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HESS J1825-137 is a pulsar wind nebula (PWN) whose TeV emission extendsacross ~1 deg. Its large asymmetric shape indicates that its progenitorsupernova interacted with a molecular cloud located in the north of the PWN asdetected by previous CO Galactic survey (e.g Lemiere, Terrier &Djannati-Ata\"i 2006). Here we provide a detailed picture of the ISM towardsthe region north of HESS J1825-137, with the analysis of the dense moleculargas from our 7mm and 12mm Mopra survey and the more diffuse molecular gas fromthe Nanten CO(1-0) and GRS $^{13}$CO(1-0) surveys. Our focus is the possibleassociation between HESS J1825-137 and the unidentified TeV source to thenorth, HESS J1826-130. We report several dense molecular regions whosekinematic distance matched the dispersion measured distance of the pulsar.Among them, the dense molecular gas located at (RA,Dec)=(18.421h,-13.282$^{\circ}$) shows enhanced turbulence and we suggest thatthe velocity structure in this region may be explained by a cloud-cloudcollision scenario. Furthermore, the presence of a H$\alpha$ rim may be thefirst evidence of the progenitor SNR of the pulsar PSR J1826-1334 as thedistance between the H$\alpha$ rim and the TeV source matched with thepredicted SNR radius R$_{\text{SNR}}$~120 pc. From our ISM study, we identify afew plausible origins of the HESS J1826-130 emission, including the progenitorSNR of PSR J1826-1334 and the PWN G018.5-0.4 powered by PSR J1826-1256. Adeeper TeV study however, is required to fully identify the origin of thismysterious TeV source.

ISM gas studies towards the TeV PWN HESS J1825-137 and northern region