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Aims. The goal of this paper is to detect synchrotron emission from the relicelectrons of the crushed pulsar wind nebula (PWN) HESS J1825-137 and toinvestigate the origin of the $\gamma$-ray emission from HESS J1826-130.\\Methods. The study of HESS J1825-137 was carried out on the basis of new radioobservations centred at the position of PSR J1826-1334 performed with the KarlG. Jansky Very Large Array at 1.4 GHz in configurations B and C. To investigatethe nature of HESS J1826-130, we reprocessed unpublished archival data obtainedwith XMM-Newton.\\ Results. The new radio continuum image towards PSRJ1826-1334 reveals a bright radio source, with the pulsar located in itscentre, which suggests that this feature could be the radio counterpart of thecompact component of the PWN detected at high energy. The new 1.4 GHz radiodata do not reveal emission with an extension comparable with that observed in$\gamma$-rays for the HESS J1825-137 source. On the other hand, the XMM-Newtonstudy of the region including PSR J1826-1256 reveals an elongated non-thermalX-ray emitting nebula with the pulsar located in the northern border and a tailtowards the peak of the very high energy source. The spectrum is characterizedby a power law with a photon index going from 1.6 around the pulsar to 2.7 inthe borders of the nebula, a behaviour consistent with synchrotron cooling ofelectrons. From our X-ray analysis we propose that HESS J1826-130 is likelyproduced by the PWN powered by PSR J1826-1256 via the inverse Comptonmechanism.

A new study towards PSR J1826-1334 and PSR J1826-1256 in the region of HESS J1825-137 and HESS J1826-130