Extended Data Fig. 3: Number density n(z) as a function of redshift for different Σ*.
From: Unexpected clustering pattern in dwarf galaxies challenges formation models
n(z) is normalized by that of the lowest-z bin (n0). a, n(z) for low-mass (\(7.5 < \log \,{M}_{* }/{{\rm{M}}}_{\odot }\le 8.5\)) and massive (\(8.5 < \log \,{M}_{\ast }/{{\rm{M}}}_{\odot } < 9\)) dwarfs separately. For massive dwarfs, the SEs become large only when z > 0.04. For less-massive dwarfs, the SEs are significant even at z ~ 0.02. For given M*, the impact of the SEs depends only weakly on Σ*, as is expected from the small redshift concerned here. At z > 0.04, there is no low-mass dwarf with Σ* > 7 M⊙pc−2. b, n(z) for red (0.3 < 0.1(g − r) < 0.6) and blue (0.1(g − r) < 0.3) dwarfs separately. Dwarfs with different colors exhibit similar behavior, indicating that the SEs are insensitive to galaxy color. This is because our galaxies have already been restricted to a relatively narrow color range.
