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The large observatory for x-ray timing


Feroci, M and den Herder, JW 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, A 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, JL 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, JM 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-Jorgensen, C and Cackett, E and Cadoux, FR and Cais, P and Caliandro, GA and Campana, R and Campana, S and Capitanio, F and Casares, J and Casella, P and Castro-Tirado, AJ and Cavazzuti, E and Cerda-Duran, P and Chakrabarty, D and Chateau, F and Chenevez, J and Coker, J and Cole, R and Collura, A and Cornelisse, R and Courvoisier, T and Cros, A and Cumming, A and Cusumano, G and D'Ai, A and D'Elia, V and Del Monte, E and de Luca, A and de Martino, D and Dercksen, JPC and de Pasquale, M and De Rosa, A and Del Santo, M and Di Cosimo, S and Diebold, S and Di Salvo, T and Donnarumma, I and Drago, A and Durant, M and Emmanoulopoulos, D and Erkut, MH and Esposito, P and Evangelista, Y and Fabian, A and Falanga, M and Favre, Y and Feldman, C and Ferrari, V and Ferrigno, C and Finger, M and Finger, MH and Fraser, GW and Frericks, M and Fuschino, F and Gabler, M and Galloway, DK and Galvez Sanchez, JL and Garcia-Berro, E and Gendre, B and Gezari, S and Giles, AB and Gilfanov, M and Giommi, P and Giovannini, G and Giroletti, M and Gogus, E and Goldwurm, A and Goluchova, K and Gotz, D and Gouiffes, C and Grassi, M and Groot, P and Gschwender, M and Gualtieri, L and Guidorzi, C and Guy, L and Haas, D and Haensel, P and Hailey, M and Hansen, F and Hartmann, DH and Haswell, CA and Hebeler, K and Heger, A and Hermsen, W and Homan, J and Hornstrup, A and Hudec, R and Huovelin, J and Ingram, A and In't Zand, JJM and Israel, G and Iwasawa, K and Izzo, L and Jacobs, HM and Jetter, F and Johannsen, T and Jonker, P and Jose, J and Kaaret, P and Kanbach, G and Karas, V and Karelin, D and Kataria, D and Keek, L and Kennedy, T and Klochkov, D and Kluzniak, W and Kokkotas, K and Korpela, S and Kouveliotou, C and Kreykenbohm, I and Kuiper, LM and Kuvvetli, I and Labanti, C and Lai, D and Lamb, FK and Laubert, PP and Lebrun, F and Lin, D and Linder, D and Lodato, G and Longo, F and Lund, N and Maccarone, TJ and Macera, D and Maestre, S and Mahmoodifar, S and Maier, D and Malcovati, P and Mandel, I and Mangano, V and Manousakis, A and Marisaldi, M and Markowitz, A and Martindale, A and Matt, G and McHardy, IM and Melatos, A and Mendez, M and Mereghetti, S and Michalska, M and Migliari, S and Mignani, R and Miller, MC and Miller, JM and Mineo, T and Miniutti, G and Morsink, S and Motch, C and Motta, S and Mouchet, M and Mouret, G and Mulacova, J and Muleri, F and Munoz-Darias, T and Negueruela, I and Neilsen, J and Norton, AJ and Nowak, M and O'Brien, P and Olsen, PEH and Orienti, M and Orio, M and Orlandini, M and Orleanski, P and Osborne, JP and Osten, R and Ozel, F and Pacciani, L and Paolillo, M and Papitto, A and Paredes, JM and Patruno, A and Paul, B and Perinati, E and Pellizzoni, A and Penacchioni, AV and Perez, MA and Petracek, V and Pittori, C and Pons, J and Portell, J and Possenti, A and Poutanen, J and Prakash, M and Le Provost, P and Psaltis, D and Rambaud, D and Ramon, P and Ramsay, G and Rapisarda, M and Rachevski, A and Rashevskaya, I and Ray, PS and Rea, N and Reddy, S and Reig, P and Reina Aranda, M and Remillard, R and Reynolds, C and Rezzolla, L and Ribo, M and de la Rie, R and Riggio, A and Rios, A and Rodriguez-Gil, P and Rodriguez, J and Rohlfs, R and Romano, P and Rossi, EMR and Rozanska, A and Rousseau, A and Ryde, F and Sabau-Graziati, L and Sala, G and Salvaterra, R and Sanna, A and Sandberg, J and Scaringi, S and Schanne, S and Schee, J and Schmid, C and Shore, S and Schneider, R and Schwenk, A and Schwope, AD and Seyler, J-Y and Shearer, A and Smith, A and Smith, DM and Smith, PJ and Sochora, V and Soffitta, P and Soleri, P and Spencer, A and Stappers, B and Steiner, AW and Stergioulas, N and Stratta, G and Strohmayer, TE and Stuchlik, Z and Suchy, S and Sulemainov, V and Takahashi, T and Tamburini, F and Tauris, T and Tenzer, C and Tolos, L and Tombesi, F and Tomsick, J and Torok, G and Torrejon, JM and Torres, DF and Tramacere, A and Trois, A and Turolla, R and Turriziani, S and Uter, P and Uttley, P and Vacchi, A and Varniere, P and Vaughan, S and Vercellone, S and Vrba, V and Walton, D and Watanabe, S and Wawrzaszek, R and Webb, N and Weinberg, N and Wende, H and Wheatley, P and Wijers, R and Wijnands, R and Wie, M and Wilson-Hodge, CA and Winter, B and Wood, K and Zampa, G and Zampa, N and Zampieri, L and Zdunik, L and Zdziarski, A and Zhang, B and Zwart, F and Ayre, M and Boenke, T and Corral van Damme, C and Kuulkers, E and Lumb, D, The large observatory for x-ray timing, SPIE Proceedings: Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 22-26 June 2014, Montreal, Canada, pp. 91442T. ISSN 0277-786X (2014) [Refereed Conference Paper]

DOI: doi: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. (2014) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only. Powered by Boohle

Item Details

Item Type:Refereed Conference Paper
Keywords:observatories, x-rays, spectral resolution, vision, sensors, equipment and services
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Giles, AB (Dr Barry Giles)
ID Code:106893
Year Published:2014
Web of Science® Times Cited:26
Deposited By:Mathematics and Physics
Deposited On:2016-02-25
Last Modified:2018-03-20

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