| Résumé | We measure the molecular-to-atomic gas ratio, Rₘₒₗ, and the star formation rate (SFR) per unit molecular gas mass, SFEₘₒₗ, in 38 nearby galaxies selected from the Virgo Environment Traced in CO (VERTICO) survey. We stack ALMA 12CO (J = 2−1) spectra coherently using H i velocities from the VIVA survey to detect faint CO emission out to galactocentric radii r gal ∼ 1.2 r 25. We determine the scale lengths for the molecular and stellar components, finding a ∼3:5 relation compared to ∼1:1 in field galaxies, indicating that the CO emission is more centrally concentrated than the stars. We compute Rₘₒₗ as a function of different physical quantities. While the spatially resolved Rₘₒₗ on average decreases with increasing radius, we find that the mean molecular-to-atomic gas ratio within the stellar effective radius Rₑ , Rₘₒₗ(r < R e ), shows a systematic increase with the level of H i, truncation and/or asymmetry (HI perturbation). Analysis of the molecular- and the atomic-to-stellar mass ratios within Rₑ , R ⋆ₘₒₗ ( r < R e ) and R ⋆ atom ( r < R e ) , shows that VERTICO galaxies have increasingly lower R ⋆ atom ( r < R e ) for larger levels of HI perturbation (compared to field galaxies matched in stellar mass), but no significant change in R ⋆ₘₒₗ ( r < R e ). We also measure a clear systematic decrease of the SFEₘₒₗ within R e , SFEₘₒₗ (r < Re ), with increasingly perturbed H i. Therefore, compared to field galaxies from the field, VERTICO galaxies are more compact in CO emission in relation to their stellar distribution, but increasingly perturbed atomic gas increases their Rₘₒₗ and decreases the efficiency with which their molecular gas forms stars. |
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