How the cool-core population transitions from galaxy groups to massive clusters - A comparison of the largest Magneticum simulation with eROSITA, XMM-Newton, Chandra and LOFAR observations

Open Access

Table 2.

Cool-core fractions from Magneticum Box2b.

M_500, min	M_500, max	M_500, med	N_tot	N_cc	f_cc
4.88	10.68	6.15	50	6	0.12 ± 0.04
3.69	4.84	4.23	50	11	0.24 ± 0.06
2.69	3.66	3.05	151	51	0.34 ± 0.04
1.69	2.68	2.02	467	204	0.45 ± 0.02
1.00	1.69	1.23	1309	609	0.47 ± 0.01
0.90	1.0	0.94	419	189	0.45 ± 0.02
0.80	0.90	0.85	567	253	0.45 ± 0.02
0.70	0.80	0.74	754	329	0.44 ± 0.02
0.60	0.70	0.65	1071	438	0.41 ± 0.02
0.50	0.60	0.54	1625	642	0.39 ± 0.01
0.40	0.50	0.44	2562	791	0.30 ± 0.01
0.30	0.40	0.34	4658	1189	0.25 ± 0.01

Notes. Columns description as in Table 1.

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