The large observatory for x-ray timing
Feroci, M. and den Herder, J. W. and Bozzo, E. and Barret, D. and Brandt, S. and Hernanz, M. and van der Klis, M. and Pohl, M. and Santangelo, A. and Stella, L. and Watts, A. and Wilms, J. and Zane, S. and Ahangarianabhari, M. and Albertus, C. and Alford, M. and Alpar, M. Ali and Altamirano, D. and Alvarez, L. and Amati, L. and Amoros, C. and Andersson, N. and Antonelli, A. and Argan, A. and Artigue, R. and Artigues, B. and Atteia, J.-L. and Azzarello, P. and Bakala, P. and Baldazzi, G. and Balman, S. and Barbera, M. and van Baren, C. and Bhattacharyya, S. and Baykal, A. and Belloni, T. and Bernardini, F. and Bertuccio, G. and Bianchi, S. and Bianchini, A. and Binko, P. and Blay, P. and Bocchino, F. and Bodin, P. and Bombaci, I. and Bonnet Bidaud, J.-M. and Boutloukos, S. and Bradley, L. and Braga, J. and Brown, E. and Bucciantini, N. and Burderi, L. and Burgay, M. and Bursa, M. and Budtz-Jørgensen, C. and Cackett, E. and Cadoux, F. R. and Cais, P. and Caliandro, G. 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ISSN 0277-786X (Print) 1996-756X (Online)
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Official URL: http://dx.doi.org/10.1117/12.2055913
The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final downselection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supranuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m2 effective area, 2-30 keV, 240 eV spectral resolution, 1° collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study.
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