Evidence for Proton Acceleration up to TeV Energies Based on VERITAS and Fermi-LAT Observations of the Cas A SNR

Abeysekara, A. U.; Archer, A.; Benbow, W.; Bird, R.; Brose, Robert; Buchovecky, M.; Buckley, J. H.; Chromey, Alisha; Cui, Wei; Daniel, M. K.; Das, Samata; Dwarkadas, Vikram V.; Falcone, A.; Feng, Q.; Finley, J. P.; Fortson, L.; Gent, A.; Gillanders, G. H.; Giuri, C.; Gueta, O.; Hanna, D.; Hassan, Tarek; Hervet, O.; Holder, J.; Hughes, G.; Humensky, T. B.; Kaaret, Philip; Kar, P.; Kelley-Hoskins, N.; Kertzman, M.; Kieda, D.; Krause, M.; Krennrich, F.; Kumar, S.; Lang, M. J.; Maier, G.; Moriarty, P.; Mukherjee, R.; Rosillo, M. Nievas; O’Brien, S.; Ong, R. A.; Park, N.; Petrashyk, A.; Pfrang, K.; Pohl, Martin; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Richards, G.; Roache, E.; Sadeh, I.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Sushch, I.; Weinstein, A.; Wilcox, P.; Wilhelm, A.; Williams, D. A.; Williamson, T. J.; Zitzer, B.; Ghiotto, Augusto

doi:10.3847/1538-4357/ab8310

Cited by 58 publications

(44 citation statements)

References 70 publications

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“…The magnetic field is generally stronger for a RSG progenitor than for a WR, and we should expect stronger synchrotron cooling in the SNRs of RSG explosions. Even after the transition to the weaker field in the SW, about 1 µG, the downstream magnetic field remains at the level of several hundreds µG, as is observed in Cas A (Cowsik & Sarkar 1980;Abeysekara et al 2020).…”

Section: Magnetic Fieldmentioning

confidence: 60%

Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field

Sushch,

Brose,

Pohl

et al. 2021

Preprint

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The very-high-energy (VHE; E > 100 GeV) gamma-ray emission observed from a number of Supernova remnants (SNRs) indicates particle acceleration to high energies at the shock of the remnants and a potentially significant contribution to Galactic cosmic rays. It is extremely difficult to determine whether protons (through hadronic interactions and subsequent pion decay) or electrons (through inverse Compton scattering on ambient photon fields) are responsible for this emission. For a successful diagnostic, a good understanding of the spatial and energy distribution of the underlying particle population is crucial. Most SNRs are created in core-collapse explosions and expand into the wind bubble of their progenitor stars. This circumstellar medium features a complex spatial distribution of gas and magnetic field which naturally strongly affects the resulting particle population. In this work, we conduct a detailed study of the spectro-spatial evolution of the electrons accelerated at the forward shock of core-collapse SNRs and their non-thermal radiation, using the RATPaC code that is designed for the time-and spatially dependent treatment of particle acceleration at SNR shocks. We focus on the impact of the spatially inhomogeneous magnetic field through the efficiency of diffusion and synchrotron cooling. It is demonstrated that the structure of the circumstellar magnetic field can leave strong signatures in the spectrum and morphology of the resulting non-thermal emission.

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Section: Magnetic Fieldmentioning

confidence: 60%

Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field

Sushch,

Brose,

Pohl

et al. 2021

Preprint

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show abstract

“…Meanwhile, panel (b) shows the observed γ-ray SEDs of a few core-collapse SNRs. Indeed, we can see that very young objects like Cas A do exhibit a relatively flat spectrum (Acciari et al 2010;Yuan et al 2013;Ahnen et al 2017;Abeysekara et al 2020), while SNRs of a few 1,000 yrs old like RX J1713.7-3946 (Abdo et al 2011;H. E. S. S. Collaboration et al 2018), Vela Jr (Tanaka et al 2011;H.E.S.S.…”

Section: Spectral Propertiesmentioning

confidence: 93%

Resurrection of Non-thermal Emissions from Type Ib/c Supernova Remnants

Yasuda,

Lee,

Maeda

2021

Preprint

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Supernova remnants (SNRs) are important objects in investigating the links among supernova (SN) explosion mechanism(s), progenitor stars, and cosmic-ray acceleration. Non-thermal emission from SNRs is an effective and promising tool for probing their surrounding circumstellar media (CSM) and, in turn, the stellar evolution and mass-loss mechanism(s) of massive stars. In this work, we calculate the time evolution of broadband non-thermal emissions from Type Ib/c SNRs whose CSM structures are derived from the mass-loss history of their progenitors. Our results predict that Type Ib/c SNRs make a transition of brightness in radio and γ-ray bands from an undetectable dark for a certain period to a re-brightening phase. This transition originates from their inhomogeneous CSM structures in which the SNRs are embedded within a low-density wind cavity surrounded by a high-density wind shell and the ambient interstellar medium (ISM). The "resurrection" in non-thermal luminosity happens at an age of ∼1,000 yrs old for a Wolf-Rayet star progenitor evolved within a typical ISM density. Combining with the results of Type II SNR evolution recently reported by Yasuda et al. (2021), this result sheds light on a comprehensive understanding of non-thermal emissions from SNRs with different SN progenitor types and ages, which is made possible for the first time by the incorporation of realistic mass-loss histories of the progenitors.

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“…Although some authors usually take pmax = 10 15.5 eV/c, corresponding to the break in the locally observed CR energy spectrum known as "the knee", we note that no SNR has been proven to accelerate particles to these energies and, somewhat surprisingly, even young SNRs show TeV spectra that instead cutoff at very low energies compared to those expected from CRs reaching the knee. A famous example of an SNR that could be near the Sedov-Taylor phase is Cas A, which shows a cutoff in its TeV spectrum around 2.3 TeV (Abeysekara et al 2020). We therefore take pmax in the range 40-100 TeV c −1 , as required by our fits to the data.…”

Section: Cr Illumination From Puppis Amentioning

confidence: 99%

Probing the origin of 4FGL J0822.8-4207: cosmic ray illumination from the SNR Puppis A and the Herbig-Haro object HH219

Araya,

Gutiérrez,

Kerby

2021

Preprint

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4FGL J0822.8-4207 is a point source found in the 4FGL-DR2 catalog by the gammaray observatory Fermi-LAT and has no known association. We carry out X-ray observations of 4FGL J0822.8-4207 to help understand its nature. We explore two scenarios for the origin of 4FGL J0822.8-4207 . In the first case we study the possibility that cosmic rays from the supernova remnant (SNR) Puppis A, seen nearby in the sky, reach the dense gas at the location of the source and produce the gamma-rays through inelastic proton-proton collisions. We apply a standard model for particle diffusion in the interstellar medium and derive the required physical parameters. We find that this scenario for the gamma rays is possible if the gas is located at a distance that is not higher than ∼ 40 pc from Puppis A, unless the SNR is older than 7 kyr or the diffusion coefficient is higher than typical Galactic values, and relatively low-energy cosmic rays are currently escaping from the SNR. In the second scenario, we consider the protostellar jet HH219 as the origin of the GeV source and find the very interesting possibility that particles could be accelerated up to energies of at least several TeV in HH219. This would make this system the first known of its kind to produce gamma-ray emission extending up to hundreds of GeV without any apparent cutoff and an excellent laboratory to study the process of particle acceleration.

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Evidence for Proton Acceleration up to TeV Energies Based on VERITAS and Fermi-LAT Observations of the Cas A SNR

Cited by 58 publications

References 70 publications

Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field

Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field

Resurrection of Non-thermal Emissions from Type Ib/c Supernova Remnants

Probing the origin of 4FGL J0822.8-4207: cosmic ray illumination from the SNR Puppis A and the Herbig-Haro object HH219

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