Constraining the Origin of the Puzzling Source HESS J1640−465 and the PeVatron Candidate HESS J1641−463 Using Fermi-Large Area Telescope Observations
| Autor: | M.-H. Grondin, Fabio Acero, C. J. Clark, M. Lemoine-Goumard, J. D. Gelfand, J. Devin, Arnaud Mares, Dave Green, S. Gabici |
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| Přispěvatelé: | Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Mares, A [0000-0003-3345-7800], Lemoine-Goumard, M [0000-0002-4462-3686], Clark, CJ [0000-0003-4355-3572], Gelfand, JD [0000-0003-4679-1058], Green, DA [0000-0003-3189-9998], Grondin, MH [0000-0002-8383-251X], Apollo - University of Cambridge Repository, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ANR-17-CE31-0014,PECORA,Rayons Cosmiques au PeV(2017) |
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Astrophysics::High Energy Astrophysical Phenomena
Cosmic ray Astrophysics::Cosmology and Extragalactic Astrophysics GeV power spectrum 01 natural sciences GLAST VHE law.invention Telescope particle: acceleration Pulsar law HESS 0103 physical sciences supernova cloud flux: upper limit 010303 astronomy & astrophysics X-ray: flux Astrophysics::Galaxy Astrophysics pulsar Physics astro-ph.HE cosmic radiation: spectrum 010308 nuclear & particles physics Astronomy Astronomy and Astrophysics Gamma-ray astronomy 13. Climate action Space and Planetary Science gamma ray curvature spectral High Energy Physics::Experiment galaxy [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Fermi Gamma-ray Space Telescope |
| Zdroj: | Astrophys.J. Astrophys.J., 2021, 912 (2), pp.158. ⟨10.3847/1538-4357/abef62⟩ |
| DOI: | 10.3847/1538-4357/abef62⟩ |
| Popis: | There are only a few very-high-energy sources in our Galaxy that might accelerate particles up to the knee of the cosmic-ray spectrum. To understand the mechanisms of particle acceleration in these PeVatron candidates, Fermi-Large Area Telescope (LAT) and High-Energy Stereoscopic System (H.E.S.S.) observations are essential to characterize their γ-ray emission. HESS J1640–465 and the PeVatron candidate HESS J1641–463 are two neighboring (0.25°) γ-ray sources, spatially coincident with the radio supernova remnants (SNRs) G338.3–0.0 and G338.5+0.1. Detected both by H.E.S.S. and the Fermi-LAT, we present here a morphological and spectral analysis of these two sources using 8 yr of Fermi-LAT data between 200 MeV and 1 TeV with multiwavelength observations to assess their nature. The morphology of HESS J1640–465 is described by a 2D Gaussian (σ = 0.053° ± 0.011°stat ± 0.03°syst) and its spectrum is modeled by a power law with a spectral index Γ = 1.8 ± 0.1stat ± 0.2syst. HESS J1641–463 is detected as a point-like source and its GeV emission is described by a logarithmic-parabola spectrum with α = 2.7 ± 0.1stat ± 0.2syst and significant curvature of β = 0.11 ± 0.03stat ± 0.05syst. Radio and X-ray flux upper limits were derived. We investigated scenarios to explain their emission, namely, the emission from accelerated particles within the SNRs spatially coincident with each source, molecular clouds illuminated by cosmic rays from the close-by SNRs, and a pulsar/pulsar wind nebula origin. Our new Fermi-LAT results and the radio and flux X-ray upper limits pose severe constraints on some of these models. |
| Databáze: | OpenAIRE |
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