2024A&A...687A.253H

Query : 2024A&A...687A.253H

2024A&A...687A.253H - Astronomy and Astrophysics, volume 687A253 (2024/7-1)

Simulating the LOcal Web (SLOW) II. Properties of local galaxy clusters.

HERNANDEZ-MARTINEZ E., DOLAG K., SEIDEL B., SORCE J.G., AGHANIM N., PILIPENKO S., GOTTLOBER S., LEBEAU T. and VALENTINI M.

Abstract (from CDS):

Context. This is the second paper in a series presenting the results from a 500 h–1Mpc large constrained simulation of the local Universe (SLOW). The initial conditions for this cosmological hydro-dynamical simulation are based on peculiar velocities derived from the CosmicFlows-2 catalog. The simulation follows cooling, star formation, and the evolution of super-massive black holes. This allows one to directly predict observable properties of the intracluster medium (ICM) within galaxy clusters, including X-ray luminosity, temperatures, and the Compton-y signal.
Aims. Comparing the properties of observed galaxy clusters within the local Universe with the properties of their simulated counterparts enables us to assess the effectiveness of the initial condition constraints in accurately replicating the mildly nonlinear properties of the largest, collapsed objects within the simulation.
Methods. Based on the combination of several, publicly available surveys we compiled a sample of galaxy clusters within the local Universe, of which we were able to cross-identify 46 of them with an associated counterpart within the SLOW simulation. We then derived the probability of the cross identification based on mass, X-ray luminosity, temperature, and Compton-y by comparing it to a random selection.
Results. Our set of 46 cross-identified local Universe clusters contains the 13 most massive clusters from the Planck SZ catalog as well as 70% of clusters with M500 larger than 2 × 1014 M⊙. Compared to previous constrained simulations of the local volume, we found in SLOW a much larger amount of replicated galaxy clusters, where their simulation-based mass prediction falls within the uncertainties of the observational mass estimates. Comparing the median observed and simulated masses of our cross-identified sample allows us to independently deduce a hydrostatic mass bias of (1 - b)≈0.87.
Conclusions. The SLOW constrained simulation of the local Universe faithfully reproduces numerous fundamental characteristics of a sizable number of galaxy clusters within our local neighborhood, opening a new avenue for studying the formation and evolution of a large set of individual galaxy clusters as well as testing our understanding of physical processes governing the ICM.

Abstract Copyright: © The Authors 2024

Journal keyword(s): methods: numerical - galaxies: clusters: general - large-scale structure of Universe

Simbad objects: 50

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Number of rows : 50
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 ACO 2734 ClG 00 11 21.60 -28 51 16.6           ~ 156 0
2 ACO 85 ClG 00 41 36.21 -09 19 30.4           ~ 974 0
3 ACO 119 ClG 00 56 08.57 -01 12 00.8           ~ 577 2
4 ACO 2877 ClG 01 09 49.3 -45 54 02           ~ 160 2
5 ACO 347 ClG 02 25 50 +41 52.5           ~ 149 1
6 2A 0251+413 ClG 02 54 26.6 +41 33 25           ~ 328 1
7 ACO 426 ClG 03 19 47.6 +41 30 54           ~ 2508 1
8 ACO S 373 ClG 03 38 29.4 -35 27 08           ~ 2029 0
9 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 402 1
10 ACO 3158 ClG 03 43 07.5 -53 38 09           ~ 327 0
11 ACO 3266 ClG 04 31 26.4 -61 25 17           ~ 447 0
12 ACO 496 ClG 04 33 40.8 -13 14 34           ~ 728 2
13 3C 129 rG 04 49 09.064 +45 00 39.40   19       ~ 273 2
14 ACO 539 ClG 05 16 35.1 +06 27 14           ~ 255 2
15 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 334 0
16 ACO 3391 ClG 06 26 15.4 -53 40 52           ~ 222 1
17 ACO 576 ClG 07 21 24.1 +55 44 20           ~ 312 1
18 ACO 644 ClG 08 17 26.1 -07 31 13           ~ 241 0
19 NAME HYA SUPERCL SCG 08 57.9 +03 10           ~ 204 0
20 ACO 754 ClG 09 09 14.8 -09 40 35           ~ 695 1
21 NAME Great Attractor SCG 10 32 -46.0           ~ 617 0
22 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 905 1
23 ACO 1185 ClG 11 10 32.15 +28 35 50.4           ~ 271 1
24 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1127 1
25 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
26 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
27 ACO 3526 ClG 12 48 49.2 -41 18 17           ~ 1154 2
28 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 391 1
29 ACO 3532 ClG 12 57 19.2 -30 22 13           ~ 185 2
30 NGC 4874 LIN 12 59 35.7093764280 +27 57 33.293892204 13.01 13.7 12.71 12.27 11.386 ~ 814 3
31 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
32 NGC 4889 EmG 13 00 08.097 +27 58 37.29 12.93 13.0 11.30 11.652 10.906 ~ 742 1
33 NAME Shapley Supercluster SCG 13 06.0 -33 04           ~ 677 0
34 ACO 1736 ClG 13 26 52.1 -27 06 33           ~ 268 2
35 ACO 3558 ClG 13 28 03.2 -31 31 35           ~ 476 2
36 ACO 3571 ClG 13 47 32.4 -32 50 12           ~ 308 2
37 ACO 1795 ClG 13 48 47.4 +26 34 55           ~ 1330 0
38 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 197 3
39 ACO 2029 ClG 15 10 54.2 +05 44 23           ~ 1020 0
40 ACO 2065 ClG 15 22 22.7 +27 44 20           ~ 398 0
41 ACO 2063 ClG 15 23 01.8 +08 38 22           ~ 414 2
42 ACO 2107 ClG 15 39 39.04 +21 46 57.8           ~ 270 0
43 ACO 3627 ClG 16 14 22.5 -60 52 07           ~ 340 2
44 ACO 2197 ClG 16 27 48.01 +40 58 04.5           ~ 290 0
45 ACO 2256 ClG 17 03 37.5 +78 37 23           ~ 928 1
46 ACO 2319 ClG 19 21 14.0 +43 56 57           ~ 495 1
47 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 676 1
48 ACO 2593 ClG 23 24 27.15 +14 33 40.2           ~ 231 0
49 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 515 2
50 ACO 2665 ClG 23 50 50.6 +06 09 00           ~ 106 0

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