Constraints on the [C II] luminosity of a proto-globular cluster at z ∼ 6 obtained with ALMA

We report on ALMA observations of D1, a system at z similar to 6.15 with stellar mass M-* similar to 10(7)M(circle dot) containing globular cluster (GC) precursors, strongly magnified by the galaxy cluster MACS J0416.1-2403. Since the discovery of GC progenitors at high redshift, ours is the first attempt to probe directly the physical properties of their neutral gas through infrared observations. A careful analysis of our data set, performed with a suitable procedure designed to identify faint narrow lines and which can test various possible values for the unknown linewidth value, allowed us to identify a 4 sigma tentative detection of [CII] emission with intrinsic luminosity L-[C II] = (2.9 +/- 1.4) 10(6) L-1, one of the lowest values ever detected at high redshift. This study offers a first insight on previously uncharted regions of the L[ C II]-SFR relation. Despite large uncertainties affecting our measure of the star formation rate, if taken at face value our estimate lies more than similar to 1 dex below the values observed in local and high redshift systems. Our weak detection indicates a deficiency of [C II] emission, possibly ascribed to various explanations, such as a low-density gas and/or a strong radiation field caused by intense stellar feedback, and a low metal content. From the non-detection in the continuum, we derive constraints on the dust mass, with 3 sigma upper limit values as low as similar to a few 10(4)M(circle dot), consistent with the values measured in local metal-poor galaxies.

Automated summary

A study of ALMA observations on the D1 system reveals a 4 sigma tentative detection of [CII] emission, shedding light on uncharted regions of the L[ C II]-SFR relation. The weak detection suggests a deficiency of [C II] emission, possibly due to low-density gas, strong radiation fields, and low metal content. Constraints on the dust mass were derived from the non-detection in the continuum, with 3 sigma upper limit values consistent with those in local metal-poor galaxies.