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Context: The supernova remnant (SNR) G35.6-0.4 shows a non-thermal radioshell, however, no {\gamma}-ray or X-ray counterparts have been found for itthus far. One TeV source, HESS J1858+020, was found near the SNR and thissource is spatially associated with some clouds at 3.6 kpc. Aims: To attain abetter understanding of the origin of HESS J1858+020, we further investigatethe association between SNR cosmic rays (CRs) and the clouds through theFermi-LAT analysis and hadronic modeling. Methods: We performed the Fermi-LATanalysis to explore the GeV emission in and around the SNR. We explored the SNRphysics with previously observed multi-wavelength data. We built a hadronicmodel using runaway CRs of the SNR to explain the GeV-TeV observation. Results:We found a hard GeV source (SrcX2) that is spatially coincident with both HESSJ1858+020 and a molecular cloud complex at 3.6 kpc. In addition, a soft GeVsource (SrcX1) was found at the northern edge of the SNR. The GeV spectrum ofSrcX2 connects well with the TeV spectrum of HESS J1858+020. The entire{\gamma}-ray spectrum ranges from several GeV up to tens of TeV and it followsa power-law with an index of ~2.15. We discuss several pieces of observationalevidence to support the middle-aged SNR argument. Using runaway CRs from theSNR, our hadronic model explains the GeV-TeV emission at HESS J1858+020, with adiffusion coefficient that is much lower than the Galactic value.

HESS J1858+020: A GeV-TeV source possibly powered by CRs from SNR G35.6-0.4