The large observatory for x-ray timing

M. Feroci, J. W. 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. AmatiC. Amoros, N. Andersson, A. Antonelli, A. Argan, R. Artigue, B. Artigues, J. L. 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, J. M. Bonnet Bidaud, S. Boutloukos, L. Bradley, J. Braga, E. Brown, N. Bucciantini, L. Burderi, M. Burgay, M. Bursa, C. Budtz-Jørgensen, E. Cackett, F. R. Cadoux, P. Caïs, G. A. Caliandro, R. Campana, S. Campana, F. Capitanio, J. Casares, P. Casella, A. J. 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, J. P.C. 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, M. H. Erkut, P. Esposito, Y. Evangelista, A. Fabian, M. Falanga, Y. Favre, C. Feldman, V. Ferrari, C. Ferrigno, M. Finger, M. H. Finger, G. W. Fraser, M. Frericks, F. Fuschino, M. Gabler, D. K. Galloway, J. L. Galvez Sanchez, E. Garcia-Berro, B. Gendre, S. Gezari, A. B. Giles, M. Gilfanov, P. Giommi, G. Giovannini, M. Giroletti, E. Gogus, A. Goldwurm, K. Goluchová, D. Götz, C. Gouiffes, M. Grassi, P. Groot, M. Gschwender, L. Gualtieri, C. Guidorzi, L. Guy, D. Haas, P. Haensel, M. Hailey, F. Hansen, D. H. Hartmann, C. A. Haswell, K. Hebeler, A. Heger, W. Hermsen, J. Homan, A. Hornstrup, R. Hudec, J. Huovelin, A. Ingram, J. J.M. In't Zand, G. Israel, K. Iwasawa, L. Izzo, H. M. Jacobs, F. Jetter, T. Johannsen, P. Jonker, J. Josè, P. Kaaret, G. Kanbach, V. Karas, D. Karelin, D. Kataria, L. Keek, T. Kennedy, D. Klochkov, W. Kluzniak, K. Kokkotas, S. Korpela, C. Kouveliotou, I. Kreykenbohm, L. M. Kuiper, I. Kuvvetli, C. Labanti, D. Lai, F. K. Lamb, P. P. Laubert, F. Lebrun, D. Lin, D. Linder, G. Lodato, F. Longo, N. Lund, T. J. Maccarone, D. Macera, S. Maestre, S. Mahmoodifar, D. Maier, P. Malcovati, I. Mandel, V. Mangano, A. Manousakis, M. Marisaldi, A. Markowitz, A. Martindale, G. Matt, I. M. Mchardy, A. Melatos, M. Mendez, S. Mereghetti, M. Michalska, S. Migliari, R. Mignani, M. C. Miller, J. M. Miller, T. Mineo, G. Miniutti, S. Morsink, C. Motch, S. Motta, M. Mouchet, G. Mouret, J. Mulaová, F. Muleri, T. Muñoz-Darias, I. Negueruela, J. Neilsen, A. J. Norton, M. Nowak, P. O'brien, P. E.H. Olsen, M. Orienti, M. Orio, M. Orlandini, P. Orleaaski, J. P. Osborne, R. Osten, F. Ozel, L. Pacciani, M. Paolillo, A. Papitto, J. M. Paredes, A. Patruno, B. Paul, E. Perinati, A. Pellizzoni, A. V. Penacchioni, M. A. Perez, V. Petracek, C. Pittori, J. Pons, J. Portell, A. Possenti, J. Poutanen, M. Prakash, P. Le Provost, D. Psaltis, D. Rambaud, P. Ramon, G. Ramsay, M. Rapisarda, A. Rachevski, I. Rashevskaya, P. S. Ray, N. Rea

Research output: Chapter in Book/Report/Conference proceedingConference PaperResearch

30 Citations (Scopus)

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 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.

Original languageEnglish
Title of host publicationSpace Telescopes and Instrumentation 2014
Subtitle of host publicationUltraviolet to Gamma Ray
EditorsTadayuki Takahashi, Jan-Willem A den Herder, Mark Bautz
PublisherSPIE
Number of pages20
Volume9144
ISBN (Electronic)9780819496126
DOIs
Publication statusPublished - 1 Jan 2014
EventConference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray 2014 - Montreal, Canada
Duration: 22 Jun 201426 Jun 2014
https://spie.org/AS14/conferencedetails/space-telescopes-and-instrumentation-uv-to-gamma (Proceedings)

Publication series

NameProceedings of SPIE
PublisherSPIE
Volume9144
ISSN (Print)0277-786X

Conference

ConferenceConference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray 2014
CountryCanada
CityMontreal
Period22/06/1426/06/14
Internet address

Keywords

  • compact objects
  • microchannel plates
  • X-ray detectors
  • X-ray imaging
  • X-ray spectroscopy
  • X-ray timing

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