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The presence of a well-defined and narrow dust lane in an edge-on spiralgalaxy is the observational signature of a thin and dense molecular disk, inwhich gravitational collapse has overcome turbulence. Using a sample ofgalaxies out to z~1 extracted from the COSMOS survey, we identify the fractionof massive disks that display a dust lane. Our goal is to explore the evolutionin the stability of the molecular ISM disks in spiral galaxies over a cosmictimescale. We check the reliability of our morphological classificationsagainst changes in restframe wavelength, resolution, and cosmic dimming with(artificially redshifted) images of local galaxies from SDSS. We find that thefraction of L* disks with dust lanes in COSMOS is consistent with the localfraction (~80%) out to z~0.7. At z=0.8, the dust lane fraction is only slightlylower. A somewhat lower dust lane fraction in starbursting galaxies tentativelysupports the notion that a high specific star formation rate can efficientlydestroy or inhibit a dense molecular disk. A small subsample of higher redshiftCOSMOS galaxies display low internal reddening (E[B-V]), as well as a lowincidence of dust lanes. These may be disks in which the growth of the dustyISM disk lags behind that of the stellar disk. We note that at z=0.8, the mostmassive galaxies display a lower dust lane fraction than lower mass galaxies. Asmall contribution of recent mergers or starbursts to this most massivepopulation may be responsible. The fact that the fraction of galaxies with dustlanes in COSMOS is consistent with little or no evolution implies that modelsto explain the Spectral Energy Distribution or the host galaxy dust extinctionof supernovae based on local galaxies are still applicable to higher redshiftspirals. It also suggests that dust lanes are long lived phenomena or can bereformed over very short time-scales.

Evolution in the Dust Lane Fraction of Edge-on L* Spiral Galaxies since z=0.8