Perinati, Institut für Astronomie and Astrophysik, Univ. Tübingen (Germany)
V. Petracek, Czech Technical Univ. in Prague (Institute of Photonics and Nanotechnologies, CNR)
M. Pohl, Geneva Univ. (Switzerland)
A. Rachevski, INFN (Italy)
P. Smith, Mullard Space Science Lab., Univ. College London (United Kingdom)
A. Santangelo, Institut für Astronomie and Astrophysik, Univ. Tübingen (Germany)
J.-Y. Seyler, CNES, Ctr. Spatial de Toulouse (France)
C. Schmid, Dr. Remeis Observatory and ECAP, Univ. of Erlangen-Nuremberg (Germany)
P. Soffitta, INAF/IAPS Roma (Italy)
S. Suchy, Institut für Astronomie and Astrophysik, Univ. Tübingen (Germany)
C. Tenzer, Institut für Astronomie and Astrophysik, Univ. Tübingen (Germany)
P. Uttley, Astronomical Institute Anton Pannokoek, Univ. of Amsterdam (Netherlands)
A. Vacchi, INFN (Italy)
G. Zampa, INFN (Italy)
N. Zampa, INFN (Italy)
J. Wilms, Dr. Remeis Observatory and ECAP, Univ. of Erlangen-Nuremberg (Germany)
B. Winter, Mullard Space Science Lab., Univ. College London (United Kingdom)


Published in SPIE Proceedings Vol. 8443:
Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray
Tadayuki Takahashi; Stephen S. Murray; Jan-Willem A. den Herder, Editor(s)

© SPIE. Terms of Use
Back to Top