On the multiplicity of red-Herschel sources and its implications for extreme star formation

TL;DR

This study investigates the multiplicity of red-Herschel sources using ALMA data, revealing that most multiple systems are likely due to internal processes rather than large-scale interactions, impacting our understanding of star formation and proto-cluster formation.

Contribution

It provides the largest analysis of red-Herschel source multiplicity with ALMA, highlighting the nature of multiple systems and their implications for star formation mechanisms.

Findings

Most multiple systems are likely physically associated.

Star formation in these galaxies is mainly driven by internal processes.

The study offers a catalog of potential overdensities for future research.

Abstract

We study the multiplicity of galaxies in the largest sample of red-Herschel sources ($S_{250 \mu \mathrm{m}} < S_{350 \mu \mathrm{m}} < S_{500 \mu \mathrm{m}}$) using archival ALMA observations. Out of 2416 fields with ALMA detections (from a total of 3,089 analyzed maps), we identify 474 multiple systems within a radius of 16 arcsec (equivalent to the 500 $\mu$m Herschel beam-size): 420 doubles, 51 triples, and 3 quadruples. In each case the brightest source contributes, on average, 64, 48, and 42 per cent of the total flux in double, triple, and quadruple systems. The average combined ALMA flux density of the sources in double systems is comparable to that of the two brightest components within triple and quadruple systems. Non-parametric tests suggest that only a small fraction of the double systems ($\lesssim13$ per cent) are comprised of sources with compatible redshifts, while 47-67 per cent of triple and quadruple fields contain at least one potentially associated pair. Simulations using a mock catalogue of dusty star-forming galaxies suggest that 32 per cent of the double systems are likely physically associated ($\Delta z < 0.01$, i.e. $\lesssim$10 comoving Mpc at $z = 3$) and, while only 8 per cent of the triple and none of the quadruple systems meet this criterion, $\sim$ 70 per cent of them include at least one likely associated pair. Our results suggest that enhanced star formation rates in submillimetre galaxies are primarily driven by internal processes rather than large-scale interactions. This study also provides a catalog of potential overdensities for follow-up observations, offering insights into proto-cluster formation and evolution.