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Optical emission is detected from filaments around the central galaxies ofclusters of galaxies. These filaments have lengths of tens of kiloparsecs. Theemission is possibly due to heating caused by the dissipation of mechanicalenergy and by cosmic ray induced ionisation. CO millimeter and submillimeterline emissions as well as H$_{2}$ infrared emission originating in suchfilaments surrounding NGC~1275, the central galaxy of the Perseus cluster, havebeen detected. Our aim is to identify those molecular species, other than CO,that may emit detectable millimeter and submillimeter line features arising inthese filaments, and to determine which of those species will produce emissionsthat might serve as diagnostics of the dissipation and cosmic ray inducedionisation. The time-dependent UCL photon-dominated region modelling code wasused in the construction of steady-state models of molecular filamentaryemission regions at appropriate pressures, for a range of dissipation andcosmic ray induced ionisation rates and incident radiation fields.HCO$^+$ andC$_2$H emissions will potentially provide information about the cosmic rayinduced ionisation rates in the filaments. HCN and, in particular, CN arespecies with millimeter and submillimeter lines that remain abundant in thewarmest regions containing molecules. Detections of the galaxy clusterfilaments in HCO$^{+}$, C$_{2}$H, and CN emissions and further detections ofthem in HCN emissions would provide significant constraints on the dissipationand cosmic ray induced ionisation rates.

Molecular Tracers of Filamentary CO Emission Regions Surrounding the Central Galaxies of Clusters