Why don't clumps of cirrus dust gravitationally collapse?

We consider the Herschel-Planck infrared observations of presumed condensations of interstellar material at a measured temperature of approximately 14 K (Juvela et al 2012 Astron. Astrophys. 541 A12), the triple point temperature of hydrogen. The standard picture is challenged that the material is cirrus-like clouds of ceramic dust responsible for Halo extinction of cosmological sources (Finkbeiner, Davis and Schlegel 1999 Astrophys. J. 524 867). Why would such dust clouds not collapse gravitationally to a point on a gravitational free-fall time scale of 108 years? Why do the particles not collide and stick together, as is fundamental to the theory of planet formation (Blum 2004 PASP Conf. Ser. 309 369; Blum and Wurm 2008 Annu. Rev. Astron. Astrophys. 46 21) in pre-solar accretion discs? Evidence from 3.3 μm and UIB emissions as well as extended red emission data point to the dominance of polycyclic aromatic hydrocarbon (PAH)-type macromolecules for cirrus dust, but such fractal dust will not spin in the manner of rigid grains (Draine and Lazarian 1998 Astrophys. J. 494 L19). IRAS dust clouds examined by Herschel-Planck are easily understood as dark matter proto-globular-star-cluster clumps of primordial gas planets, as predicted by (Gibson 1996 Appl. Mech. Rev. 49 299-315) and observed by (Schild 1996 Astrophys. J. 464 125).