Leftpanel: PDF of μ₁ = cos θ₁, the angle between the minor axis of the central galaxy and the satellite separation vector r_gs. Right panel: PDF of μ = cos θ, the angle between the spin of the central galaxy and the separation vector. Distributions are plotted for three different subsets of low-mass centrals with varying types of satellites (green and blue shades): Γ₁: 10⁹ < M_g < 10¹⁰ M_⊙, Γ₂: 5 × 10⁹< M_g < 10¹⁰ M_⊙ and M_s < 2 × 10⁹ M_⊙, Γ₃: 5 × 10⁹< M_g < 10¹⁰ M_⊙, M_s < 2× 10⁹ M_⊙ and R_gs > R_vir. Satellites oflow-mass centrals tend to align with their central’s spin/minor axis, consistently with the fact that they tend to align with the nearest filament. However, the signal is limited in amplitude and tends to vanish when traced with the minor axis for centrals with massive satellites and/or with satellites in their close vicinity. In this mass range for the central, the satellite is often of comparable mass and both galaxies equally impact the orientation and shape of one another prior to merger.