Caught in the cosmic web: Environmental effects on subhalo abundance and internal density profiles

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Table 3.

Best-fitting β values and power-law slope s for cumulative subhalo mass functions.

$⟨ M_{200} ⟩ [h^{- 1} M_{⊙}]$ $\langle M_{200} \rangle\, \left[{h}^{-1}\, \mathrm{M_\odot}\right]$	Cosmic mean	Filaments	Walls	Voids	Equally weighted	Power-law slope, s
10¹²	129 ± 4	100 ± 9	124 ± 8	–	94 ± 2	0.93 ± 0.02
10¹¹	89 ± 6	79 ± 5	95 ± 4	89 ± 2	97 ± 3	0.92 ± 0.02
10¹⁰	67 ± 2	48 ± 1	54 ± 2	60 ± 2	57 ± 1	0.91 ± 0.01

Notes. The best-fitting β values are obtained from fits of Eq. (4) to the cSHMF, shown as a function of the host halo mass, in the cosmic mean, filament, wall, void, and the equally weighted samples. The final column shows the best-fitting power-law slope, s, which is independent of the host halo environment.

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