V. VillanuevaIbar, EduardoEduardoIbarT. M. HughesM. A. Lara-LópezL. DunneS. EalesR. J. IvisonM. AravenaM. BaesN. BourneP. CassataA. CoorayH. DannerbauerL. J. M. DaviesS. P. DriverS. DyeC. FurlanettoR. Herrera-CamusS. J. MaddoxM. J. MichałowskiJ. MolinaD. RiechersA. E. SansomM. W. L. SmithG. RodighieroE. ValianteP. van der Werf2025-12-072025-12-072017-05-3010.1093/mnras/stx13382-s2.0-85029509115https://cris-uv-2.scimago.es/handle/123456789/7559WOS:000408207600001We present an extragalactic survey using observations from the Atacama Large Millimeter/submillimeter Array (ALMA) to characterise galaxy populations up to z = 0.35: the Valparaíso ALMA Line Emission Survey (VALES). We use ALMA Band-3 CO(1–0) observations to study the molecular gas content in a sample of 67 dusty normal star-forming galaxies selected from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We have spectrally detected 49 galaxies at >5σ significance and 12 others are seen at low significance in stacked spectra. CO luminosities are in the range of (0.03 − 1.31) × 1010 K km s−1 pc2, equivalent to log (Mgas/M⊙) = 8.9 − 10.9 assuming an αCO = 4.6 (K km s−1 pc2)−1, which perfectly complements the parameter space previously explored with local and high-z normal galaxies. We compute the optical to CO size ratio for 21 galaxies resolved by ALMA at ∼3
\n′′.
\n.′′
\n 
\n5 resolution (6.5 kpc), finding that the molecular gas is on average ∼ 0.6 times more compact than the stellar component. We obtain a global Schmidt-Kennicutt relation, given by 
\nlog[ΣSFR/(M⊙yr−1kpc−2)]=(1.26±0.02)×log[ΣMH2/(M⊙pc−2)]−(3.6±0.2)
\nlog⁡[ΣSFR/(M⊙yr−1kpc−2)]=(1.26±0.02)×log⁡[ΣMH2/(M⊙pc−2)]−(3.6±0.2)
\n. We find a significant fraction of galaxies lying at ‘intermediate efficiencies’ between a long-standing mode of star-formation activity and a starburst, specially at 
\nLIR=1011−12L⊙
\nLIR=1011−12L⊙
\n.Combining our observations with data taken from the literature, we propose that star formation efficiencies can be parameterised by 
\nlog[SFR/MH2]=0.19×(logLIR−11.45)−8.26−0.41×arctan[−4.84(logLIR−11.45)]
\nlog[SFR/MH2]=0.19×(logLIR−11.45)−8.26−0.41×arctan⁡[−4.84(log⁡LIR−11.45)]
\n. Within the redshift range we explore (z < 0.35), we identify a rapid increase of the gas content as a function of redshift.enacceso abiertoAstronomy And AstrophysicsSpace And Planetary Sciencearticle