Low Star Formation Efficiency in Typical Galaxies at z = 5–6

Abstract

Using the Very Large Array and ALMA, we have obtained CO(2–1), [C ii ], and [N ii ] line emission and multiple dust continuum measurements in a sample of “normal” galaxies at z  = 5–6. We report the highest-redshift detection of low- J CO emission from a Lyman break galaxy, at z  ∼ 5.7. The CO line luminosity implies a massive molecular gas reservoir of (1.3 ± 0.3)( α CO /4.5 M ⊙ (K km s −1 pc 2 ) −1 ) × 10 11 M ⊙ , suggesting low star formation efficiency with a gas depletion timescale of order ∼1 Gyr. This efficiency is much lower than traditionally observed in z  ≳ 5 starbursts, indicating that star-forming conditions in main-sequence galaxies at z  ∼ 6 may be comparable to those of normal galaxies probed up to z  ∼ 3 to date but with rising gas fractions across the entire redshift range. We also obtain a deep CO upper limit for a main-sequence galaxy at z  ∼ 5.3 with an approximately three times lower star formation rate, perhaps implying a high α CO conversion factor, as typically found in low-metallicity galaxies. For a sample including both CO targets, we also find faint [N ii ] 205 μ m emission relative to [C ii ] in all but the most IR-luminous “normal” galaxies at z  = 5–6, implying more intense or harder radiation fields in the ionized gas relative to lower redshift. These radiation properties suggest that low metallicity may be common in typical ∼10 10 M ⊙ galaxies at z  = 5–6. While a fraction of main-sequence star formation in the first billion yr may take place in conditions not dissimilar to lower redshift, lower metallicity may affect the remainder of the population.