2011A&A...530A..25P

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. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the J=3-2, 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.From the and J=3-2 lines and the 1.1mm continuum emission, we derive a density of between 10³ and 10⁴cm^–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.