Constraining the volume density of Dusty Star-Forming Galaxies through the first 3mm Number Counts from ALMA

TL;DR

This study uses ALMA 3mm observations to derive the first galaxy number counts at this wavelength, revealing a significant contribution of dusty star-forming galaxies to early universe star formation, challenging previous assumptions.

Contribution

First measurement of 3mm galaxy number counts from ALMA data, constraining the volume density of dusty star-forming galaxies at high redshift.

Findings

Detected 16 sources with >5sigma significance

Indicates non-negligible contribution of DSFGs to star formation at z > 4

Challenges the assumption of declining obscured galaxy contribution at high redshift

Abstract

We carry out a blind search of 3mm continuum sources using the ALMA Science Archive to derive the first galaxy number counts at this wavelength. The analyzed data are drawn from observations towards three extragalactic legacy fields: COSMOS, CDF-S, and the UDS comprising more than 130 individual ALMA Band 3 pointings and an effective survey area of ~200 sq. arcmin with a continuum sensitivity that allows for the direct detection of unlensed Dusty Star-Forming Galaxies (DSFGs) dust emission beyond the epoch of reionization. We present a catalog of 16 sources detected at >5sigma with flux densities S_3mm = 60 - 600 uJy from which number counts are derived. These number counts are then used to place constraints on the volume density of DSFGs with an empirical backward evolution model. Our measured 3mm number counts indicate that the contribution of DSFGs to the cosmic star formation rate density at z >~ 4 is non-negligible. This is contrary to the generally adopted assumption of a sharply decreasing contribution of obscured galaxies at z > 4 as inferred by optical and near-infrared surveys. This work demonstrates the power of ALMA 3mm observations which can reach outstanding continuum sensitivities during typical spectral line science programs. Further constraints on 3mm-selected galaxies will be essential to refine models of galaxy formation and evolution as well as models of early Universe dust production mechanisms.