2018Natur.556..469M

Query : 2018Natur.556..469M

2018Natur.556..469M - Nature, 556, 469-472 (2018)

A massive core for a cluster of galaxies at a redshift of 4.3.

MILLER T.B., CHAPMAN S.C., ARAVENA M., ASHBY M.L.N., HAYWARD C.C., VIEIRA J.D., WEISS A., BABUL A., BETHERMIN M., BRADFORD C.M., BRODWIN M., CARLSTROM J.E., CHEN C.-C., CUNNINGHAM D.J.M., DE BREUCK C., GONZALEZ A.H., GREVE T.R., HARNETT J., HEZAVEH Y., LACAILLE K., LITKE K.C., MA J., MALKAN M., MARRONE D.P., MORNINGSTAR W., MURPHY E.J., NARAYANAN D., PASS E., PERRY R., PHADKE K.A., RENNEHAN D., ROTERMUND K.M., SIMPSON J., SPILKER J.S., SREEVANI J., STARK A.A., STRANDET M.L. and STROM A.L.

Abstract (from CDS):

Massive galaxy clusters have been found that date to times as early as three billion years after the Big Bang, containing stars that formed at even earlier epochs. The high-redshift progenitors of these galaxy clusters-termed ‘protoclusters’-can be identified in cosmological simulations that have the highest overdensities (greater-than-average densities) of dark matter. Protoclusters are expected to contain extremely massive galaxies that can be observed as luminous starbursts. However, recent detections of possible protoclusters hosting such starbursts do not support the kind of rapid cluster-core formation expected from simulations: the structures observed contain only a handful of starbursting galaxies spread throughout a broad region, with poor evidence for eventual collapse into a protocluster. Here we report observations of carbon monoxide and ionized carbon emission from the source SPT2349-56. We find that this source consists of at least 14 gas-rich galaxies, all lying at redshifts of 4.31. We demonstrate that each of these galaxies is forming stars between 50 and 1,000 times more quickly than our own Milky Way, and that all are located within a projected region that is only around 130 kiloparsecs in diameter. This galaxy surface density is more than ten times the average blank-field value (integrated over all redshifts), and more than 1,000 times the average field volume density. The velocity dispersion (approximately 410 kilometres per second) of these galaxies and the enormous gas and star-formation densities suggest that this system represents the core of a cluster of galaxies that was already at an advanced stage of formation when the Universe was only 1.4 billion years old. A comparison with other known protoclusters at high redshifts shows that SPT2349-56 could be building one of the most massive structures in the Universe today.

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Nomenclature: Fig. 1, Table 1, Extended Data Table 1: [MCA2018] SPT J2349-56 A (Nos A-N). Extended Data Table 3: [MCA2018] JHHMMSS+DDMMSS N=2+3.

CDS comments: Fig 2: not all clusters were identified.

Simbad objects: 39

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Number of rows : 39
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 ACT-CL J0217.7-0345 ClG 02 17 44 -03 45.5           ~ 50 0
2 JKCS 41 ClG 02 26 44.0 -04 41 36           ~ 64 0
3 AS2COS 0059.1 rG 10 00 20.690 +02 35 20.37           ~ 116 0
4 ClG J1001+0220 ClG 10 01.0 +02 20           ~ 54 0
5 PKS J1140-2628 rG 11 40 48.35884 -26 29 08.6316     22.00     ~ 325 1
6 NAME Hubble Deep Field reg 12 36 49.5 +62 12 58           ~ 1967 1
7 NAME SMM J123652+621225 smm 12 36 51.976 +62 12 25.80           ~ 186 0
8 NAME SMM J123711+622212 rG 12 37 11.92 +62 22 12.1   27.1786 25.185   24.4196 ~ 237 0
9 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
10 IDCS J1426.5+3508 ClG 14 26.5 +35 08           ~ 64 0
11 ClG J1449+0856 ClG 14 49.0 +08 56           ~ 70 0
12 IC 1127 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 3090 4
13 QSO B1921-293 BLL 19 24 51.05595254 -29 14 30.1210248   18.71 18.21 15.07   ~ 918 1
14 ICRF J193925.0-634245 Sy2 19 39 25.0245304992 -63 42 45.640373400   18.87 18.37 17.64   ~ 1332 2
15 NAME SSA22 Protocluster PCG 22 17 34.0 +00 17 01           ~ 175 0
16 QSO B2340-567 QSO 23 43 27.0972079488 -56 26 24.097133508   18.5       ~ 16 1
17 SPT-CL J2349-5638 PCG 23 49.0 -56 38           ~ 47 0
18 [MCA2018] J234912-564031 IR 23 49 12.0 -56 40 31           ~ 1 0
19 [MCA2018] J234925-563527 IR 23 49 25.0 -56 35 27           ~ 1 0
20 [MCA2018] J234936-564117 IR 23 49 36.0 -56 41 17           ~ 1 0
21 [MCA2018] J234939-563633 IR 23 49 39.0 -56 36 33           ~ 1 0
22 [HCS2020] C8 G 23 49 41.23 -56 38 24.4           ~ 11 0
23 [HCS2020] C4 G 23 49 41.42 -56 38 22.6           ~ 11 0
24 [MCA2018] J234942-563825 IR 23 49 42.0 -56 38 25           ~ 1 0
25 [HCS2020] C5 G 23 49 42.14 -56 38 25.8           ~ 9 0
26 [HCS2020] C9 G 23 49 42.22 -56 38 28.3           ~ 9 0
27 [HCS2020] C11 G 23 49 42.38 -56 38 25.8           ~ 9 0
28 [HCS2020] C1 G 23 49 42.67 -56 38 19.3           ~ 12 0
29 [HCS2020] C13 G 23 49 42.74 -56 38 25.1           ~ 12 0
30 [HCS2020] C3 G 23 49 42.79 -56 38 24.0           ~ 13 0
31 [HCS2020] C6 G 23 49 42.84 -56 38 25.1           ~ 13 0
32 [HCS2020] C7 G 23 49 42.96 -56 38 17.9           ~ 9 0
33 [MCA2018] J234943-563731 IR 23 49 43.0 -56 37 31           ~ 1 0
34 [HCS2020] C2 G 23 49 43.22 -56 38 30.1           ~ 10 0
35 [HCS2020] C14 G 23 49 43.27 -56 38 22.9           ~ 9 0
36 [HCS2020] C17 G 23 49 43.39 -56 38 21.1           ~ 8 0
37 [HCS2020] C10 G 23 49 43.46 -56 38 26.2           ~ 9 0
38 [MCA2018] J234955-563417 IR 23 49 55.0 -56 34 17           ~ 2 0
39 QSO B2355-534 BLL 23 57 53.26605016 -53 11 13.6895021   18.63 17.8 16.89   ~ 177 1

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