The Large Observatory for X-ray Timing (LOFT)

Feroci, M.; Stella, L.; van der Klis, M.; Courvoisier, T. J.-L.; Hernanz, M.; Hudec, R.; Santangelo, A.; Walton, D.; Zdziarski, A.; Barret, D.; Belloni, T.; Braga, J.; Brandt, S.; Budtz-Jørgensen, C.; Campana, S.; den Herder, J.-W.; Huovelin, J.; Israel, G. L.; Pohl, M.; Ray, P.; Vacchi, A.; Zane, S.; Argan, A.; Attinà, P.; Bertuccio, G.; Bozzo, E.; Campana, R.; Chakrabarty, D.; Costa, E.; De Rosa, A.; Del Monte, E.; Di Cosimo, S.; Donnarumma, I.; Evangelista, Y.; Haas, D.; Jonker, P.; Korpela, S.; Labanti, C.; Malcovati, P.; Mignani, R.; Muleri, F.; Rapisarda, M.; Rashevsky, A.; Rea, N.; Rubini, A.; Tenzer, C.; Wilson-Hodge, C.; Winter, B.; Wood, K.; Zampa, G.; Zampa, N.; Abramowicz, M. A.; Alpar, M. A.; Altamirano, D.; Alvarez, J. M.; Amati, L.; Amoros, C.; Antonelli, L. A.; Artigue, R.; Azzarello, P.; Bachetti, M.; Baldazzi, G.; Barbera, M.; Barbieri, C.; Basa, S.; Baykal, A.; Belmont, R.; Boirin, L.; Bonvicini, V.; Burderi, L.; Bursa, M.; Cabanac, C.; Cackett, E.; Caliandro, G. A.; Casella, P.; Chaty, S.; Chenevez, J.; Coe, M. J.; Collura, A.; Corongiu, A.; Covino, S.; Cusumano, G.; D'Amico, F.; D’Amico, F.; Dall’Osso, S.; De Martino, D.; De Paris, G.; Di Persio, G.; Di Salvo, T.; Done, C.; Dovčiak, M.; Drago, A.; Ertan, U.; Fabiani, S.; Falanga, M.; Fender, R.; Ferrando, P.; Della Monica Ferreira, D.; Fraser, G.; Frontera, F.; Fuschino, F.; Galvez, J. L.; Gandhi, P.; Giommi, P.; Godet, O.; Göǧüş, E.; Goldwurm, A.; Götz, D.; Grassi, M.; Guttridge, P.; Hakala, P.; Henri, G.; Hermsen, W.; Horak, J.; Hornstrup, A.; in’t Zand, J. J. M.; Isern, J.; Kalemci, E.; Kanbach, G.; Karas, V.; Kataria, D.; Kennedy, T.; Klochkov, D.; Kluźniak, W.; Kokkotas, K.; Kreykenbohm, I.; Krolik, J.; Kuiper, L.; Kuvvetli, I.; Kylafis, N.; Lattimer, J. M.; Lazzarotto, F.; Leahy, D.; Lebrun, F.; Lin, D.; Lund, N.; Maccarone, T.; Malzac, J.; Marisaldi, M.; Martindale, A.; Mastropietro, M.; McClintock, J.; McHardy, I.; Mendez, M.; Mereghetti, S.; Miller, M. C.; Mineo, T.; Morelli, E.; Morsink, S.; Motch, C.; Motta, S.; Muñoz-Darias, T.; Naletto, G.; Neustroev, V.; Nevalainen, J.; Olive, J. F.; Orio, M.; Orlandini, M.; Orleanski, P.; Ozel, F.; Pacciani, L.; Paltani, S.; Papadakis, I.; Papitto, A.; Patruno, A.; Pellizzoni, A.; Petráček, V.; Petri, J.; Petrucci, P. O.; Phlips, B.; Picolli, L.; Possenti, A.; Psaltis, D.; Rambaud, D.; Reig, P.; Remillard, R.; Rodriguez, J.; Romano, P.; Romanova, M.; Schanz, T.; Schmid, C.; Segreto, A.; Shearer, A.; Smith, A.; Smith, P. J.; Soffitta, P.; Stergioulas, N.; Stolarski, M.; Stuchlik, Z.; Tiengo, A.; Torres, D.; Török, G.; Turolla, R.; Uttley, P.; Vaughan, S.; Vercellone, S.; Waters, R.; Watts, A.; Wawrzaszek, R.; Webb, N.; Wilms, J.; Zampieri, L.; Zezas, A.; Ziolkowski, J.

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Springer (part of Springer Nature), Experimental Astronomy, 2(34), p. 415-444

DOI: 10.1007/s10686-011-9237-2

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The Large Observatory for X-ray Timing (LOFT)

Journal article published in 2011 by M. Feroci, L. Stella, M. van der Klis, T. J.-L. Courvoisier, M. Hernanz, R. Hudec, A. Santangelo, D. Walton, A. Zdziarski, D. Barret, T. Belloni, J. Braga, S. Brandt, C. Budtz-Jørgensen, S. Campana and other authors.

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Abstract

From the issue entitled "Special Issue: ESA's Cosmic Vision 2015-2025 Astrophysics and Fundamental Physics Mission Proposals" ; High-time-resolution X-ray observations of compact objects provide direct access to strong-field gravity, to the equation of state of ultradense matter and to black hole masses and spins. A 10 m2-class instrument in combination with good spectral resolution is required to exploit the relevant diagnostics and answer two of the fundamental questions of the European Space Agency (ESA) Cosmic Vision Theme "Matter under extreme conditions", namely: does matter orbiting close to the event horizon follow the predictions of general relativity? What is the equation of state of matter in neutron stars? The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionise the study of collapsed objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. Thanks to an innovative design and the development of large-area monolithic silicon drift detectors, the Large Area Detector (LAD) on board LOFT will achieve an effective area of ~12 m2 (more than an order of magnitude larger than any spaceborne predecessor) in the 2-30 keV range (up to 50 keV in expanded mode), yet still fits a conventional platform and small/medium-class launcher. With this large area and a spectral resolution of

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The Large Observatory for X-ray Timing (LOFT)

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