Megaparsec-scale structure around the protocluster core SPT2349-56 at z = 4.3
Greve, Thomas R.; Spilker, Justin; Aravena, Manuel; Chapman, Scott; Hayward, Christopher C.; Hezaveh, Yashar; Hill, Ryley; Marrone, Daniel P.; Reuter, Cassie; De Breuck, Carlos; Béthermin, Matthieu; Bradford, C. M.; Scott, Douglas; Malkan, Matt; Canning, Rebecca E. A.; Gonzalez, Anthony; Weiß, Axel; Dong, Chenxing; Vieira, Joaquin D.; Apostolovski, Yordanka; Litke, Katrina; Phadke, Kedar; Rotermund, Kaja
Canada, Chile, France, United States, Germany, United Kingdom, Denmark
Abstract
We present an extensive ALMA spectroscopic follow-up programme of the z = 4.3 structure SPT2349-56, one of the most actively star-forming protocluster cores known, to identify additional members using their [C II] 158 μm and CO(4-3) lines. In addition to robustly detecting the 14 previously published galaxies in this structure, we identify a further 15 associated galaxies at z = 4.3, resolving 55±5 per cent of the 870 μm flux density at 0.5 arcsec resolution compared to 21 arcsec single-dish data. These galaxies are distributed into a central core containing 23 galaxies extending out to 300 kpc in diameter, and a northern extension, offset from the core by 400 kpc, containing three galaxies. We discovered three additional galaxies in a red Herschel-SPIRE source 1.5 Mpc from the main structure, suggesting the existence of many other sources at the same redshift as SPT2349-56 that are not yet detected in the limited coverage of our data. An analysis of the velocity distribution of the central galaxies indicates that this region may be virialized with a mass of (9±5) × 1012 M⊙, while the two offset galaxy groups are about 30 and 60 per cent less massive and show significant velocity offsets from the central group. We calculate the [C II] and far-infrared number counts, and find evidence for a break in the [C II] luminosity function. We estimate the average SFR density within the region of SPT2349-56 containing single-dish emission (a proper diameter of 720 kpc), assuming spherical symmetry, to be roughly 4×104 M⊙ yr-1 Mpc-3; this may be an order of magnitude greater than the most extreme examples seen in simulations.