Study of the molecular clump associated with the high-energy source HESS J1858+020
Author
dc.contributor.author
Paron, S.
Author
dc.contributor.author
Giacani, E.
es_CL
Author
dc.contributor.author
Rubio López, Mónica
es_CL
Author
dc.contributor.author
Dubner, G.
es_CL
Admission date
dc.date.accessioned
2014-01-14T13:43:14Z
Available date
dc.date.available
2014-01-14T13:43:14Z
Publication date
dc.date.issued
2011
Cita de ítem
dc.identifier.citation
A&A 530, A25 (2011)
en_US
Identifier
dc.identifier.issn
0004-6361
Identifier
dc.identifier.other
DOI: 10.1051/0004-6361/201016390
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/126238
General note
dc.description
Artículo de publicación
en_US
Abstract
dc.description.abstract
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
104 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.