LOFT: a large observatory for x-ray timing

Feroci, M.; Herder, J. den; Bozzo, E.; Barret, D.; Brandt, S.; Hernanz, M.; Klis, M. van der; Pohl, M.; Santangelo, A.; Stella, L.; Watts, Anna L.; Wilms, J.; Zane, S.; Ahangarianabhari, M.; Alpar, A.; Altamirano, D.; Álvarez, Laura; Amati, L.; Amoros, C.; Andersson, Nils; Antonelli, A.; Argan, A.; Artigue, R.; Azzarello, P.; Baldazzi, G.; Balman, Ş.; Barbera, Marco; Belloni, T.; Bertuccio, G.; Bianchi, S.; Bianchini, A.; Bodin, P.; Bidaud, J.-M. Bonnet; Boutloukos, Stratos; Braga, J.; Brown, Edward F.; Bucciantini, N.; Burderi, L.; Burša, Milan; rgensen, C Budtz-JA; Cackett, E.; Cadoux, FR; Caïs, Philippe; Caliandro, GA; Campana, R.; Campana, S.; Casella, P.; Chakrabarty, Deepto; Chenevez, J.; Coker, J.; Cole, Richard E.; Collura, A.; Courvoisier, T.; Cros, A.; Cumming, Andrew; Cusumano, G.; D'aa, A; Delia,; Monte, E. Del; Martino, D. de; Rosa, A. De; Cosimo, Sergio Di; Diebold, S.; Di., Salvo T.; Donnarumma, I.; Drago, A.; Durant, Martin; Emmanoulopoulos, D.; Evangelista, Y.; Fabian, A.; Falanga, M.; Favre, Y.; Feldman, Charlotte; Ferrigno, C.; Finger, M.; Fraser, G. W.; Fuschino, F.; Galloway, DK; Sanchez, J. L. Galvez; Garcı́a–Berro, E.; Gendre, B.; Gezari, Suvi; Giles, AB; Gilfanov, M.; Giommi, P.; Giovannini, G.; Giroletti, M.; Goldwurm, A.; Götz, D.; Gouiffès, C.; Grassi, M.; Groot, P.; Guidorzi, C.; Haas, D.; Hansen, Flemming Thorbjørn; Hartmann, D. H.; Haswell, C. A.; Heger, Alexander; Henning, W.; Homan, J.; Hornstrup, A.; Hudec, R.; Huovelin, J.; Ingram, Adam; Zand, Jjm in 't; Isern, J.; Israel, G. L.; Izzo, L.; Jonker, P. G.; Kaaret, P.; Karas,; Karelin, D.; Kataria, D. O.; Keek, L.; Kennedy, T.; Klochkov, D.; Kluźniak, W.; Kokkotas, Kostas D.; Korpela, Seppo A.; Kouveliotou, C.; Kreykenbohm, I.; Kuiper, LM; Kuvvetli, I.; Labanti, C.; Lai, Dong; Lamb, F. K.; Lebrun, F.; Linder, Dietmar; Lodato, Giuseppe; Longo, F.; Lund, N.; Maccarone, T. J.; Macera, D.; Malcovati, P.; Mangano,; Manousakis, A.; Marisaldi, M.; Markowitz, A.; Martindale, A.; Matt, Giorgio; McHardy, I. M.; Melatos, A.; Méndez, Mariano; Migliari, S.; Mignani, Roberto; Miller, C. J.; Miller, J. M.; Mineo, T.; Miniutti, G.; Morsink, Sharon M.; Motch, C.; Motta, S.; Mouchet, M.; Muleri, Fabio; Norton, A. J.; Nowak, Michael A.; O’Brien, P.; Orienti, M.; Orio, Marina; Orlandini, M.; Orleaski, P; Osborne, J. P.; Osten, Rachel A.; Özel, Feryal; Pacciani, L.; Papitto, A.; Paul, Bikash Chandra; Perinati, E.; Petracek,; Portell, J.; Poutanen, Juri; Psaltis, Dimitrios; Rambaud, D.; Ramsay, Gavin; Rapisarda, M.; Rachevski, A.; Ray, Paul S.; Rea, N.; Reddy, Sanjay; Reig, P.; Aranda, M. Reina; Remillard, Ron; Rodríguez‐Gil, P.; Rodríguez, J.; Romano, P.; Rossi, Emr; Ryde, F.; Graziati, Sabau; Sala, G.; Salvaterra, R.; Sanna, A.; Schanne, S.; Schanz, T.; Schee, Jan; Schmid, Christian; Schwenk, A.; Schwope, A.; Seyler, J.-Y.; Shearer, A.; Smith, A.; Smith, David M.; Smith, P. G.; Sochora,; Soffitta, P.; Soleri, P.; Stappers, B. W.; Stelzer, B.; Stergioulas, Nikolaos; Stratta, G.; Strohmayer, TE; Stuchlík, Zdeněk; Suchy, S.; Sulemainov,; Takahashi, Tomohiro; Tamburini, Fabrizio; Tenzer, C.; Tolós, Laura; Török, Gabriel; Torrejon, JM; Torres, DF; Tramacere, A.; Trois, A.; Turriziani, S.; Uter, P.; Uttley, P.; Vacchi, A.; Varnière, P.; Vaughan, S.; Vercellone, S.; Vrba,; Walton, D.; Watanabe, Shigeto; Wawrzaszek, R.; Webb, N.; Weinberg, Nevin N.; Wheatley, S; Wijers, R. A. M. J.; Wijnands, Rad; Wille, M.; Wilson-Hodge, C.; Winter, B.; Wood, K. S.; Zampa, G.; Zampa, N.; Zampieri, L.; Zdziarski, A. A.; Zhang, B

doi:10.1117/12.857337

Cited by 10 publications

(4 citation statements)

References 23 publications

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“…LOFT [5] is devoted to study matter in extreme states such as those found at the event horizon of black holes or the surface of neutron stars. These sources exhibit rapid luminosity changes and spectral variability in the X-ray region, providing the key scientific justification for the Large Area Detector [LAD; 21] one of the two core scientific instruments proposed for LOFT.…”

Section: Introductionmentioning

confidence: 99%

Effects of capillary reflection in the performance of the collimator of the Large Area Detector on board LOFT

et al. 2013

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The Large Observatory For X-ray Timing (LOFT) is one of the candidate missions selected by the European Space Agency for an initial assessment phase in the Cosmic Vision programme. It is proposed for the M3 launch slot and has broad scientific goals related to fast timing of astrophysical X-ray sources. LOFT will carry the Large Area Detector (LAD), as one of the two core science instruments, necessary to achieve the challenging objectives of the project. LAD is a collimated detector working in the energy range 2-50 keV with an effective area of approximately 10 m 2 at 8 keV. The instrument comprises an array of modules located on deployable panels. Lead-glass microchannel plate (MCP) collimators are located in front of the large-area Silicon Drift Detectors (SDD) to reduce the background contamination from off-axis resolved point sources and from the diffuse X-ray background. The inner walls of the microchannel plate pores reflect grazing incidence X-ray photons with a probability that depends on energy. In this paper, we present a study performed with an ad-hoc simulator of the effects of this capillary reflectivity on the overall instrument performance. The reflectiv-On behalf of LOFT collaboration T. 2 Teresa Mineo et al.ity is derived from a limited set of laboratory measurements, used to constrain the model. The measurements were taken using a prototype collimator whose thickness is similar to that adopted in the current baseline design proposed for the LAD. We find that the experimentally measured level of reflectivity of the pore inner walls enhances the off-axis transmission at low energies, producing an almost flat-top response. The resulting background increase due to the diffuse cosmic X-ray emission and sources within the field of view does not degrade the instrument sensitivity.

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Section: Introductionmentioning

confidence: 99%

Effects of capillary reflection in the performance of the collimator of the Large Area Detector on board LOFT

et al. 2013

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“…Among them, the 6th Japanese X-ray satellite ASTRO-H, to be launched in 2014, is the next major international X-ray mission which will be operated as an observatory. Much larger missions, such as Athena [8] and LOFT [9], have been proposed for the 2020's.…”

Section: Future X-ray Missionsmentioning

confidence: 99%

Multiwavelength Astronomy and CTA: X-rays

Takahashi

Uchiyama

Stawarz

2013

Astroparticle Physics

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We discuss how future X-ray instruments which are under development can contribute to our understanding of the non-thermal Universe. Much progress has been made in the field of X-ray Astronomy recently, thanks to the operation of modern X-ray telescopes such as Chandra, XMM-Newton, Suzaku, and Swift, but more in-depth investigation awaits future missions. These future missions include ASTROSAT, NuStar, e-ROSITA, ASTRO-H and GEMS, which will be realized in the next decade, and also much larger projects such as Athena and LOFT, which have been proposed for the 2020's. All of those are expected to bring a variety of novel observational results regarding astrophysical sources of high-energy particles and radiation, i.e. supernova remnants, neutron stars, stellar-mass black holes, active galaxies, and clusters of galaxies among others. The operation of the future X-ray instruments will proceed in parallel with the operation of Fermi-LAT and the Cherenkov Telescope Array. We emphasize that the synergy between the X-ray and gamma-ray observations is particularly important, and that the planned X-ray missions, when in conjunction with the modern gamma-ray observatories, will indeed provide a qualitatively better insight into the high-energy Universe.Comment: 18 pages, 15 figures. Accepted for publication in the Astroparticle Physics, Special Issue on Physics with the Cherenkov Telescope Array (editors: J. Hinton, S. Sarkar, & D.F. Torres

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“…We discussed in [9] whether the proposed Large Observatory for X-ray Timing (LOFT), [10,11], will have the necessary capability to reconstruct the parameters from a model spectrum. We produced artificial data with appropriate properties and then we analyzed them by using a preliminary response file for LOFT.…”

Section: Introductionmentioning

confidence: 99%

Beyond the Standard Model of the Disc–line Spectral Profiles From Black Hole Accretion Discs

et al. 2014

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Abstract. The strong gravitational field of a black hole has distinct effects on the observed profile of a spectral line from an accretion disc near a black hole. The observed profile of the spectral line is broadened and skewed by a fast orbital motion and redshifted by a gravitational field. These effects can help us to constrain the parameters of a system with a black hole, both in active galactic nuclei and in a stellar-mass black hole. Here we explore the fact that an accretion disc emission can be mathematically imagined as a superposition of radiating accretion rings that extend from the inner edge to the outer rim of the disc, with some radially varying emissivity. In our work, we show that a characteristic double-horn profile of several radially confined (relatively narrow) accretion rings or belts could be recognized by the planned instruments onboard future satellites (such as the proposed ESA Large Observatory for X-ray Timing).

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LOFT: a large observatory for x-ray timing

Cited by 10 publications

References 23 publications

Effects of capillary reflection in the performance of the collimator of the Large Area Detector on board LOFT

Effects of capillary reflection in the performance of the collimator of the Large Area Detector on board LOFT

Multiwavelength Astronomy and CTA: X-rays

Beyond the Standard Model of the Disc–line Spectral Profiles From Black Hole Accretion Discs

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