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We present 12 mm Mopra observations of dense molecular gas towards the W28 supernova remnant (SNR) field. The focus is on the dense molecular gas towards the TeV gamma‐ray sources detected by the HESS telescopes, which likely trace the cosmic rays from W28 and possibly other sources in the region. Using the NH  3   inversion transitions we reveal several dense cores inside the molecular clouds, the majority of which coincide with high‐mass star formation and H  ii  regions, including the energetic ultracompact H  ii  region G5.89 − 0.39. A key exception to this is the cloud north‐east of W28, which is well known to be disrupted as evidenced by clusters of 1720 MHz OH masers and broad CO line emission. Here we detect broad NH  3  , up to the (9,9) transition, with linewidths up to 16 km s  −1  . This broad NH  3   emission spatially matches well with the TeV source HESS J1801 − 233 and CO emission, and its velocity dispersion distribution suggests external disruption from the W28 SNR direction. Other lines are detected, such as HC  3  N and HC  5  N, H  2  O masers, and many radio recombination lines, all of which are primarily found towards the southern high‐mass star formation regions. These observations provide a new view on to the internal structures and dynamics of the dense molecular gas towards the W28 SNR field and, in tandem with future higher‐resolution TeV gamma‐ray observations, will offer the chance to probe the transport of cosmic rays into molecular clouds.

12 mm line survey of the dense molecular gas towards the W28 field TeV gamma‐ray sources