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Start Over Author "De Martino D" Publisher escholarship, university of california
4 results on '"De Martino D"'

1. Science with e-ASTROGAM A space mission for MeV–GeV gamma-ray astrophysics

Author

De Angelis, A, Tatischeff, V, Grenier, IA, McEnery, J, Mallamaci, M, Tavani, M, Oberlack, U, Hanlon, L, Walter, R, Argan, A, Von Ballmoos, P, Bulgarelli, A, Bykov, A, Hernanz, M, Kanbach, G, Kuvvetli, I, Pearce, M, Zdziarski, A, Conrad, J, Ghisellini, G, Harding, A, Isern, J, Leising, M, Longo, F, Madejski, G, Martinez, M, Mazziotta, MN, Paredes, JM, Pohl, M, Rando, R, Razzano, M, Aboudan, A, Ackermann, M, Addazi, A, Ajello, M, Albertus, C, Álvarez, JM, Ambrosi, G, Antón, S, Antonelli, LA, Babic, A, Baibussinov, B, Balbo, M, Baldini, L, Balman, S, Bambi, C, de Almeida, U Barres, Barrio, JA, Bartels, R, Bastieri, D, Bednarek, W, Bernard, D, Bernardini, E, Bernasconi, T, Bertucci, B, Biland, A, Bissaldi, E, Boettcher, M, Bonvicini, V, Bosch-Ramon, V, Bottacini, E, Bozhilov, V, Bretz, T, Branchesi, M, Brdar, V, Bringmann, T, Brogna, A, Jørgensen, C Budtz, Busetto, G, Buson, S, Busso, M, Caccianiga, A, Camera, S, Campana, R, Caraveo, P, Cardillo, M, Carlson, P, Celestin, S, Cermeño, M, Chen, A, Cheung, CC, Churazov, E, Ciprini, S, Coc, A, Colafrancesco, S, Coleiro, A, Collmar, W, Coppi, P, da Silva, R Curado, Cutini, S, D'Ammando, F, De Lotto, B, de Martino, D, De Rosa, A, Del Santo, M, Delgado, L, Diehl, R, Dietrich, S, Dolgov, AD, and Domínguez, A

Subjects
astro-ph.HE, astro-ph.IM, astro-ph.SR, hep-ex
Abstract

e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV–GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA.

Published
2018

2. XIPE: the x-ray imaging polarimetry explorer

Author

Soffitta, Paolo, Bellazzini, Ronaldo, Bozzo, Enrico, Burwitz, Vadim, Castro Tirado, Alberto, Costa, Enrico, Courvoisier, Thierry, Feng, Hua, Gburek, Szymon, Goosmann, Rene', Karas, Vladimir, Matt, Giorgio, Muleri, Fabio, Nandra, Kirpal, Pearce, Mark, Poutanen, Juri, Reglero, Victor, Graziati, Maria Dolores, Santangelo, Andrea, Tagliaferri, Gianpiero, Tenzer, Christopher, Vink, Jacco, Weisskopf, Martin, Zane, Silvia, Agudo, I, Antonelli, A, Attina, P, Baldini, L, Bykov, A, Carpentiero, R, Cavazzuti, E, Churazov, E, Del Monte, E, De Martino, D, Donnarumma, I, Doroshenko, V, Evangelista, Y, Ferreira, I, Gallo, E, Grosso, N, Kaaret, P, Kuulkers, E, Laranaga, J, Latronico, L, Lumb, DH, Macian, J, Malzac, J, Marin, F, Massaro, E, Minuti, M, Mundell, C, Ness, JU, Oosterbroek, T, Paltani, S, Pareschi, G, Perna, R, Petrucci, P-O, Pinazo, HB, Pinchera, M, Rodriguez, JP, Roncadelli, M, Santovincenzo, A, Sazonov, S, Sgro, C, Spiga, D, Svoboda, J, Theobald, C, Theodorou, T, Turolla, R, Wilhelmi de Ona, E, Winter, B, Akbar, AM, Allan, H, Aloisio, R, Altamirano, D, Amati, L, Amato, E, Angelakis, E, Arezu, J, Atteia, J-L, Axelsson, M, Bachetti, M, Ballo, L, Balman, S, Bandiera, R, Barcons, X, Basso, S, Baykal, A, Becker, W, Behar, E, Beheshtipour, B, Belmont, R, Berger, E, Bernardini, F, Bianchi, S, Bisnovatyi-Kogan, G, Blasi, P, Blay, P, Bodaghee, A, and Boer, M

Subjects
X-ray Astronomy, Polarimetry, X-ray optics, Gas Pixel Detector
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

3. XIPE: The X-ray imaging polarimetry explorer

Author

Soffitta, P, Bellazzini, R, Bozzo, E, Burwitz, V, Castro-Tirado, AJ, Costa, E, Courvoisier, T, Feng, H, Gburek, S, Goosmann, R, Karas, V, Matt, G, Muleri, F, Nandra, K, Pearce, M, Poutanen, J, Reglero, V, Sabau Maria, D, Santangelo, A, Tagliaferri, G, Tenzer, C, Vink, J, Weisskopf, MC, Zane, S, Agudo, I, Antonelli, A, Attina, P, Baldini, L, Bykov, A, Carpentiero, R, Cavazzuti, E, Churazov, E, Del Monte, E, De Martino, D, Donnarumma, I, Doroshenko, V, Evangelista, Y, Ferreira, I, Gallo, E, Grosso, N, Kaaret, P, Kuulkers, E, Laranaga, J, Latronico, L, Lumb, DH, Macian, J, Malzac, J, Marin, F, Massaro, E, Minuti, M, Mundell, C, Ness, JU, Oosterbroek, T, Paltani, S, Pareschi, G, Perna, R, Petrucci, PO, Pinazo, HB, Pinchera, M, Rodriguez, JP, Roncadelli, M, Santovincenzo, A, Sazonov, S, Sgro, C, Spiga, D, Svoboda, J, Theobald, C, Theodorou, T, Turolla, R, Wilhelmi De Ona, E, Winter, B, Akbar, AM, Allan, H, Aloisio, R, Altamirano, D, Amati, L, Amato, E, Angelakis, E, Arezu, J, Atteia, JL, Axelsson, M, Bachetti, M, Ballo, L, Balman, S, Bandiera, R, Barcons, X, Basso, S, Baykal, A, Becker, W, Behar, E, Beheshtipour, B, Belmont, R, Berger, E, Bernardini, F, Bianchi, S, Bisnovatyi-Kogan, G, Blasi, P, Blay, P, Bodaghee, A, and Boer, M

Subjects
X-ray Astronomy, Polarimetry, X-ray optics, Gas Pixel Detector
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

4. The Large Observatory for x-ray timing

Author

Feroci, M, Herder, JW den, Bozzo, E, Barret, D, Brandt, S, Hernanz, M, van der Klis, M, Pohl, M, Santangelo, A, Stella, L, Watts, A, Wilms, J, Zane, S, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J-L, Azzarello, P, Bakala, P, Baldazzi, G, Balman, S, Barbera, M, van Baren, C, Bhattacharyya, S, Baykal, A, Belloni, T, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bodin, P, Bombaci, I, Bidaud, J-M Bonnet, Boutloukos, S, Bradley, L, Braga, J, Brown, E, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jørgensen, C, Cackett, E, Cadoux, FR, Caïs, P, Caliandro, GA, Campana, R, Campana, S, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, AJ, Cavazzuti, E, Cerda-Duran, P, Chakrabarty, D, Château, F, Chenevez, J, Coker, J, Cole, R, Collura, A, Cornelisse, R, Courvoisier, T, Cros, A, Cumming, A, Cusumano, G, D'Ai, A, D'Elia, V, Del Monte, E, de Luca, A, de Martino, D, Dercksen, JPC, de Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Diebold, S, Di Salvo, T, Donnarumma, I, Drago, A, Durant, M, Emmanoulopoulos, D, Erkut, MH, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, and Favre, Y

Subjects
X-ray timing, X-ray spectroscopy, X-ray imaging, compact objects, X-ray detectors, microchannel plates, astro-ph.IM
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.

Published
2014

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