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Statements

Subject Item
n2:RIV%2F68407700%3A21340%2F14%3A00224137%21RIV15-MSM-21340___
rdf:type
skos:Concept n14:Vysledek
dcterms:description
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. 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.
dcterms:title
The Large Observatory For x-ray Timing The Large Observatory For x-ray Timing
skos:prefLabel
The Large Observatory For x-ray Timing The Large Observatory For x-ray Timing
skos:notation
RIV/68407700:21340/14:00224137!RIV15-MSM-21340___
n3:aktivita
n12:I
n3:aktivity
I
n3:dodaniDat
n16:2015
n3:domaciTvurceVysledku
n21:8215154
n3:druhVysledku
n6:D
n3:duvernostUdaju
n19:S
n3:entitaPredkladatele
n9:predkladatel
n3:idSjednocenehoVysledku
25667
n3:idVysledku
RIV/68407700:21340/14:00224137
n3:jazykVysledku
n5:eng
n3:klicovaSlova
Observatories; X-rays; Spectral resolution; Vision; Sensors; Equipment and services
n3:klicoveSlovo
n7:Spectral%20resolution n7:Vision n7:Sensors n7:Observatories n7:Equipment%20and%20services n7:X-rays
n3:kontrolniKodProRIV
[4DA9E5DF1D8B]
n3:mistoKonaniAkce
Montréal
n3:mistoVydani
Bellingham
n3:nazevZdroje
Proceedings of SPIE vol. 9144: Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray
n3:obor
n18:JB
n3:pocetDomacichTvurcuVysledku
1
n3:pocetTvurcuVysledku
344
n3:rokUplatneniVysledku
n16:2014
n3:tvurceVysledku
Andersson, N. Barret, D. van der Klis, M. Watts, A. Alford, M. Santangelo, A. Amoros, C. Argan, A. Alpar, A. Antonelli, A. Stella, L. Wilms, J. Amati, L. Altamirano, D. Zane, S. Albertus, C. Feroci, M. Brandt, S. Pohl, M. Ahangarianabhari, M. Petráček, Vojtěch Hernanz, M. Alvarez, L. Bozzo, E. Hudec, René den Herder, J. W.
n3:typAkce
n11:WRD
n3:zahajeniAkce
2014-06-22+02:00
s:issn
0277-786X
s:numberOfPages
20
n15:doi
10.1117/12.2055913
n20:hasPublisher
SPIE
n13:isbn
978-0-8194-9612-6
n4:organizacniJednotka
21340