The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465

The supernova remnant (SNR) G338.3-0.0 spatially correlates with HESS J1640-465, which is considered the most luminous γ-ray source associated with a SNR in our Galaxy. The X-ray pulsar PSR J1640-4631 has been recently discovered within the SNR shell, which could favor a leptonic origin for the dete...

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Autores principales: Supan, L., Supanitsky, A.D., Castelletti, G.
Formato: JOUR
Materias:
Gamma rays: ISM
ISM: individual objects: SNR G338.3-0.0
ISM: supernova remnants
Pulsars
Supernovae
Emission mechanism
Gamma ray cross-section
Gamma rays: isms
ISM: individual objects
Proton proton collisions
Spectral energy distribution
Supernova remnants
Gamma rays
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v589_n_p_Supan
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_00046361_v589_n_p_Supan
record_format dspace
spelling todo:paper_00046361_v589_n_p_Supan2023-10-03T14:00:58Z The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465 Supan, L. Supanitsky, A.D. Castelletti, G. Gamma rays: ISM ISM: individual objects: SNR G338.3-0.0 ISM: supernova remnants Pulsars Supernovae Emission mechanism Gamma ray cross-section Gamma rays: isms ISM: individual objects ISM: supernova remnants Proton proton collisions Spectral energy distribution Supernova remnants Gamma rays The supernova remnant (SNR) G338.3-0.0 spatially correlates with HESS J1640-465, which is considered the most luminous γ-ray source associated with a SNR in our Galaxy. The X-ray pulsar PSR J1640-4631 has been recently discovered within the SNR shell, which could favor a leptonic origin for the detected very-high-energy (VHE) emission. In spite of this, the origin of the VHE radiation from HESS J1640-465 has not been unambiguously clarified so far. Indeed, a hadronic explanation cannot be ruled out by current observations. On the basis of atomic (HI) and molecular (12CO) archival data, we determine, for the first time, the total ambient density of protons in the region of the G338.3-0.0/HESS J1640-465 system, a critical parameter for understanding the emission mechanisms at very high energies. The value obtained is in the 100-130 cm-3 range. Besides this, we developed a new hadronic model to describe the spectral energy distribution (SED) of the HESS J1640-465 source, which includes the latest total γ-ray cross-section for proton-proton collisions available in the literature. By using the assessed ambient proton density, we found that the total energy in accelerated protons required to fit the data is 5.4+4.7 -2.3 ×1049 erg and 1.6+1.4 -0.7 ×1050 erg for a source distance of 8.5 and 13 kpc, respectively. The case where the source distance is 8.5 kpc agrees with the typical scenario in which the energy released is on the order of 1051 erg and ~10% of that energy is transferred to the accelerated protons, whereas the case corresponding to a source distance of 13 kpc requires either a higher value of the energy released in the explosion or a larger energy fraction to accelerate protons. © ESO, 2016. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v589_n_p_Supan
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Gamma rays: ISM
ISM: individual objects: SNR G338.3-0.0
ISM: supernova remnants
Pulsars
Supernovae
Emission mechanism
Gamma ray cross-section
Gamma rays: isms
ISM: individual objects
ISM: supernova remnants
Proton proton collisions
Spectral energy distribution
Supernova remnants
Gamma rays
spellingShingle Gamma rays: ISM
ISM: individual objects: SNR G338.3-0.0
ISM: supernova remnants
Pulsars
Supernovae
Emission mechanism
Gamma ray cross-section
Gamma rays: isms
ISM: individual objects
ISM: supernova remnants
Proton proton collisions
Spectral energy distribution
Supernova remnants
Gamma rays
Supan, L.
Supanitsky, A.D.
Castelletti, G.
The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
topic_facet Gamma rays: ISM
ISM: individual objects: SNR G338.3-0.0
ISM: supernova remnants
Pulsars
Supernovae
Emission mechanism
Gamma ray cross-section
Gamma rays: isms
ISM: individual objects
ISM: supernova remnants
Proton proton collisions
Spectral energy distribution
Supernova remnants
Gamma rays
description The supernova remnant (SNR) G338.3-0.0 spatially correlates with HESS J1640-465, which is considered the most luminous γ-ray source associated with a SNR in our Galaxy. The X-ray pulsar PSR J1640-4631 has been recently discovered within the SNR shell, which could favor a leptonic origin for the detected very-high-energy (VHE) emission. In spite of this, the origin of the VHE radiation from HESS J1640-465 has not been unambiguously clarified so far. Indeed, a hadronic explanation cannot be ruled out by current observations. On the basis of atomic (HI) and molecular (12CO) archival data, we determine, for the first time, the total ambient density of protons in the region of the G338.3-0.0/HESS J1640-465 system, a critical parameter for understanding the emission mechanisms at very high energies. The value obtained is in the 100-130 cm-3 range. Besides this, we developed a new hadronic model to describe the spectral energy distribution (SED) of the HESS J1640-465 source, which includes the latest total γ-ray cross-section for proton-proton collisions available in the literature. By using the assessed ambient proton density, we found that the total energy in accelerated protons required to fit the data is 5.4+4.7 -2.3 ×1049 erg and 1.6+1.4 -0.7 ×1050 erg for a source distance of 8.5 and 13 kpc, respectively. The case where the source distance is 8.5 kpc agrees with the typical scenario in which the energy released is on the order of 1051 erg and ~10% of that energy is transferred to the accelerated protons, whereas the case corresponding to a source distance of 13 kpc requires either a higher value of the energy released in the explosion or a larger energy fraction to accelerate protons. © ESO, 2016.
format JOUR
author Supan, L.
Supanitsky, A.D.
Castelletti, G.
author_facet Supan, L.
Supanitsky, A.D.
Castelletti, G.
author_sort Supan, L.
title The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
title_short The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
title_full The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
title_fullStr The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
title_full_unstemmed The environment of the γ-ray emitting SNR G338.3-0.0: A hadronic interpretation for HESS J1640-465
title_sort environment of the γ-ray emitting snr g338.3-0.0: a hadronic interpretation for hess j1640-465
url http://hdl.handle.net/20.500.12110/paper_00046361_v589_n_p_Supan
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