The Large Observatory for X-ray Timing (LOFT)

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

doi:10.1007/s10686-011-9237-2

The Large Observatory for X-ray Timing (LOFT)

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
, J. W. den Herder
, J. Huovelin
, G. L. Israel
, M. Pohl
, P. Ray

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

Physics and Astronomy

Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
National Institute for Nuclear Physics
National Institute for Astrophysics
University of Amsterdam
University of Geneva
Institute of Space Studies of Catalonia
Czech Technical University in Prague
University of Tübingen
University College London
Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
Institute de Recherche en Astrophysique et Planétologie
Osservatorio Astronomico di Brera
Instituto Nacional de Pesquisas Espaciais
Technical University of Denmark
SRON Netherlands Institute for Space Research
University of Helsinki
Naval Research Laboratory
Alenia Spazio
Polytechnic University of Milan
Massachusetts Institute of Technology
University of Pavia
University of Zielona Gora
Agenzia nazionale per le nuove tecnologie, l'energia e lo sviluppo economico sostenibile
NASA Marshall Space Flight Center
University of Gothenburg
Sabanci University
University of Palermo
University of Padua
LAM
Middle East Technical University
Observatoire Astronomique de Strasbourg
University of Cagliari
Czech Academy of Sciences
University of Cambridge
University of Southampton
CEA Saclay
Hebrew University of Jerusalem
Durham University
University of Ferrara
ISSI Bern
University of Leicester
Japan Aerospace Exploration Agency
ASI
FINCA
UJF Grenoble 1 CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), UMR 5274
Max Planck Institute for Extraterrestrial Physics
Friedrich-Alexander University Erlangen-Nürnberg
Johns Hopkins University
University of Crete
University of Calgary
Harvard-Smithsonian Ctr. Astrophys.
University of Groningen
University of Maryland, College Park
University of Alberta
University of Oulu
Space Research Centre
University of Arizona
Foundation for Research and Technology-Hellas
Cornell University
University of Galway
Aristotle University of Thessaloniki
Silesian University in Opava
ICREA

Research output: Contribution to journal › Article › peer-review

196 Scopus citations

Abstract

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 m ²-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 m ² (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 <260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength.

Original language	English
Pages (from-to)	415-444
Number of pages	30
Journal	Experimental Astronomy
Volume	34
Issue number	2
DOIs	https://doi.org/10.1007/s10686-011-9237-2
State	Published - Oct 2012

Keywords

Missions
X-ray timing
black holes
compact objects
neutron stars

Access to Document

10.1007/s10686-011-9237-2

Cite this

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., ... Ziolkowski, J. (2012). The Large Observatory for X-ray Timing (LOFT). Experimental Astronomy, 34(2), 415-444. https://doi.org/10.1007/s10686-011-9237-2

@article{447544bec30f49d0920925ea52f8a397,

title = "The Large Observatory for X-ray Timing (LOFT)",

abstract = "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 m 2-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 \textasciitilde{}12 m 2 (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 <260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength.",

keywords = "Missions, X-ray timing, black holes, compact objects, neutron stars",

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

year = "2012",

month = oct,

doi = "10.1007/s10686-011-9237-2",

language = "English",

volume = "34",

pages = "415--444",

journal = "Experimental Astronomy",

issn = "0922-6435",

number = "2",

}

Feroci, M, Stella, L, van der Klis, M, Courvoisier, TJL, 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, JW, Huovelin, J, Israel, GL, 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, MA, Alpar, MA, Altamirano, D, Alvarez, JM, Amati, L, Amoros, C, Antonelli, LA, 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, GA, Casella, P, Chaty, S, Chenevez, J, Coe, MJ, Collura, A, Corongiu, A, Covino, S, Cusumano, G, 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, JL, 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, JJM, 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, JM, 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, MC, Mineo, T, Morelli, E, Morsink, S, Motch, C, Motta, S, Muñoz-Darias, T, Naletto, G, Neustroev, V, Nevalainen, J, Olive, JF, 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, PO, 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, PJ, 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 2012, 'The Large Observatory for X-ray Timing (LOFT)', Experimental Astronomy, vol. 34, no. 2, pp. 415-444. https://doi.org/10.1007/s10686-011-9237-2

TY - JOUR

T1 - The Large Observatory for X-ray Timing (LOFT)

AU - Feroci, M.

AU - Stella, L.

AU - van der Klis, M.

AU - Courvoisier, T. J.L.

AU - Hernanz, M.

AU - Hudec, R.

AU - Santangelo, A.

AU - Walton, D.

AU - Zdziarski, A.

AU - Barret, D.

AU - Belloni, T.

AU - Braga, J.

AU - Brandt, S.

AU - Budtz-Jørgensen, C.

AU - Campana, S.

AU - den Herder, J. W.

AU - Huovelin, J.

AU - Israel, G. L.

AU - Pohl, M.

AU - Ray, P.

AU - Vacchi, A.

AU - Zane, S.

AU - Argan, A.

AU - Attinà, P.

AU - Bertuccio, G.

AU - Bozzo, E.

AU - Campana, R.

AU - Chakrabarty, D.

AU - Costa, E.

AU - de Rosa, A.

AU - Del Monte, E.

AU - Di Cosimo, S.

AU - Donnarumma, I.

AU - Evangelista, Y.

AU - Haas, D.

AU - Jonker, P.

AU - Korpela, S.

AU - Labanti, C.

AU - Malcovati, P.

AU - Mignani, R.

AU - Muleri, F.

AU - Rapisarda, M.

AU - Rashevsky, A.

AU - Rea, N.

AU - Rubini, A.

AU - Tenzer, C.

AU - Wilson-Hodge, C.

AU - Winter, B.

AU - Wood, K.

AU - Zampa, G.

AU - Zampa, N.

AU - Abramowicz, M. A.

AU - Alpar, M. A.

AU - Altamirano, D.

AU - Alvarez, J. M.

AU - Amati, L.

AU - Amoros, C.

AU - Antonelli, L. A.

AU - Artigue, R.

AU - Azzarello, P.

AU - Bachetti, M.

AU - Baldazzi, G.

AU - Barbera, M.

AU - Barbieri, C.

AU - Basa, S.

AU - Baykal, A.

AU - Belmont, R.

AU - Boirin, L.

AU - Bonvicini, V.

AU - Burderi, L.

AU - Bursa, M.

AU - Cabanac, C.

AU - Cackett, E.

AU - Caliandro, G. A.

AU - Casella, P.

AU - Chaty, S.

AU - Chenevez, J.

AU - Coe, M. J.

AU - Collura, A.

AU - Corongiu, A.

AU - Covino, S.

AU - Cusumano, G.

AU - D'Amico, F.

AU - Dall'Osso, S.

AU - de Martino, D.

AU - de Paris, G.

AU - Di Persio, G.

AU - Di Salvo, T.

AU - Done, C.

AU - Dovčiak, M.

AU - Drago, A.

AU - Ertan, U.

AU - Fabiani, S.

AU - Falanga, M.

AU - Fender, R.

AU - Ferrando, P.

AU - della Monica Ferreira, D.

AU - Fraser, G.

AU - Frontera, F.

AU - Fuschino, F.

AU - Galvez, J. L.

AU - Gandhi, P.

AU - Giommi, P.

AU - Godet, O.

AU - Göǧüş, E.

AU - Goldwurm, A.

AU - Götz, D.

AU - Grassi, M.

AU - Guttridge, P.

AU - Hakala, P.

AU - Henri, G.

AU - Hermsen, W.

AU - Horak, J.

AU - Hornstrup, A.

AU - in't Zand, J. J.M.

AU - Isern, J.

AU - Kalemci, E.

AU - Kanbach, G.

AU - Karas, V.

AU - Kataria, D.

AU - Kennedy, T.

AU - Klochkov, D.

AU - Kluźniak, W.

AU - Kokkotas, K.

AU - Kreykenbohm, I.

AU - Krolik, J.

AU - Kuiper, L.

AU - Kuvvetli, I.

AU - Kylafis, N.

AU - Lattimer, J. M.

AU - Lazzarotto, F.

AU - Leahy, D.

AU - Lebrun, F.

AU - Lin, D.

AU - Lund, N.

AU - Maccarone, T.

AU - Malzac, J.

AU - Marisaldi, M.

AU - Martindale, A.

AU - Mastropietro, M.

AU - McClintock, J.

AU - McHardy, I.

AU - Mendez, M.

AU - Mereghetti, S.

AU - Miller, M. C.

AU - Mineo, T.

AU - Morelli, E.

AU - Morsink, S.

AU - Motch, C.

AU - Motta, S.

AU - Muñoz-Darias, T.

AU - Naletto, G.

AU - Neustroev, V.

AU - Nevalainen, J.

AU - Olive, J. F.

AU - Orio, M.

AU - Orlandini, M.

AU - Orleanski, P.

AU - Ozel, F.

AU - Pacciani, L.

AU - Paltani, S.

AU - Papadakis, I.

AU - Papitto, A.

AU - Patruno, A.

AU - Pellizzoni, A.

AU - Petráček, V.

AU - Petri, J.

AU - Petrucci, P. O.

AU - Phlips, B.

AU - Picolli, L.

AU - Possenti, A.

AU - Psaltis, D.

AU - Rambaud, D.

AU - Reig, P.

AU - Remillard, R.

AU - Rodriguez, J.

AU - Romano, P.

AU - Romanova, M.

AU - Schanz, T.

AU - Schmid, C.

AU - Segreto, A.

AU - Shearer, A.

AU - Smith, A.

AU - Smith, P. J.

AU - Soffitta, P.

AU - Stergioulas, N.

AU - Stolarski, M.

AU - Stuchlik, Z.

AU - Tiengo, A.

AU - Torres, D.

AU - Török, G.

AU - Turolla, R.

AU - Uttley, P.

AU - Vaughan, S.

AU - Vercellone, S.

AU - Waters, R.

AU - Watts, A.

AU - Wawrzaszek, R.

AU - Webb, N.

AU - Wilms, J.

AU - Zampieri, L.

AU - Zezas, A.

AU - Ziolkowski, J.

PY - 2012/10

Y1 - 2012/10

N2 - 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 m 2-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 m 2 (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 <260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength.

AB - 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 m 2-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 m 2 (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 <260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength.

KW - Missions

KW - X-ray timing

KW - black holes

KW - compact objects

KW - neutron stars

UR - https://www.scopus.com/pages/publications/84866887519

U2 - 10.1007/s10686-011-9237-2

DO - 10.1007/s10686-011-9237-2

M3 - Article

AN - SCOPUS:84866887519

SN - 0922-6435

VL - 34

SP - 415

EP - 444

JO - Experimental Astronomy

JF - Experimental Astronomy

IS - 2

ER -

The Large Observatory for X-ray Timing (LOFT)

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