How Many Ultra-High Energy Cosmic Rays Could We Expect From Centaurus A?

Fraija, N.; González, M. M.; Pérez, Marina; Marinelli, A.

doi:10.1088/0004-637x/753/1/40

Cited by 27 publications

(44 citation statements)

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“…Due to photo-disintegration of Fe nuclei by 170 KeV photons we expect a peak in the high energy gamma ray spectrum at 400M eV . In [36] the authors have used the low energy photon spectrum from [40] for calculating the high energy gamma ray flux from the lobes of Cen A, but the low energy photon spectrum given in [40] is observed from the core of Cen A.…”

Section: Discussionmentioning

confidence: 99%

“…If the lower energy bound is 1 EeV then the estimated luminosity in the band of 1 EeV to 150 EeV is 5 × 10 40 erg/sec, which is below the bolometric luminosity 10 43 erg/sec of this source. Fraija et al [36] have explained the emission of gamma rays observed by HESS and the UHECR events observed by Pierre Auger with p − p interactions assuming the gamma ray emission is from the lobes of Cen A. They have shown that the scenario of p − γ interactions in their model is not consistent with the observational results.…”

Section: Introductionmentioning

confidence: 99%

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Testing hadronic models of gamma ray production at the core of Cen A

Joshi

Gupta

2013

Phys. Rev. D

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Pierre Auger experiment has observed a few cosmic ray events above 55 EeV from the direction of the core of Cen A. These cosmic rays might have originated from the core of Cen A. High energy gamma ray emission has been observed by HESS from the radio core and inner kpc jets of Cen A. We are testing whether pure hadronic interactions of protons or heavy nuclei with the matter in the core region or photo-disintegration of heavy nuclei can explain the cosmic ray and high energy gamma ray observations from the core of Cen A. The scenario of p − γ interactions followed by photo-pion decay has been tested earlier by Sahu et al. (2012) and found to be consistent with the observational results. In this paper we have considered some other possibilities (i) the primary cosmic rays at the core of Cen A are protons and the high energy gamma rays are produced in p − p interactions,(ii) the primary cosmic rays are Fe nuclei and the high energy gamma rays are produced in F e − p interactions and (iii) the primary cosmic rays are Fe nuclei and they are photo-disintegrated at the core. The daughter nuclei de-excite and high energy gamma rays are produced. The high energy gamma ray fluxes expected in each of these cases are compared with the flux observed by HESS experiment to normalise the spectrum of the primary cosmic rays at the core. We have calculated the expected number of cosmic ray nucleon events between 55 EeV and 150 EeV in each of these cases to verify the consistencies of the different scenarios with the observations by Pierre Auger experiment. We find that if the primary cosmic rays are Fe nuclei then their photo-disintegration followed by de-excitation of daughter nuclei may explain the observed high energy particle emissions from the core of Cen A. The luminosity of the cosmic ray Fe nuclei required to explain the observational results of HESS and Pierre Auger is higher than the luminosity of the cosmic ray protons in the pγ interaction model. The required cosmic ray luminosity depends on the density of the low energy photons at the source which photo-disintegrate the Fe nuclei and the size of the emitting region.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Testing hadronic models of gamma ray production at the core of Cen A

Joshi

Gupta

2013

Phys. Rev. D

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“…Hadronic interactions within the extended lobes have been proposed to produce gamma-rays in the GeV -TeV energy range [75]. Assuming that CRs are described by a simple power law,…”

Section: A3 Hadronic Interactionsmentioning

confidence: 99%

Analysis of Fermi-LAT observations, UHECRs and neutrinos from the radio galaxy Centaurus B

Fraija

Araya

Galván-Gaméz

et al. 2019

J. Cosmol. Astropart. Phys.

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Centaurus B (Cen B) is one of the closest and brightest radio-loud galaxy in the southern sky. This radio galaxy, proposed as a plausible candidate for accelerating ultra-high-energy cosmic rays (UHECRs), is near the highest-energy neutrino event reported (IC35) in the High-Energy Starting Events catalog. Pierre Auger observatory reported the highest energy comic rays during 10 years of collecting data with some of them around this source. In this paper, the analysis of the gamma-ray spectrum and the light curve above 200 MeV is presented with nine years of cumulative Fermi-LAT data around Cen B. Taking into consideration the multi-wavelength observations carried out about this radio galaxy, leptonic and hadronic scenarios are introduced in order to fit the spectral energy distribution, assuming that the gamma-ray flux is produced in a region close to the core and in the extended lobes. Using the best-fit values found, several physics properties of this radio galaxy are derived. Furthermore, a statistical analysis of the cosmic ray distribution around Cen B is performed, finding that this distribution is not different from the background at a level of significance of 5%. Considering the UHECR event associated to this source by Moskalenko et al.[1] and extrapolating its luminosity to low energies, we do not find enough evidence to associate the highest-energy neutrino event (IC35) with this radio galaxy.

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“…Taking into account the proton distribution (Eq. 2.1) and the conservation of the photo pion flux (Atoyan & Dermer 2003;Fraija et al 2012b;Aharonian 2002) where the proportionality constant of pp interaction is…”

Section: Vhe Neutrino Expectation From Fr Imentioning

confidence: 99%

Very high energy neutrino expectation from Fanaroff-Riley I sources

Marinelli

Fraija

2014

Proc. IAU

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Abstract. Fanaroff-Riley I radiogalaxies have been observed in TeV gamma-rays during the last decades. The origin of the emission processes related with this energy band is still under debate. Here we consider the case of the two closest Fanaroff-Riley I objects: Centaurus A and M87. Their entire broadband spectral energy distributions and variability fluxes show evidences that leptonic models are not sufficient to explain their fluxes above 100 GeV. Indeed, both objects have been imaged by LAT instrument aboard of Fermi telescope with measured spectra well connected with one-zone leptonic models. However, to explain the TeV spectra obtained with campaigns by H.E.S.S., for Centaurus A, and by VERITAS, MAGIC and H.E.S.S. for M87, different emission processes must be introduced. In this work we introduce hadronic scenarios to describe the TeV gamma-ray fluxes observed and to obtain the expected neutrino counterparts for each considered TeV campaign. With the obtained neutrino spectra we calculate, through Monte Carlo simulations, the expected neutrino event rate in a hypothetical Km 3 neutrino telescope and we compare the results with what has been observed by IceCube experiment up to now.

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How Many Ultra-High Energy Cosmic Rays Could We Expect From Centaurus A?

Cited by 27 publications

References 50 publications

Testing hadronic models of gamma ray production at the core of Cen A

Testing hadronic models of gamma ray production at the core of Cen A

Analysis of Fermi-LAT observations, UHECRs and neutrinos from the radio galaxy Centaurus B

Very high energy neutrino expectation from Fanaroff-Riley I sources

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