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A large fraction of Galactic very-high energy (VHE; E$\gtrsim$100 GeV)$\gamma$-ray sources is cataloged as unidentified. In this work we explore thepossibility that these unidentified sources are located in ambientsparticularly rich in material content unaccounted by traditional tracers. In ascenario where the VHE emission is due to the interaction of the acceleratedparticles with a target mass, a large mass of untraced material could besubstantially contributing to the VHE emission from these regions. Here, we usethree tracers for the commonly explored components: intensity of the$^\textrm{12}$CO(1$\rightarrow$0) line to trace the molecular material, HIhyperfine transition at 21cm to trace atomic hydrogen, and dust emission totrace the total hydrogen content. We show that the estimates of materialcontent from these three tracers are compatible if the uncertainty on therespective conversion factors is taken into account. No additional gascomponent is found in these regions. However, a simple mass estimation from the$^\textrm{12}$CO(1$\rightarrow$0) line intensity might underestimate the totalmass component in some locations.

Estimating Galactic gas content using different tracers: Compatibility of results, dark gas, and unidentified TeV sources