We investigate how the scaling relations between central black hole mass and host galaxy properties ( velocity dispersion , bulge stellar mass and bulge luminosity ) depend on the large scale environment .
For each of a sample of 69 galaxies with dynamical black hole measurements we compile four environmental measures ( nearest neighbor distance , fixed aperture number density , total halo mass , and central/satellite ) .
We find that central and satellite galaxies follow distinctly separate scalings in each of the three relations we have examined .
The M _ { \bullet } - \sigma relation of central galaxies is significantly steeper ( \beta = 6.39 \pm 0.50 ) than that of satellite galaxies ( \beta = 4.78 \pm 0.51 ) , but has a similar intercept .
This behavior remains even after restricting to a sample of only early type galaxies or after removing the 8 brightest cluster galaxies .
The M _ { \bullet } - \sigma relation shows more modest differences when splitting the sample based on the other environmental indicators , suggesting that they are driven by the underlying satellite/central fractions .
Separate relations for centrals and satellites are also seen in the power law scaling between black hole mass and bulge stellar mass or bulge luminosity .
We suggest that gas rich , low mass galaxies undergo a period of rapid black hole growth in the process of becoming satellites .
If central galaxies on the current M _ { \bullet } - \sigma relation are representative progenitors of the satellite population , the observations imply that a \sigma = 120 { km } { s } ^ { -1 } galaxy must nearly triple its central black hole mass .
The elevated black hole masses of massive central galaxies are then a natural consequence of the accretion of satellites .