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Fig. 4


Power spectra of gas surface density fluctuations in isolated gasoline and ramses galaxies. The power spectra are normalized by a third-degree power law to highlight the differences between simulations. Shaded error regions indicate the 10–90th percentile range from bootstrap resampling. gasoline shows more power at small scales and less power at large scales, emphasizing that gas structures in our gasoline simulations tend to have smaller sizes than those in ramses.

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