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The Cherenkov Telescope Array potential for the study of young supernova remnants

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...

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Authors

B.S. Acharya

C. Aramo

A. Babic

J.A. Barrio

A. Baushev

J. Becker Tjus

D. Berge

M. Bohacova

A. Bonardi

A. Brown

V. Bugaev

T. Bulik

M. Burton

G. Busetto

P. Caraveo

R. Carosi

J. Carr

J. Chudoba

V. Conforti

V. Connaughton

J.L. Contreras

G. Cotter

F. Dazzi

A. De Franco

I. de la Calle

R. de los Reyes Lopez

B. De Lotto

F. De Palma

T. Di Girolamo

C. Di Giulio

F. Di Pierro

J.-L. Dournaux

V. Dwarkadas

J. Ebr

K. Egberts

M. Fesquet

H. Fleischhack

L. Font

G. Fontaine

A. Förster

M. Fuessling

B. Garcia

R. Garcia López

M. Garczarczyk

F. Gargano

D. Garrido

M. Gaug

N. Giglietto

F. Giordano

A. Giuliani

N. Godinovic

M.M. Gonzalez

T. Grabarczyk

T. Hassan

J. Hörandel

M. Hrabovsky

D. Hrupec

T.B. Humensky

J. Huovelin

M. Jamrozy

P. Janecek

P.E. Kaaret

U. Katz

S. Kaufmann

B. Khélifi

W. Kluźniak

J. Kocot

N. Komin

H. Kubo

J. Kushida

G. Lamanna

W.H. Lee

J.-P. Lenain

T. Lohse

S. Lombardi

R. López-Coto

A. López-Oramas

F. Lucarelli

M.C. Maccarone

G. Maier

P. Majumdar

G. Malaguti

D. Mandat

M.N. Mazziotta

K. Meagher

N. Mirabal

A. Morselli

E. Moulin

J. Niemiec

M. Nievas

K. Nishijima

D. Nosek

F. Nunio

M. Ohishi

S. Ohm

R.A. Ong

R. Orito

N. Otte

M. Palatka

G. Pareschi

M. Pech

M. Persic

M. Pohl

M. Prouza

A. Quirrenbach

S. Rainó

G. Rodriguez Fernandez

P. Romano

A.C. Rovero

B. Rudak

P. Schovanek

M. Shayduk

H. Siejkowski

A. Sillanpää

S. Stefanik

T. Stolarczyk

M. Szanecki

T. Szepieniec

L.A. Tejedor

I. Telezhinsky

M. Teshima

L. Tibaldo

O. Tibolla

G. Tovmassian

P. Travnicek

M. Trzeciak

P. Vallania

C. van Eldik

S. Vercellone

C. Vigorito

S.J. Wagner

S.P. Wakely

A. Weinstein

A. Wierzcholska

A. Wilhelm

P. Wojcik

T. Yoshikoshi



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 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.

Journal Article Type Article
Acceptance Date Aug 30, 2014
Online Publication Date Sep 28, 2014
Publication Date Mar 1, 2015
Deposit Date Apr 15, 2015
Publicly Available Date Jun 1, 2018
Journal Astroparticle Physics
Print ISSN 0927-6505
Publisher Elsevier
Peer Reviewed Peer Reviewed
Volume 62
Pages 152-164
DOI https://doi.org/10.1016/j.astropartphys.2014.08.005
Keywords Acceleration of particles, Gamma rays, General, ISM: Supernova remnants, Radiation mechanisms: Non-termal.
Public URL https://durham-repository.worktribe.com/output/1442701

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