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We propose a physically based, analytic model for intergalactic filamentsduring the first gigayear of the universe. The structure of a filament is basedupon a gravitationally bound, isothermal cylinder of gas. The modelsuccessfully predicts for a cosmological simulation the total mass per unitlength of a filament (dark matter plus gas) based solely upon the sound speedof the gas component, contrary to the expectation for collisionless dark matteraggregation. It argues that the gas, through its hydrodynamic properties, playsa key role in filament structure rather than being a passive passenger in apreformed dark matter potential. The dark matter of a galaxy follows theclassic equation of collapse of a spherically symmetric overdensity in anexpanding universe. In contrast, the gas usually collapses more slowly. Therelative rates of collapse of these two components for individual galaxies canexplain the varying baryon deficits of the galaxies under the assumption thatmatter moves along a single filament passing through the galaxy centre, ratherthan by spherical accretion. The difference in behaviour of the dark matter andgas can be simply and plausibly related to the model. The range of galaxiesstudied includes that of the so-called "too big to fail" galaxies, which arethought to be problematic for the standard Lambda-CDM model of the universe.The isothermal-cylinder model suggests a simple explanation for why thesegalaxies are, unaccountably, missing from the night sky.

A Model For Intergalactic Filaments and Galaxy Formation During the First Gigayear