The Cherenkov Telescope Array potential for the study of young supernova remnants
Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Acharya, B.S. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015transfer abstract |
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| Schlagwörter: |
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| Umfang: |
13 |
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| Übergeordnetes Werk: |
Enthalten in: Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells - 2012transfer abstract, Amsterdam [u.a.] |
|---|---|
| Übergeordnetes Werk: |
volume:62 ; year:2015 ; pages:152-164 ; extent:13 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.astropartphys.2014.08.005 |
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| Katalog-ID: |
ELV029097657 |
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| 245 | 1 | 4 | |a The Cherenkov Telescope Array potential for the study of young supernova remnants |
| 264 | 1 | |c 2015transfer abstract | |
| 300 | |a 13 | ||
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| 520 | |a Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. | ||
| 520 | |a Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. | ||
| 650 | 7 | |a ISM: Supernova remnants |2 Elsevier | |
| 650 | 7 | |a Radiation mechanisms: Non-termal |2 Elsevier | |
| 650 | 7 | |a Gamma rays: General |2 Elsevier | |
| 650 | 7 | |a Acceleration of particles |2 Elsevier | |
| 700 | 1 | |a Aramo, C. |4 oth | |
| 700 | 1 | |a Babic, A. |4 oth | |
| 700 | 1 | |a Barrio, J.A. |4 oth | |
| 700 | 1 | |a Baushev, A. |4 oth | |
| 700 | 1 | |a Becker Tjus, J. |4 oth | |
| 700 | 1 | |a Berge, D. |4 oth | |
| 700 | 1 | |a Bohacova, M. |4 oth | |
| 700 | 1 | |a Bonardi, A. |4 oth | |
| 700 | 1 | |a Brown, A. |4 oth | |
| 700 | 1 | |a Bugaev, V. |4 oth | |
| 700 | 1 | |a Bulik, T. |4 oth | |
| 700 | 1 | |a Burton, M. |4 oth | |
| 700 | 1 | |a Busetto, G. |4 oth | |
| 700 | 1 | |a Caraveo, P. |4 oth | |
| 700 | 1 | |a Carosi, R. |4 oth | |
| 700 | 1 | |a Carr, J. |4 oth | |
| 700 | 1 | |a Chadwick, P. |4 oth | |
| 700 | 1 | |a Chudoba, J. |4 oth | |
| 700 | 1 | |a Conforti, V. |4 oth | |
| 700 | 1 | |a Connaughton, V. |4 oth | |
| 700 | 1 | |a Contreras, J.L. |4 oth | |
| 700 | 1 | |a Cotter, G. |4 oth | |
| 700 | 1 | |a Dazzi, F. |4 oth | |
| 700 | 1 | |a De Franco, A. |4 oth | |
| 700 | 1 | |a de la Calle, I. |4 oth | |
| 700 | 1 | |a de los Reyes Lopez, R. |4 oth | |
| 700 | 1 | |a De Lotto, B. |4 oth | |
| 700 | 1 | |a De Palma, F. |4 oth | |
| 700 | 1 | |a Di Girolamo, T. |4 oth | |
| 700 | 1 | |a Di Giulio, C. |4 oth | |
| 700 | 1 | |a Di Pierro, F. |4 oth | |
| 700 | 1 | |a Dournaux, J.-L. |4 oth | |
| 700 | 1 | |a Dwarkadas, V. |4 oth | |
| 700 | 1 | |a Ebr, J. |4 oth | |
| 700 | 1 | |a Egberts, K. |4 oth | |
| 700 | 1 | |a Fesquet, M. |4 oth | |
| 700 | 1 | |a Fleischhack, H. |4 oth | |
| 700 | 1 | |a Font, L. |4 oth | |
| 700 | 1 | |a Fontaine, G. |4 oth | |
| 700 | 1 | |a Förster, A. |4 oth | |
| 700 | 1 | |a Fuessling, M. |4 oth | |
| 700 | 1 | |a Garcia, B. |4 oth | |
| 700 | 1 | |a Garcia López, R. |4 oth | |
| 700 | 1 | |a Garczarczyk, M. |4 oth | |
| 700 | 1 | |a Gargano, F. |4 oth | |
| 700 | 1 | |a Garrido, D. |4 oth | |
| 700 | 1 | |a Gaug, M. |4 oth | |
| 700 | 1 | |a Giglietto, N. |4 oth | |
| 700 | 1 | |a Giordano, F. |4 oth | |
| 700 | 1 | |a Giuliani, A. |4 oth | |
| 700 | 1 | |a Godinovic, N. |4 oth | |
| 700 | 1 | |a Gonzalez, M.M. |4 oth | |
| 700 | 1 | |a Grabarczyk, T. |4 oth | |
| 700 | 1 | |a Hassan, T. |4 oth | |
| 700 | 1 | |a Hörandel, J. |4 oth | |
| 700 | 1 | |a Hrabovsky, M. |4 oth | |
| 700 | 1 | |a Hrupec, D. |4 oth | |
| 700 | 1 | |a Humensky, T.B. |4 oth | |
| 700 | 1 | |a Huovelin, J. |4 oth | |
| 700 | 1 | |a Jamrozy, M. |4 oth | |
| 700 | 1 | |a Janecek, P. |4 oth | |
| 700 | 1 | |a Kaaret, P.E. |4 oth | |
| 700 | 1 | |a Katz, U. |4 oth | |
| 700 | 1 | |a Kaufmann, S. |4 oth | |
| 700 | 1 | |a Khélifi, B. |4 oth | |
| 700 | 1 | |a Kluźniak, W. |4 oth | |
| 700 | 1 | |a Kocot, J. |4 oth | |
| 700 | 1 | |a Komin, N. |4 oth | |
| 700 | 1 | |a Kubo, H. |4 oth | |
| 700 | 1 | |a Kushida, J. |4 oth | |
| 700 | 1 | |a Lamanna, G. |4 oth | |
| 700 | 1 | |a Lee, W.H. |4 oth | |
| 700 | 1 | |a Lenain, J.-P. |4 oth | |
| 700 | 1 | |a Lohse, T. |4 oth | |
| 700 | 1 | |a Lombardi, S. |4 oth | |
| 700 | 1 | |a López-Coto, R. |4 oth | |
| 700 | 1 | |a López-Oramas, A. |4 oth | |
| 700 | 1 | |a Lucarelli, F. |4 oth | |
| 700 | 1 | |a Maccarone, M.C. |4 oth | |
| 700 | 1 | |a Maier, G. |4 oth | |
| 700 | 1 | |a Majumdar, P. |4 oth | |
| 700 | 1 | |a Malaguti, G. |4 oth | |
| 700 | 1 | |a Mandat, D. |4 oth | |
| 700 | 1 | |a Mazziotta, M.N. |4 oth | |
| 700 | 1 | |a Meagher, K. |4 oth | |
| 700 | 1 | |a Mirabal, N. |4 oth | |
| 700 | 1 | |a Morselli, A. |4 oth | |
| 700 | 1 | |a Moulin, E. |4 oth | |
| 700 | 1 | |a Niemiec, J. |4 oth | |
| 700 | 1 | |a Nievas, M. |4 oth | |
| 700 | 1 | |a Nishijima, K. |4 oth | |
| 700 | 1 | |a Nosek, D. |4 oth | |
| 700 | 1 | |a Nunio, F. |4 oth | |
| 700 | 1 | |a Ohishi, M. |4 oth | |
| 700 | 1 | |a Ohm, S. |4 oth | |
| 700 | 1 | |a Ong, R.A. |4 oth | |
| 700 | 1 | |a Orito, R. |4 oth | |
| 700 | 1 | |a Otte, N. |4 oth | |
| 700 | 1 | |a Palatka, M. |4 oth | |
| 700 | 1 | |a Pareschi, G. |4 oth | |
| 700 | 1 | |a Pech, M. |4 oth | |
| 700 | 1 | |a Persic, M. |4 oth | |
| 700 | 1 | |a Pohl, M. |4 oth | |
| 700 | 1 | |a Prouza, M. |4 oth | |
| 700 | 1 | |a Quirrenbach, A. |4 oth | |
| 700 | 1 | |a Rainó, S. |4 oth | |
| 700 | 1 | |a Rodriguez Fernandez, G. |4 oth | |
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| 700 | 1 | |a Rovero, A.C. |4 oth | |
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| 700 | 1 | |a Schovanek, P. |4 oth | |
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| 700 | 1 | |a Tejedor, L.A. |4 oth | |
| 700 | 1 | |a Telezhinsky, I. |4 oth | |
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| 700 | 1 | |a Tibaldo, L. |4 oth | |
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| 700 | 1 | |a Wagner, S.J. |4 oth | |
| 700 | 1 | |a Wakely, S.P. |4 oth | |
| 700 | 1 | |a Weinstein, A. |4 oth | |
| 700 | 1 | |a Wierzcholska, A. |4 oth | |
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10.1016/j.astropartphys.2014.08.005 doi GBV00000000000235A.pica (DE-627)ELV029097657 (ELSEVIER)S0927-6505(14)00129-7 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Acharya, B.S. verfasserin aut The Cherenkov Telescope Array potential for the study of young supernova remnants 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. ISM: Supernova remnants Elsevier Radiation mechanisms: Non-termal Elsevier Gamma rays: General Elsevier Acceleration of particles Elsevier Aramo, C. oth Babic, A. oth Barrio, J.A. oth Baushev, A. oth Becker Tjus, J. oth Berge, D. oth Bohacova, M. oth Bonardi, A. oth Brown, A. oth Bugaev, V. oth Bulik, T. oth Burton, M. oth Busetto, G. oth Caraveo, P. oth Carosi, R. oth Carr, J. oth Chadwick, P. oth Chudoba, J. oth Conforti, V. oth Connaughton, V. oth Contreras, J.L. oth Cotter, G. oth Dazzi, F. oth De Franco, A. oth de la Calle, I. oth de los Reyes Lopez, R. oth De Lotto, B. oth De Palma, F. oth Di Girolamo, T. oth Di Giulio, C. oth Di Pierro, F. oth Dournaux, J.-L. oth Dwarkadas, V. oth Ebr, J. oth Egberts, K. oth Fesquet, M. oth Fleischhack, H. oth Font, L. oth Fontaine, G. oth Förster, A. oth Fuessling, M. oth Garcia, B. oth Garcia López, R. oth Garczarczyk, M. oth Gargano, F. oth Garrido, D. oth Gaug, M. oth Giglietto, N. oth Giordano, F. oth Giuliani, A. oth Godinovic, N. oth Gonzalez, M.M. oth Grabarczyk, T. oth Hassan, T. oth Hörandel, J. oth Hrabovsky, M. oth Hrupec, D. oth Humensky, T.B. oth Huovelin, J. oth Jamrozy, M. oth Janecek, P. oth Kaaret, P.E. oth Katz, U. oth Kaufmann, S. oth Khélifi, B. oth Kluźniak, W. oth Kocot, J. oth Komin, N. oth Kubo, H. oth Kushida, J. oth Lamanna, G. oth Lee, W.H. oth Lenain, J.-P. oth Lohse, T. oth Lombardi, S. oth López-Coto, R. oth López-Oramas, A. oth Lucarelli, F. oth Maccarone, M.C. oth Maier, G. oth Majumdar, P. oth Malaguti, G. oth Mandat, D. oth Mazziotta, M.N. oth Meagher, K. oth Mirabal, N. oth Morselli, A. oth Moulin, E. oth Niemiec, J. oth Nievas, M. oth Nishijima, K. oth Nosek, D. oth Nunio, F. oth Ohishi, M. oth Ohm, S. oth Ong, R.A. oth Orito, R. oth Otte, N. oth Palatka, M. oth Pareschi, G. oth Pech, M. oth Persic, M. oth Pohl, M. oth Prouza, M. oth Quirrenbach, A. oth Rainó, S. oth Rodriguez Fernandez, G. oth Romano, P. oth Rovero, A.C. oth Rudak, B. oth Schovanek, P. oth Shayduk, M. oth Siejkowski, H. oth Sillanpää, A. oth Stefanik, S. oth Stolarczyk, T. oth Szanecki, M. oth Szepieniec, T. oth Tejedor, L.A. oth Telezhinsky, I. oth Teshima, M. oth Tibaldo, L. oth Tibolla, O. oth Tovmassian, G. oth Travnicek, P. oth Trzeciak, M. oth Vallania, P. oth van Eldik, C. oth Vercellone, S. oth Vigorito, C. oth Wagner, S.J. oth Wakely, S.P. oth Weinstein, A. oth Wierzcholska, A. oth Wilhelm, A. oth Wojcik, P. oth Yoshikoshi, T. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:62 year:2015 pages:152-164 extent:13 https://doi.org/10.1016/j.astropartphys.2014.08.005 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 62 2015 152-164 13 045F 540 |
| spelling |
10.1016/j.astropartphys.2014.08.005 doi GBV00000000000235A.pica (DE-627)ELV029097657 (ELSEVIER)S0927-6505(14)00129-7 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Acharya, B.S. verfasserin aut The Cherenkov Telescope Array potential for the study of young supernova remnants 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. ISM: Supernova remnants Elsevier Radiation mechanisms: Non-termal Elsevier Gamma rays: General Elsevier Acceleration of particles Elsevier Aramo, C. oth Babic, A. oth Barrio, J.A. oth Baushev, A. oth Becker Tjus, J. oth Berge, D. oth Bohacova, M. oth Bonardi, A. oth Brown, A. oth Bugaev, V. oth Bulik, T. oth Burton, M. oth Busetto, G. oth Caraveo, P. oth Carosi, R. oth Carr, J. oth Chadwick, P. oth Chudoba, J. oth Conforti, V. oth Connaughton, V. oth Contreras, J.L. oth Cotter, G. oth Dazzi, F. oth De Franco, A. oth de la Calle, I. oth de los Reyes Lopez, R. oth De Lotto, B. oth De Palma, F. oth Di Girolamo, T. oth Di Giulio, C. oth Di Pierro, F. oth Dournaux, J.-L. oth Dwarkadas, V. oth Ebr, J. oth Egberts, K. oth Fesquet, M. oth Fleischhack, H. oth Font, L. oth Fontaine, G. oth Förster, A. oth Fuessling, M. oth Garcia, B. oth Garcia López, R. oth Garczarczyk, M. oth Gargano, F. oth Garrido, D. oth Gaug, M. oth Giglietto, N. oth Giordano, F. oth Giuliani, A. oth Godinovic, N. oth Gonzalez, M.M. oth Grabarczyk, T. oth Hassan, T. oth Hörandel, J. oth Hrabovsky, M. oth Hrupec, D. oth Humensky, T.B. oth Huovelin, J. oth Jamrozy, M. oth Janecek, P. oth Kaaret, P.E. oth Katz, U. oth Kaufmann, S. oth Khélifi, B. oth Kluźniak, W. oth Kocot, J. oth Komin, N. oth Kubo, H. oth Kushida, J. oth Lamanna, G. oth Lee, W.H. oth Lenain, J.-P. oth Lohse, T. oth Lombardi, S. oth López-Coto, R. oth López-Oramas, A. oth Lucarelli, F. oth Maccarone, M.C. oth Maier, G. oth Majumdar, P. oth Malaguti, G. oth Mandat, D. oth Mazziotta, M.N. oth Meagher, K. oth Mirabal, N. oth Morselli, A. oth Moulin, E. oth Niemiec, J. oth Nievas, M. oth Nishijima, K. oth Nosek, D. oth Nunio, F. oth Ohishi, M. oth Ohm, S. oth Ong, R.A. oth Orito, R. oth Otte, N. oth Palatka, M. oth Pareschi, G. oth Pech, M. oth Persic, M. oth Pohl, M. oth Prouza, M. oth Quirrenbach, A. oth Rainó, S. oth Rodriguez Fernandez, G. oth Romano, P. oth Rovero, A.C. oth Rudak, B. oth Schovanek, P. oth Shayduk, M. oth Siejkowski, H. oth Sillanpää, A. oth Stefanik, S. oth Stolarczyk, T. oth Szanecki, M. oth Szepieniec, T. oth Tejedor, L.A. oth Telezhinsky, I. oth Teshima, M. oth Tibaldo, L. oth Tibolla, O. oth Tovmassian, G. oth Travnicek, P. oth Trzeciak, M. oth Vallania, P. oth van Eldik, C. oth Vercellone, S. oth Vigorito, C. oth Wagner, S.J. oth Wakely, S.P. oth Weinstein, A. oth Wierzcholska, A. oth Wilhelm, A. oth Wojcik, P. oth Yoshikoshi, T. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:62 year:2015 pages:152-164 extent:13 https://doi.org/10.1016/j.astropartphys.2014.08.005 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 62 2015 152-164 13 045F 540 |
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10.1016/j.astropartphys.2014.08.005 doi GBV00000000000235A.pica (DE-627)ELV029097657 (ELSEVIER)S0927-6505(14)00129-7 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Acharya, B.S. verfasserin aut The Cherenkov Telescope Array potential for the study of young supernova remnants 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. ISM: Supernova remnants Elsevier Radiation mechanisms: Non-termal Elsevier Gamma rays: General Elsevier Acceleration of particles Elsevier Aramo, C. oth Babic, A. oth Barrio, J.A. oth Baushev, A. oth Becker Tjus, J. oth Berge, D. oth Bohacova, M. oth Bonardi, A. oth Brown, A. oth Bugaev, V. oth Bulik, T. oth Burton, M. oth Busetto, G. oth Caraveo, P. oth Carosi, R. oth Carr, J. oth Chadwick, P. oth Chudoba, J. oth Conforti, V. oth Connaughton, V. oth Contreras, J.L. oth Cotter, G. oth Dazzi, F. oth De Franco, A. oth de la Calle, I. oth de los Reyes Lopez, R. oth De Lotto, B. oth De Palma, F. oth Di Girolamo, T. oth Di Giulio, C. oth Di Pierro, F. oth Dournaux, J.-L. oth Dwarkadas, V. oth Ebr, J. oth Egberts, K. oth Fesquet, M. oth Fleischhack, H. oth Font, L. oth Fontaine, G. oth Förster, A. oth Fuessling, M. oth Garcia, B. oth Garcia López, R. oth Garczarczyk, M. oth Gargano, F. oth Garrido, D. oth Gaug, M. oth Giglietto, N. oth Giordano, F. oth Giuliani, A. oth Godinovic, N. oth Gonzalez, M.M. oth Grabarczyk, T. oth Hassan, T. oth Hörandel, J. oth Hrabovsky, M. oth Hrupec, D. oth Humensky, T.B. oth Huovelin, J. oth Jamrozy, M. oth Janecek, P. oth Kaaret, P.E. oth Katz, U. oth Kaufmann, S. oth Khélifi, B. oth Kluźniak, W. oth Kocot, J. oth Komin, N. oth Kubo, H. oth Kushida, J. oth Lamanna, G. oth Lee, W.H. oth Lenain, J.-P. oth Lohse, T. oth Lombardi, S. oth López-Coto, R. oth López-Oramas, A. oth Lucarelli, F. oth Maccarone, M.C. oth Maier, G. oth Majumdar, P. oth Malaguti, G. oth Mandat, D. oth Mazziotta, M.N. oth Meagher, K. oth Mirabal, N. oth Morselli, A. oth Moulin, E. oth Niemiec, J. oth Nievas, M. oth Nishijima, K. oth Nosek, D. oth Nunio, F. oth Ohishi, M. oth Ohm, S. oth Ong, R.A. oth Orito, R. oth Otte, N. oth Palatka, M. oth Pareschi, G. oth Pech, M. oth Persic, M. oth Pohl, M. oth Prouza, M. oth Quirrenbach, A. oth Rainó, S. oth Rodriguez Fernandez, G. oth Romano, P. oth Rovero, A.C. oth Rudak, B. oth Schovanek, P. oth Shayduk, M. oth Siejkowski, H. oth Sillanpää, A. oth Stefanik, S. oth Stolarczyk, T. oth Szanecki, M. oth Szepieniec, T. oth Tejedor, L.A. oth Telezhinsky, I. oth Teshima, M. oth Tibaldo, L. oth Tibolla, O. oth Tovmassian, G. oth Travnicek, P. oth Trzeciak, M. oth Vallania, P. oth van Eldik, C. oth Vercellone, S. oth Vigorito, C. oth Wagner, S.J. oth Wakely, S.P. oth Weinstein, A. oth Wierzcholska, A. oth Wilhelm, A. oth Wojcik, P. oth Yoshikoshi, T. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:62 year:2015 pages:152-164 extent:13 https://doi.org/10.1016/j.astropartphys.2014.08.005 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 62 2015 152-164 13 045F 540 |
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10.1016/j.astropartphys.2014.08.005 doi GBV00000000000235A.pica (DE-627)ELV029097657 (ELSEVIER)S0927-6505(14)00129-7 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Acharya, B.S. verfasserin aut The Cherenkov Telescope Array potential for the study of young supernova remnants 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. ISM: Supernova remnants Elsevier Radiation mechanisms: Non-termal Elsevier Gamma rays: General Elsevier Acceleration of particles Elsevier Aramo, C. oth Babic, A. oth Barrio, J.A. oth Baushev, A. oth Becker Tjus, J. oth Berge, D. oth Bohacova, M. oth Bonardi, A. oth Brown, A. oth Bugaev, V. oth Bulik, T. oth Burton, M. oth Busetto, G. oth Caraveo, P. oth Carosi, R. oth Carr, J. oth Chadwick, P. oth Chudoba, J. oth Conforti, V. oth Connaughton, V. oth Contreras, J.L. oth Cotter, G. oth Dazzi, F. oth De Franco, A. oth de la Calle, I. oth de los Reyes Lopez, R. oth De Lotto, B. oth De Palma, F. oth Di Girolamo, T. oth Di Giulio, C. oth Di Pierro, F. oth Dournaux, J.-L. oth Dwarkadas, V. oth Ebr, J. oth Egberts, K. oth Fesquet, M. oth Fleischhack, H. oth Font, L. oth Fontaine, G. oth Förster, A. oth Fuessling, M. oth Garcia, B. oth Garcia López, R. oth Garczarczyk, M. oth Gargano, F. oth Garrido, D. oth Gaug, M. oth Giglietto, N. oth Giordano, F. oth Giuliani, A. oth Godinovic, N. oth Gonzalez, M.M. oth Grabarczyk, T. oth Hassan, T. oth Hörandel, J. oth Hrabovsky, M. oth Hrupec, D. oth Humensky, T.B. oth Huovelin, J. oth Jamrozy, M. oth Janecek, P. oth Kaaret, P.E. oth Katz, U. oth Kaufmann, S. oth Khélifi, B. oth Kluźniak, W. oth Kocot, J. oth Komin, N. oth Kubo, H. oth Kushida, J. oth Lamanna, G. oth Lee, W.H. oth Lenain, J.-P. oth Lohse, T. oth Lombardi, S. oth López-Coto, R. oth López-Oramas, A. oth Lucarelli, F. oth Maccarone, M.C. oth Maier, G. oth Majumdar, P. oth Malaguti, G. oth Mandat, D. oth Mazziotta, M.N. oth Meagher, K. oth Mirabal, N. oth Morselli, A. oth Moulin, E. oth Niemiec, J. oth Nievas, M. oth Nishijima, K. oth Nosek, D. oth Nunio, F. oth Ohishi, M. oth Ohm, S. oth Ong, R.A. oth Orito, R. oth Otte, N. oth Palatka, M. oth Pareschi, G. oth Pech, M. oth Persic, M. oth Pohl, M. oth Prouza, M. oth Quirrenbach, A. oth Rainó, S. oth Rodriguez Fernandez, G. oth Romano, P. oth Rovero, A.C. oth Rudak, B. oth Schovanek, P. oth Shayduk, M. oth Siejkowski, H. oth Sillanpää, A. oth Stefanik, S. oth Stolarczyk, T. oth Szanecki, M. oth Szepieniec, T. oth Tejedor, L.A. oth Telezhinsky, I. oth Teshima, M. oth Tibaldo, L. oth Tibolla, O. oth Tovmassian, G. oth Travnicek, P. oth Trzeciak, M. oth Vallania, P. oth van Eldik, C. oth Vercellone, S. oth Vigorito, C. oth Wagner, S.J. oth Wakely, S.P. oth Weinstein, A. oth Wierzcholska, A. oth Wilhelm, A. oth Wojcik, P. oth Yoshikoshi, T. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:62 year:2015 pages:152-164 extent:13 https://doi.org/10.1016/j.astropartphys.2014.08.005 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 62 2015 152-164 13 045F 540 |
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10.1016/j.astropartphys.2014.08.005 doi GBV00000000000235A.pica (DE-627)ELV029097657 (ELSEVIER)S0927-6505(14)00129-7 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Acharya, B.S. verfasserin aut The Cherenkov Telescope Array potential for the study of young supernova remnants 2015transfer abstract 13 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. ISM: Supernova remnants Elsevier Radiation mechanisms: Non-termal Elsevier Gamma rays: General Elsevier Acceleration of particles Elsevier Aramo, C. oth Babic, A. oth Barrio, J.A. oth Baushev, A. oth Becker Tjus, J. oth Berge, D. oth Bohacova, M. oth Bonardi, A. oth Brown, A. oth Bugaev, V. oth Bulik, T. oth Burton, M. oth Busetto, G. oth Caraveo, P. oth Carosi, R. oth Carr, J. oth Chadwick, P. oth Chudoba, J. oth Conforti, V. oth Connaughton, V. oth Contreras, J.L. oth Cotter, G. oth Dazzi, F. oth De Franco, A. oth de la Calle, I. oth de los Reyes Lopez, R. oth De Lotto, B. oth De Palma, F. oth Di Girolamo, T. oth Di Giulio, C. oth Di Pierro, F. oth Dournaux, J.-L. oth Dwarkadas, V. oth Ebr, J. oth Egberts, K. oth Fesquet, M. oth Fleischhack, H. oth Font, L. oth Fontaine, G. oth Förster, A. oth Fuessling, M. oth Garcia, B. oth Garcia López, R. oth Garczarczyk, M. oth Gargano, F. oth Garrido, D. oth Gaug, M. oth Giglietto, N. oth Giordano, F. oth Giuliani, A. oth Godinovic, N. oth Gonzalez, M.M. oth Grabarczyk, T. oth Hassan, T. oth Hörandel, J. oth Hrabovsky, M. oth Hrupec, D. oth Humensky, T.B. oth Huovelin, J. oth Jamrozy, M. oth Janecek, P. oth Kaaret, P.E. oth Katz, U. oth Kaufmann, S. oth Khélifi, B. oth Kluźniak, W. oth Kocot, J. oth Komin, N. oth Kubo, H. oth Kushida, J. oth Lamanna, G. oth Lee, W.H. oth Lenain, J.-P. oth Lohse, T. oth Lombardi, S. oth López-Coto, R. oth López-Oramas, A. oth Lucarelli, F. oth Maccarone, M.C. oth Maier, G. oth Majumdar, P. oth Malaguti, G. oth Mandat, D. oth Mazziotta, M.N. oth Meagher, K. oth Mirabal, N. oth Morselli, A. oth Moulin, E. oth Niemiec, J. oth Nievas, M. oth Nishijima, K. oth Nosek, D. oth Nunio, F. oth Ohishi, M. oth Ohm, S. oth Ong, R.A. oth Orito, R. oth Otte, N. oth Palatka, M. oth Pareschi, G. oth Pech, M. oth Persic, M. oth Pohl, M. oth Prouza, M. oth Quirrenbach, A. oth Rainó, S. oth Rodriguez Fernandez, G. oth Romano, P. oth Rovero, A.C. oth Rudak, B. oth Schovanek, P. oth Shayduk, M. oth Siejkowski, H. oth Sillanpää, A. oth Stefanik, S. oth Stolarczyk, T. oth Szanecki, M. oth Szepieniec, T. oth Tejedor, L.A. oth Telezhinsky, I. oth Teshima, M. oth Tibaldo, L. oth Tibolla, O. oth Tovmassian, G. oth Travnicek, P. oth Trzeciak, M. oth Vallania, P. oth van Eldik, C. oth Vercellone, S. oth Vigorito, C. oth Wagner, S.J. oth Wakely, S.P. oth Weinstein, A. oth Wierzcholska, A. oth Wilhelm, A. oth Wojcik, P. oth Yoshikoshi, T. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:62 year:2015 pages:152-164 extent:13 https://doi.org/10.1016/j.astropartphys.2014.08.005 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 62 2015 152-164 13 045F 540 |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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Acharya, B.S. @@aut@@ Aramo, C. @@oth@@ Babic, A. @@oth@@ Barrio, J.A. @@oth@@ Baushev, A. @@oth@@ Becker Tjus, J. @@oth@@ Berge, D. @@oth@@ Bohacova, M. @@oth@@ Bonardi, A. @@oth@@ Brown, A. @@oth@@ Bugaev, V. @@oth@@ Bulik, T. @@oth@@ Burton, M. @@oth@@ Busetto, G. @@oth@@ Caraveo, P. @@oth@@ Carosi, R. @@oth@@ Carr, J. @@oth@@ Chadwick, P. @@oth@@ Chudoba, J. @@oth@@ Conforti, V. @@oth@@ Connaughton, V. @@oth@@ Contreras, J.L. @@oth@@ Cotter, G. @@oth@@ Dazzi, F. @@oth@@ De Franco, A. @@oth@@ de la Calle, I. @@oth@@ de los Reyes Lopez, R. @@oth@@ De Lotto, B. @@oth@@ De Palma, F. @@oth@@ Di Girolamo, T. @@oth@@ Di Giulio, C. @@oth@@ Di Pierro, F. @@oth@@ Dournaux, J.-L. @@oth@@ Dwarkadas, V. @@oth@@ Ebr, J. @@oth@@ Egberts, K. @@oth@@ Fesquet, M. @@oth@@ Fleischhack, H. @@oth@@ Font, L. @@oth@@ Fontaine, G. @@oth@@ Förster, A. @@oth@@ Fuessling, M. @@oth@@ Garcia, B. @@oth@@ Garcia López, R. @@oth@@ Garczarczyk, M. @@oth@@ Gargano, F. @@oth@@ Garrido, D. @@oth@@ Gaug, M. @@oth@@ Giglietto, N. @@oth@@ Giordano, F. @@oth@@ Giuliani, A. @@oth@@ Godinovic, N. @@oth@@ Gonzalez, M.M. @@oth@@ Grabarczyk, T. @@oth@@ Hassan, T. @@oth@@ Hörandel, J. @@oth@@ Hrabovsky, M. @@oth@@ Hrupec, D. @@oth@@ Humensky, T.B. @@oth@@ Huovelin, J. @@oth@@ Jamrozy, M. @@oth@@ Janecek, P. @@oth@@ Kaaret, P.E. @@oth@@ Katz, U. @@oth@@ Kaufmann, S. @@oth@@ Khélifi, B. @@oth@@ Kluźniak, W. @@oth@@ Kocot, J. @@oth@@ Komin, N. @@oth@@ Kubo, H. @@oth@@ Kushida, J. @@oth@@ Lamanna, G. @@oth@@ Lee, W.H. @@oth@@ Lenain, J.-P. @@oth@@ Lohse, T. @@oth@@ Lombardi, S. @@oth@@ López-Coto, R. @@oth@@ López-Oramas, A. @@oth@@ Lucarelli, F. @@oth@@ Maccarone, M.C. @@oth@@ Maier, G. @@oth@@ Majumdar, P. @@oth@@ Malaguti, G. @@oth@@ Mandat, D. @@oth@@ Mazziotta, M.N. @@oth@@ Meagher, K. @@oth@@ Mirabal, N. @@oth@@ Morselli, A. @@oth@@ Moulin, E. @@oth@@ Niemiec, J. @@oth@@ Nievas, M. @@oth@@ Nishijima, K. @@oth@@ Nosek, D. @@oth@@ Nunio, F. @@oth@@ Ohishi, M. @@oth@@ Ohm, S. @@oth@@ Ong, R.A. @@oth@@ Orito, R. @@oth@@ Otte, N. @@oth@@ Palatka, M. @@oth@@ Pareschi, G. @@oth@@ Pech, M. @@oth@@ Persic, M. @@oth@@ Pohl, M. @@oth@@ Prouza, M. @@oth@@ Quirrenbach, A. @@oth@@ Rainó, S. @@oth@@ Rodriguez Fernandez, G. @@oth@@ Romano, P. @@oth@@ Rovero, A.C. @@oth@@ Rudak, B. @@oth@@ Schovanek, P. @@oth@@ Shayduk, M. @@oth@@ Siejkowski, H. @@oth@@ Sillanpää, A. @@oth@@ Stefanik, S. @@oth@@ Stolarczyk, T. @@oth@@ Szanecki, M. @@oth@@ Szepieniec, T. @@oth@@ Tejedor, L.A. @@oth@@ Telezhinsky, I. @@oth@@ Teshima, M. @@oth@@ Tibaldo, L. @@oth@@ Tibolla, O. @@oth@@ Tovmassian, G. @@oth@@ Travnicek, P. @@oth@@ Trzeciak, M. @@oth@@ Vallania, P. @@oth@@ van Eldik, C. @@oth@@ Vercellone, S. @@oth@@ Vigorito, C. @@oth@@ Wagner, S.J. @@oth@@ Wakely, S.P. @@oth@@ Weinstein, A. @@oth@@ Wierzcholska, A. @@oth@@ Wilhelm, A. @@oth@@ Wojcik, P. @@oth@@ Yoshikoshi, T. @@oth@@ |
| publishDateDaySort_date |
2015-01-01T00:00:00Z |
| hierarchy_top_id |
ELV016257995 |
| dewey-sort |
3540 |
| id |
ELV029097657 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV029097657</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230625165833.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180603s2015 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.astropartphys.2014.08.005</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000235A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV029097657</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0927-6505(14)00129-7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">540</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">540</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">690</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">50.92</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Acharya, B.S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The Cherenkov Telescope Array potential for the study of young supernova remnants</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">13</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models.</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">ISM: Supernova remnants</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Radiation mechanisms: Non-termal</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Gamma rays: General</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Acceleration of particles</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Aramo, C.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Babic, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Barrio, 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The Cherenkov Telescope Array potential for the study of young supernova remnants |
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Acharya, B.S. |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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cherenkov telescope array potential for the study of young supernova remnants |
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The Cherenkov Telescope Array potential for the study of young supernova remnants |
| abstract |
Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. |
| abstractGer |
Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. |
| abstract_unstemmed |
Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. |
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The Cherenkov Telescope Array potential for the study of young supernova remnants |
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https://doi.org/10.1016/j.astropartphys.2014.08.005 |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV029097657</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230625165833.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180603s2015 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.astropartphys.2014.08.005</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000235A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV029097657</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0927-6505(14)00129-7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">540</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">540</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">690</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">50.92</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Acharya, B.S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The Cherenkov Telescope Array potential for the study of young supernova remnants</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">13</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models.</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">ISM: Supernova remnants</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Radiation mechanisms: Non-termal</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Gamma rays: General</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Acceleration of particles</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Aramo, C.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Babic, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Barrio, 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T.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Burton, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Busetto, G.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Caraveo, P.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Carosi, R.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Carr, J.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Chadwick, P.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Chudoba, J.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Conforti, V.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Connaughton, V.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Contreras, J.L.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Cotter, G.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Dazzi, F.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">De Franco, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">de la Calle, I.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">de los Reyes Lopez, R.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" 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ind2=" "><subfield code="a">Nievas, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Nishijima, K.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Nosek, D.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Nunio, F.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ohishi, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ohm, S.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ong, R.A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Orito, R.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" 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"><subfield code="a">Rainó, S.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rodriguez Fernandez, G.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Romano, P.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rovero, A.C.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rudak, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Schovanek, P.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Shayduk, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Siejkowski, H.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" 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