The large observatory for x-ray timing

M Feroci; JW Den Herder; E Bozzo; D Barret; S Brandt; M Hernanz; M Van Der Klis; M Pohl; A Santangelo; L Stella; A Watts; J Wilms; S Zane; M Ahangarianabhari; C Albertus; M Alford; A Alpar; D Altamirano; L Alvarez; L Amati; C Amoros; N Andersson; A Antonelli; A Argan; R Artigue; B Artigues; JL Atteia; P Azzarello; P Bakala; G Baldazzi; S Balman; M Barbera; C Van Baren; S Bhattacharyya; A Baykal; T Belloni; F Bernardini; G Bertuccio; S Bianchi; A Bianchini; P Binko; P Blay; F Bocchino; P Bodin; I Bombaci; JM Bonnet Bidaud; S Boutloukos; L Bradley; J Braga; E Brown; N Bucciantini; L Burderi; M Burgay; M Bursa; C Budtz-Jørgensen; E Cackett; FR Cadoux; P Caïs; GA Caliandro; R Campana; S Campana; F Capitanio; J Casares; P Casella; AJ Castro-Tirado; E Cavazzuti; P Cerda-Duran; D Chakrabarty; F Château; J Chenevez; J Coker; R Cole; A Collura; R Cornelisse; T Courvoisier; A Cros; A Cumming; G Cusumano; A D'ai; V D'elia; E Del Monte; A De Luca; D De Martino; JPC Dercksen; M De Pasquale; A De Rosa; M Del Santo; S Di Cosimo; S Diebold; T Di Salvo; I Donnarumma; A Drago; M Durant; D Emmanoulopoulos; MH Erkut; P Esposito; Y Evangelista; A Fabian; M Falanga; Y Favre

Conference Proceedings

The large observatory for x-ray timing

M Feroci, JW Den Herder, E Bozzo, D Barret, S Brandt, M Hernanz, M Van Der Klis, M Pohl, A Santangelo, L Stella, A Watts, J Wilms, S Zane, M Ahangarianabhari, C Albertus, M Alford, A Alpar, D Altamirano, L Alvarez, L Amati Show all

Proceedings of SPIE the International Society for Optical Engineering | Published : 2014

DOI: 10.1117/12.2055913

Abstract

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 Mo..

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