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We present ALMA observations at a spatial resolution of 0.2 arcsec (60 pc) ofCO emission from the Taffy galaxies (UGC 12914/5). The observations arecompared with narrow-band Pa$\alpha$, mid-IR, radio continuum and X-rayimaging, plus optical spectroscopy. The galaxies have undergone a recenthead-on collision, creating a massive gaseous bridge which is known to behighly turbulent. The bridge contains a complex web of narrow molecularfilaments and clumps. The majority of the filaments are devoid of starformation, and fall significantly below the Kennicutt-Schmidt relationship fornormal galaxies, especially for the numerous regions undetected in Pa$\alpha$emission. Within the loosely connected filaments and clumps of gas we findregions of high velocity dispersion which appear gravitationally unbound for awide range of likely values of $X_{\rm CO}$. Like the "Firecracker" region inthe Antennae system, they would require extremely high external dynamical orthermal pressure to stop them dissipating rapidly on short crossing timescalesof 2-5~Myrs. We suggest that the clouds may be transient structures within ahighly turbulent multi-phase medium which is strongly suppressing starformation. Despite the overall turbulence in the system, stars seem to haveformed in compact hotspots within a kpc-sized extragalactic HII region, wherethe molecular gas has a lower velocity dispersion than elsewhere, and showsevidence for a collision with an ionized gas cloud. Like the shocked gas in theStephan's Quintet group, the conditions in the Taffy bridge shows how difficultit is to form stars within a turbulent, multi-phase, gas.

The CO emission in the Taffy Galaxies (UGC 12914/5) at 60pc resolution-I: The battle for star formation in the turbulent Taffy Bridge