Acharya, B. S.; Aramo, C.; Babic, A.; Barrio, J. A.; Baushev, A.; Becker Tjus, J.; Berge, D.; Bohacova, M.; Bonardi, A.; Brown, A.; Bugaev, V.; Bulik, T.; Burton, M.; Busetto, G.; Caraveo, P.; Carosi, R.; Carr, J.; Chadwick, P.; Chudoba, J.; Conforti, V.; Connaughton, V.; Contreras, J. L.; Cotter, G.; Dazzi, F.; De Franco, A.; de la Calle, I.; de los Reyes Lopez, R.; De Lotto, B.; De Palma, F.; Di Girolamo, T.; Di Giulio, C.; Di Pierro, F.; Dournaux, J.-L.; Dwarkadas, V.; Ebr, J.; Egberts, K.; Fesquet, M.; Fleischhack, H.; Font, L.; Fontaine, G.; Förster, A.; Fuessling, M.; Garcia, B.; Garcia López, R.; Garczarczyk, M.; Gargano, F.; Garrido, D.; Gaug, M.; Giglietto, N.; Giordano, F.; Giuliani, A.; Godinovic, N.; Gonzalez, M. M.; Grabarczyk, T.; Hassan, T.; Hörandel, J.; Hrabovsky, M.; Hrupec, D.; Humensky, T. B.; Huovelin, J.; Jamrozy, M.; Janecek, P.; Kaaret, P. E.; Katz, U.; Kaufmann, S.; Khélifi, B.; Kluźniak, W.; Kocot, J.; Komin, N.; Kubo, H.; Kushida, J.; Lamanna, G.; Lee, W. H.; Lenain, J.-P.; Lohse, T.; Lombardi, S.; López-Coto, R.; López-Oramas, A.; Lucarelli, F.; Maccarone, M. C.; Maier, G.; Majumdar, P.; Malaguti, G.; Mandat, D.; Mazziotta, M. N.; Meagher, K.; Mirabal, N.; Morselli, A.; Moulin, E.; Niemiec, J.; Nievas, M.; Nishijima, K.; Nosek, D.; Nunio, F.; Ohishi, M.; Ohm, S.; Ong, R. A.; Orito, R.; Otte, N.; Palatka, M. et al.
Referencia bibliográfica
Astroparticle Physics, Volume 62, p. 152-164.
Fecha de publicación:
3
2015
Revista
Número de citas
6
Número de citas referidas
5
Descripción
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 2000 years 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.
Proyectos relacionados
Astrofísica de Partículas
El Grupo de Astrofísica de Partículas del IAC participa activamente en tres grandes colaboraciones internacionales de astrofísica de muy altas energías: AMS (Alpha Magnetic Spectrometer), los telescopios de radiación Cherenkov MAGIC I y II, y el Cherenkov Telescope Array (CTA). AMS es un detector de partículas diseñado para operar en el espacio, a
Ramón
García López