Modelling the multi-wavelength detection of protoclusters. I: An excess of submillimetre galaxies in protocluster cores

TL;DR

This study uses semi-analytic modeling to show that protocluster cores have a higher fraction of submillimetre-bright galaxies due to environmental overdensities, aiding interpretation of multi-wavelength observations.

Contribution

It provides a theoretical link between submillimetre galaxy excess and protocluster environments using the L-GALAXIES model applied to the Millennium simulation.

Findings

Higher fraction of submm-bright galaxies in protocluster cores.

Excess not driven by starburst frequency but by halo overdensity.

Dust-obscured star formation is more prevalent in protocluster cores.

Abstract

Studies of galaxy protoclusters yield insights into galaxy cluster formation complementary to those obtained via `archaeological' studies of present-day galaxy clusters. Submillimetre-selected galaxies (SMGs) are one class of sources used to find high-redshift protoclusters. However, due to the rarity of protoclusters (and thus the large simulation volume required) and the complexity of modeling dust emission from galaxies, the relationship between SMGs and protoclusters has not been adequately addressed in the theoretical literature. In this work, we apply the L-GALAXIES semi-analytic model (SAM) to the Millennium N-body simulation. We assign submillimetre (submm) flux densities to the model galaxies using a scaling relation from previous work, in which dust radiative transfer was performed on high-resolution galaxy zoom simulations. We find that the fraction of model galaxies that are submm-bright is higher in protocluster cores than in both protocluster `outskirts' and the field; the fractions for the latter two are similar. This excess is not driven by an enhanced starburst frequency. Instead, the primary reason is that overdense environments have a relative overdensity of high-mass halos and thus `oversample' the high-mass end of the star formation main sequence relative to less-dense environments. The fraction of SMGs that are optically bright is dependent on stellar mass and redshift but independent of environment. The fraction of galaxies for which the majority of star formation is dust-obscured is higher in protocluster cores, primarily due to the dust-obscured fraction being correlated with stellar mass. Our results can be used to guide and interpret multi-wavelength studies of galaxy populations in protoclusters.