The submillimetre view of massive clusters at z ∼ 0.8–1.6

Abstract

We analyse 850 µm continuum observations of eight massive X-ray detected galaxy clusters at z ∼ 0.8-1.6 taken with SCUBA-2 on the James Clerk Maxwell Telescope. We find an average overdensity of 850 µm-selected sources of a factor of 4 ± 2 per cluster within the central 1 Mpc compared to the field. We investigate the multiwavelength properties of these sources and identify 34 infrared counterparts to 26 SCUBA-2 sources. Their colours suggest that the majority of these counterparts are probable cluster members. We use the multi-wavelength far-infrared photometry to measure the total luminosities and total cluster star-formation rates demonstrating that they are roughly three orders of magnitude higher than local clusters. We predict the H-band luminosities of the descendants of our cluster submillimetre galaxies and find that their stellar luminosity distribution is consistent with that of passive elliptical galaxies in z ∼ 0 clusters. Together, the faded descendants of the passive cluster population already in place at z ∼ 1 and the cluster submillimetre galaxies are able to account for the total luminosity function of early-type cluster galaxies at z ∼ 0. This suggests that the majority of the luminous passive population in z ∼ 0 clusters are likely to have formed at z ≫ 1 through an extreme, dust-obscured starburst event.

A Multiwavelength Study of ELAN Environments (AMUSE$^2$): Ubiquitous dusty star-forming galaxies associated with enormous Ly$α$ nebulae on megaparsec scales

“…We have tried splitting the counts by the distance to the ELAN, meaning the inner < 2 and outer > 2 regions, but we do not find any significant differences, so there is no evidence of counts overdensity as a function of radial distance, contrary to what was found in other submillimeter or millimeter counts studies toward other AGN samples or dense fields at high redshifts (Zeballos et al 2018;Cooke et al 2019).…”

VIS3COS

“…Some studies found a flattening and/or reversal of this relation (z ∼ 1−1.5, e.g. Cucciati et al 2006;Elbaz et al 2007;Ideue et al 2009;Tran et al 2010;Popesso et al 2011;Li et al 2011;Santos et al 2014;Stach et al 2017;Cooke et al 2019), while others found the same trends we see locally (e.g. Patel et al 2009;Sobral et al 2011;Muzzin et al 2012;Santos et al 2013;Scoville et al 2013;Darvish et al 2016).…”

FIR-luminous [C ii] Emitters in the ALMA-SCUBA-2 COSMOS Survey (AS2COSMOS): The Nature of Submillimeter Galaxies in a 10 Comoving Megaparsec-scale Structure at z ∼ 4.6

“…Submillimeter galaxies (SMGs) are dusty strongly starforming galaxies at high redshift (e.g., Smail et al 1997;Barger et al 1998;Hughes et al 1998;Scott et al 2010;Yun et al 2012), which are believed to be tracers of massive dark-matter halos in the early universe (Blain et al 1999;Hickox et al 2012;Chen et al 2016;Wilkinson et al 2017;An et al 2019;Dudzevičiūtė et al 2020). As such, SMGs are potential signposts to identify large-scale structures (Tamura et al 2009;Umehata et al 2014Umehata et al , 2015Umehata et al , 2019Casey et al 2014;Casey 2016;Miller et al 2018;Oteo et al 2018;Cooke et al 2019;Hill et al 2020;Miller et al 2020) and also provide insights into the formation processes of massive galaxies. The majority of SMGs are found at z=1-4 and they are thought to be powered by gas-rich mergers or rapid gas accretion from the cosmic web (e.g., Tacconi et al 2008;Umehata et al 2019;McAlpine et al 2019).…”