Table A.1.
Best-fitting parameters obtained from performing our statistical analysis to 22 spiral galaxies.
Galaxy | Region | tCO[Myr] | tfb[Myr] | λ[pc] | ϵSF[%] | ΣCO, comp | ΣSFR | εgas | tref[Myr] |
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IC 1954 | inter-arm |
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spiral arm (*) |
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NGC 0628 | inter-arm |
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spiral arm |
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NGC 1097 | inter-arm |
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spiral arm (*) |
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NGC 1300 | inter-arm |
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spiral arm |
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NGC 1365 | inter-arm |
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spiral arm |
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NGC 1385 | inter-arm (*) |
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spiral arm (*) |
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NGC 1512 | inter-arm |
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spiral arm |
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NGC 1672 | inter-arm |
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spiral arm (*) |
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NGC 2090 | inter-arm |
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spiral arm (*) |
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NGC 2283 | inter-arm |
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spiral arm (*) |
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NGC 2835 | inter-arm |
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spiral arm |
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NGC 2997 | inter-arm |
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spiral arm |
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NGC 3507 | inter-arm |
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spiral arm (*) |
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NGC 3627 | inter-arm |
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spiral arm |
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NGC 4254 | inter-arm |
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spiral arm |
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NGC 4303 | inter-arm |
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spiral arm (*) |
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NGC 4321 | inter-arm |
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spiral arm (*) |
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NGC 4535 | inter-arm |
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spiral arm |
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NGC 4548 | inter-arm |
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spiral arm (*) |
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NGC 5248 | inter-arm |
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spiral arm |
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NGC 5643 | inter-arm |
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spiral arm |
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NGC 6744 | inter-arm |
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spiral arm |
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Notes. (*) indicates the environments in which the ratio λ/lap, min < 1.5, implying that the independent star-forming regions are not sufficiently resolved. In these cases the estimates of tfb and λ are only 1-σ upper limits, while the estimate of tCO is unaffected by resolution issues (see section 4.3.6 in Kruijssen et al. 2018). There is a strong bias for this issue to occur preferentially in the spiral arms as the surface density and the number of regions is higher in this environment.
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