Simulating the LOcal Web (SLOW) - IV. Not all that is close will merge in the end: Superclusters and their Lagrangian collapse regions

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Table 2.

Survivor halos of the local superclusters.

Region	N_m	M_FoF	M_vir	M_est (reference)	$\frac{M (z = 0)}{M_{fin}}$ $\frac{M(z = 0)}{M_{\mathrm{fin}}}$	$\frac{M_{fin}}{M_{peak}}$ $\frac{M_{\mathrm{fin}}}{M_{\mathrm{peak}}}$
Shapley	3	72.86	44.42	500.0^(a)	0.42	0.86
Perseus-Pisces	2	18.09	12.13	249.0 (B2)	0.87	0.99
Coma	2	47.08	29.52	168.0 (B1)	0.64	0.84
Virgo	2	16.59	11.91	25.0 (B1)	0.84	0.98
Centaurus	2	34.56	21.59	56.0 (B1)	0.47	0.89
Hercules	3	38.13	24.05	21 ± 2 (MO)	0.64	0.99

Notes. For each region we list number of accreted members and their masses at the final snapshot (a = 1000). All masses are given in units of 10¹⁴ M_⊙.

^(a)

Proust et al. (2006).

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