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We present a multiwavelength morphological analysis of star forming cloudsand filaments in the central ($< 50$ kpc) regions of 16 low redshift ($z<0.3$)cool core brightest cluster galaxies (BCGs). New Hubble Space Telescope (HST)imaging of far ultraviolet continuum emission from young ($\sim 10$ Myr),massive ($> 5$ \Msol) stars reveals filamentary and clumpy morphologies, whichwe quantify by means of structural indices. The FUV data are compared withX-ray, Ly$\alpha$, narrowband H$\alpha$, broadband optical/IR, and radio maps,providing a high spatial resolution atlas of star formation locales relative tothe ambient hot ($\sim10^{7-8}$ K) and warm ionised ($\sim 10^4$ K) gas phases,as well as the old stellar population and radio-bright AGN outflows. Nearlyhalf of the sample possesses kpc-scale filaments that, in projection, extendtoward and around radio lobes and/or X-ray cavities. These filaments may havebeen uplifted by the propagating jet or buoyant X-ray bubble, or may haveformed {\it in situ} by cloud collapse at the interface of a radio lobe orrapid cooling in a cavity's compressed shell. The morphological diversity ofnearly the entire FUV sample is reproduced by recent hydrodynamical simulationsin which the AGN powers a self-regulating rain of thermally unstable starforming clouds that precipitate from the hot atmosphere. In this model,precipitation triggers where the cooling-to- freefall time ratio is$t_{\mathrm{cool}}/t_{\mathrm{ff}}\sim 10$. This condition is roughly met atthe maxmial projected FUV radius for more than half of our sample, andclustering about this ratio is stronger for sources with higher star formationrates.

Far Ultraviolet Morphology of Star Forming Filaments in Cool Core Brightest Cluster Galaxies