The supermassive black hole population from seeding via collisions in nuclear star clusters

Open Access

Fig. 7

Comparison between the BHMF determined by Vika et al. (2009, gray dots) with our SAMs at ɀ = 0 for galaxies with stellar masses higher than 10⁶ M_⊙ that host NSCs with stellar masses above 10³ M_⊙. The gray dots include the ±1σ error bars, while the thickness of our lines denotes the ±1σ error for our SAMs, estimated as $Φ_{•} / \sqrt{N}$ ${{\rm{\Phi }}_{\rm{ \bullet }}}/\sqrt N$ , where N is the number of SMBHs contained in the bin.

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