Is HESS J1912+101 associated with an old Supernova Remnant?
  HESS J1912+101 is a shell-like TeV source that has no clear counterpart in
multiwavelength. Using CO and H i data, we reveal that VLSR~+60 km/s molecular
clouds (MCs), together with shocked molecular gas and high-velocity neutral
atomic shells, are concentrated toward HESS J1912+101. The prominent wing
profiles up to VLSR~+80 km/s seen in 12CO (J=1-0 and J=3-2) data, as well as
the high-velocity expanding H i shells up to VLSR~ +100 km/s, exhibit striking
redshifted-broadening relative to the quiescent gas. These features provide
compelling evidences for large-scale perturbation in the region. We argue that
the shocked MCs and the high-velocity Hi shells may originate from an old
supernova remnant (SNR). The distance to the SNR is estimated to be ~4.1 kpc
based on the Hi self-absorption method, which leads to a physical radius of
29.0 pc for the ~(0.7-2.0)x10e5 years old remnant with an expansion velocity of
>40 km/s. The +60 km/s MCs and the disturbed gas are indeed found to coincide
with the bright TeV emission, supporting the physical association between them.
Naturally, the shell-like TeV emission comes from the decay of neutral pions
produced by interactions between the accelerated hadrons from the SNR and the
surrounding high-density molecular gas.
