Evolution of Dust-obscured Star Formation and Gas to Z = 2.2 from Hizels

We investigate the far-infrared (far-IR) properties of galaxies selected via deep, narrow-band imaging of the Hα emission line in four redshift slices from z = 0.40–2.23 over ∼ 1 deg as part of the Highredshift Emission Line Survey (HiZELS). We use a stacking approach in the Herschel PACS/SPIRE far-IR bands, along with 850μm imaging from SCUBA-2 and Very Large Array (VLA) 1.4GHz imaging to study the evolution of the dust properties of Hα-emitters selected above an evolving characteristic luminosity threshold, 0.2LHα(z). We investigate the relationship between the dust temperatures, Tdust, and the far-infrared luminosities, LIR of our stacked samples, finding that our Hα-selection identifies cold, low-LIR galaxies (Tdust ∼ 14k; log[LIR/L⊙] ∼ 9.9) at z = 0.40, and more luminous, warmer systems (Tdust ∼ 34k; log[LIR/L⊙] ∼ 11.5) at z = 2.23. Using a modified greybody model, we estimate “characteristic sizes” for the dust-emitting regions of Hα-selected galaxies of ∼ 0.5 kpc, nearly an order of magnitude smaller than their stellar continuum sizes, which may provide indirect evidence of clumpy ISM structure. Lastly, we use measurements of the dust masses from our far-IR stacking along with metallicity-dependent gas-to-dust ratios (δGDR) to measure typical molecular gas masses of ∼ 1× 10M⊙ for these bright Hα-emitters. The gas depletion timescales are shorter than the Hubble time at each redshift, suggesting probable replenishment of their gas reservoirs from the intergalactic medium. Based on the number density of Hα-selected galaxies, we find that typical star-forming galaxies brighter than 0.2LHα(z) comprise a significant fraction (35 ± 10%) of the total gas content of the Universe, consistent with the predictions of the latest state-of-the-art cosmological simulations. Subject headings: galaxies: starburst, galaxies: high-redshift