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• W1984072856 endingPage "25" @default.
• W1984072856 startingPage "25" @default.
• W1984072856 abstract "Nearby spiral galaxies show an extremely tight correlation between tracers of molecular hydrogen (H2) in the interstellar medium and tracers of recent star formation, but it is unclear whether this correlation is fundamental or accidental. In the galaxies that have been surveyed to date, H2 resides predominantly in gravitationally bound clouds cooled by carbon monoxide (CO) molecules, but in galaxies of low metal content the correlations between bound clouds, CO, and H2 break down, and it is unclear if the star formation rate (SFR) will then correlate with H2 or with some other quantity. Here, we show that star formation will continue to follow H2 independent of metallicity. This is not because H2 is directly important for cooling, but instead because the transition from predominantly atomic hydrogen (H i) to H2 occurs under the same conditions as a dramatic drop in gas temperature and Bonnor–Ebert mass that destabilizes clouds and initiates collapse. We use this model to compute how SFR will correlate with total gas mass, with mass of gas where the hydrogen is H2, and with mass of gas where the carbon is CO in galaxies of varying metallicity, and show that preliminary observations match the trend we predict." @default.
• W1984072856 created "2016-06-24" @default.
• W1984072856 creator A5014544028 @default.
• W1984072856 creator A5050357373 @default.
• W1984072856 creator A5063633367 @default.
• W1984072856 date "2011-03-18" @default.
• W1984072856 modified "2023-10-15" @default.
• W1984072856 title "WHICH PHASE OF THE INTERSTELLAR MEDIUM CORRELATES WITH THE STAR FORMATION RATE?" @default.
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• W1984072856 doi "https://doi.org/10.1088/0004-637x/731/1/25" @default.
• W1984072856 hasPublicationYear "2011" @default.
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