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The young composite supernova remnant (SNR) Kesteven 75, with a pulsar windnebula at its center, has an unusual morphology with a bright southernhalf-shell structure in multiwavelengths. The distance to Kes 75 has long beenuncertain. Aiming to address these issues, we have made millimeterspectroscopic observations of the molecular gas toward the remnant. TheV_{LSR}~83--96 km/s molecular clouds (MCs) are found to overlap a largenorth-western region of the remnant and are suggested to be located in front ofthe SNR along the line of sight. Also in the remnant area, the V_{LSR}= 45--58km/s MC shows a blue-shifted broadening in the 12CO (J=1-0) line profile and aperturbed position-velocity structure near the edge of the remnant, with theintensity centroid sitting in the northern area of the remnant. In particular,a cavity surrounded by a molecular shell is unveiled in the intensity map inthe broadened blue wing (45--51 km/s), and the southern molecular shell followsthe bright partial SNR shell seen in X-rays, mid-infrared, and radio continuum.These observational features provide effective evidences for the association ofKes 75 with the adjacent 54 km/s MC. This association leads to a determinationof the kinematic distance at ~10.6 kpc to the remnant, which agrees with alocation at the far side of the Sagittarius arm. The morphological coincidenceof the shell seen in multiwavelengths is consistent with a scenario in whichthe SNR shock hits a pre-existing dense shell. This dense molecular shell issuggested to likely represent the debris of the cooled, clumpy shell of theprogenitor's wind bubble proximately behind the 54 km/s cloud. The discovery ofthe association with MC provides a possible explanation for the gamma-rayexcess of the remnant.

Discovery of molecular shells associated with supernova remnants. (II) Kesteven 75