Identifying the counterpart of HESS J1858+020

Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar...

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Detalles Bibliográficos
Publicado:	2010
Materias:	Clouds - ISM Individual objects ISM ISM - ISM Supernova remnants - Gamma rays Clouds Elementary particles Signal to noise ratio Stars Clouds-ISM Supernova remnants Gamma rays
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v509_n1_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v509_n1_p_Paron
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046361_v509_n1_p_Paron
record_format	dspace
spelling	paper:paper_00046361_v509_n1_p_Paron2023-06-08T14:27:52Z Identifying the counterpart of HESS J1858+020 Clouds - ISM Individual objects ISM ISM - ISM Supernova remnants - Gamma rays Clouds Elementary particles Signal to noise ratio Stars Clouds-ISM Individual objects ISM ISM - ISM Supernova remnants Gamma rays Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission. Methods: Using the 13CO J = 1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4. Results. The 13CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ∼5 × 103 M⊙ and ∼500 cm -3 respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm-3 could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission. © ESO 2010. 2010 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v509_n1_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v509_n1_p_Paron
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Clouds - ISM Individual objects ISM ISM - ISM Supernova remnants - Gamma rays Clouds Elementary particles Signal to noise ratio Stars Clouds-ISM Individual objects ISM ISM - ISM Supernova remnants Gamma rays
spellingShingle	Clouds - ISM Individual objects ISM ISM - ISM Supernova remnants - Gamma rays Clouds Elementary particles Signal to noise ratio Stars Clouds-ISM Individual objects ISM ISM - ISM Supernova remnants Gamma rays Identifying the counterpart of HESS J1858+020
topic_facet	Clouds - ISM Individual objects ISM ISM - ISM Supernova remnants - Gamma rays Clouds Elementary particles Signal to noise ratio Stars Clouds-ISM Individual objects ISM ISM - ISM Supernova remnants Gamma rays
description	Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission. Methods: Using the 13CO J = 1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4. Results. The 13CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ∼5 × 103 M⊙ and ∼500 cm -3 respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm-3 could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission. © ESO 2010.
title	Identifying the counterpart of HESS J1858+020
title_short	Identifying the counterpart of HESS J1858+020
title_full	Identifying the counterpart of HESS J1858+020
title_fullStr	Identifying the counterpart of HESS J1858+020
title_full_unstemmed	Identifying the counterpart of HESS J1858+020
title_sort	identifying the counterpart of hess j1858+020
publishDate	2010
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v509_n1_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v509_n1_p_Paron
_version_	1768545718779248640

Identifying the counterpart of HESS J1858+020

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