Study of the molecular clump associated with the high-energy source HESS J1858+020

Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. s...

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Publicado:	2011
Materias:	gamma rays: ISM ISM: clouds ISM: individual objects: HESS J1858+020 ISM: supernova remnants A-density A-thermal Angular resolution Archival data Atacama Continuum emission H II regions Hadronic interactions High energy emission High-energy sources ISM: individual objects Molecular clouds Molecular clumps Molecular gas Molecular outflows Protostars Shock fronts Submillimeters Young stellar objects Clouds High energy physics Stars Tellurium compounds Gamma rays
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v530_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v530_n_p_Paron
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046361_v530_n_p_Paron
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spelling	paper:paper_00046361_v530_n_p_Paron2023-06-08T14:27:56Z Study of the molecular clump associated with the high-energy source HESS J1858+020 gamma rays: ISM ISM: clouds ISM: individual objects: HESS J1858+020 ISM: supernova remnants A-density A-thermal Angular resolution Archival data Atacama Continuum emission H II regions Hadronic interactions High energy emission High-energy sources ISM: clouds ISM: individual objects ISM: supernova remnants Molecular clouds Molecular clumps Molecular gas Molecular outflows Protostars Shock fronts Submillimeters Young stellar objects Clouds High energy physics Stars Tellurium compounds Gamma rays Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3-2, 13CO J = 3-2, HCO+J = 4-3, and CS J = 7-6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3-2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4. © 2011 ESO. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v530_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v530_n_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	gamma rays: ISM ISM: clouds ISM: individual objects: HESS J1858+020 ISM: supernova remnants A-density A-thermal Angular resolution Archival data Atacama Continuum emission H II regions Hadronic interactions High energy emission High-energy sources ISM: clouds ISM: individual objects ISM: supernova remnants Molecular clouds Molecular clumps Molecular gas Molecular outflows Protostars Shock fronts Submillimeters Young stellar objects Clouds High energy physics Stars Tellurium compounds Gamma rays
spellingShingle	gamma rays: ISM ISM: clouds ISM: individual objects: HESS J1858+020 ISM: supernova remnants A-density A-thermal Angular resolution Archival data Atacama Continuum emission H II regions Hadronic interactions High energy emission High-energy sources ISM: clouds ISM: individual objects ISM: supernova remnants Molecular clouds Molecular clumps Molecular gas Molecular outflows Protostars Shock fronts Submillimeters Young stellar objects Clouds High energy physics Stars Tellurium compounds Gamma rays Study of the molecular clump associated with the high-energy source HESS J1858+020
topic_facet	gamma rays: ISM ISM: clouds ISM: individual objects: HESS J1858+020 ISM: supernova remnants A-density A-thermal Angular resolution Archival data Atacama Continuum emission H II regions Hadronic interactions High energy emission High-energy sources ISM: clouds ISM: individual objects ISM: supernova remnants Molecular clouds Molecular clumps Molecular gas Molecular outflows Protostars Shock fronts Submillimeters Young stellar objects Clouds High energy physics Stars Tellurium compounds Gamma rays
description	Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3-2, 13CO J = 3-2, HCO+J = 4-3, and CS J = 7-6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3-2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4. © 2011 ESO.
title	Study of the molecular clump associated with the high-energy source HESS J1858+020
title_short	Study of the molecular clump associated with the high-energy source HESS J1858+020
title_full	Study of the molecular clump associated with the high-energy source HESS J1858+020
title_fullStr	Study of the molecular clump associated with the high-energy source HESS J1858+020
title_full_unstemmed	Study of the molecular clump associated with the high-energy source HESS J1858+020
title_sort	study of the molecular clump associated with the high-energy source hess j1858+020
publishDate	2011
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v530_n_p_Paron http://hdl.handle.net/20.500.12110/paper_00046361_v530_n_p_Paron
_version_	1768541777734664192

Study of the molecular clump associated with the high-energy source HESS J1858+020

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