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The stellar, gaseous and young stellar disks in the LITTLE THINGS sample ofnearby dIrrs are fitted with functions to search for correlations between theparameters. We find that the HI radial profiles are generally flatter in thecenter and fall faster in the outer regions than the V-band profiles, whileyoung stars are more centrally concentrated, especially if the HI is morecentrally flat. This pattern suggests that the HI is turning into molecules inthe center and the molecular clouds are forming stars and FUV. A model thatassumes the molecular surface density is proportional to the total gas surfacedensity to a power of 1.5 or 2, in analogy with the Kennicutt-Schmidt relation,reproduces the relationship between the ratio of the visible to the HI scalelength and the HI Sersic index. The molecular fraction is estimated as afunction of radius for each galaxy by converting the FUV to a molecular surfacedensity using conventional calibrations. The average molecular fraction inside3R_D is 23+/-17%. However, the break in the stellar surface brightness profilehas no unified tracer related to star formation.

the astronomical journal

Relationships between the Stellar, Gaseous, and Star Formation Disks in  LITTLE THINGS Dwarf Irregular Galaxies: Indirect Evidence for Substantial  Fractions of Dark Molecular Gas