Examinando por Autor "Hill, R."

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    Megaparsec-scale structure around the protocluster core SPT2349-56 at z = 4.3
    (Oxford University Press, 2020-05) Hill, R.; Chapman, S.; Scott, D.; Apostolovski, Y.; Aravena, M.; Béthermin, M.; Bradford, C.M.; Canning, R.E.A.; De Breuck, C.; Dong, C.; González, A.; Greve, T.R.; Hayward, C.C.; Hezaveh, Y.; Litke, K.; Malkan, M.; Marrone, D.P.; Phadke, K.; Reuter, C.; Rotermund, K.; Spilker, J.; Vieira, J.D.; Weiß, A.
    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$\, {\pm }\,$5 per cent of the 870 μm flux density at 0.5 arcsec resolution compared to 21 arcsec single-dish data. These galaxies are distributed into a central core containing 23 galaxies extending out to 300 kpc in diameter, and a northern extension, offset from the core by 400 kpc, containing three galaxies. We discovered three additional galaxies in a red Herschel-SPIRE source 1.5 Mpc from the main structure, suggesting the existence of many other sources at the same redshift as SPT2349-56 that are not yet detected in the limited coverage of our data. An analysis of the velocity distribution of the central galaxies indicates that this region may be virialized with a mass of (9$\pm 5)\, {\times }\, 10^{12}$ 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$\, {\times }\, 10^4$ M⊠yr-1 Mpc-3; this may be an order of magnitude greater than the most extreme examples seen in simulations. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.