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We present a multiscale approach for measurements of galaxy density, applied to a volume‐limited sample constructed from the Sloan Digital Sky Survey Data Release 5 (SDSS DR5). We populate a rich parameter space by obtaining independent measurements of density on different scales for each galaxy. This parametrization purely relies on observations and avoids the implicit assumptions involved, e.g. in the construction of group catalogues. As the first application of this method, we study how the bimodality in galaxy colour distribution (specifically   u − r  ) depends on multiscale density. The   u − r   galaxy colour distribution is described as the sum of two Gaussians (a red and a blue one) with five parameters: the fraction of red galaxies ( f  red ) and the position and width of the red and blue peaks ( μ red , μ blue , σ red   and σ blue ). Galaxies mostly react to their smallest scale ( &lt;0.5 Mpc ) environments: in denser environments red galaxies are more common (larger  f  red ), redder (larger  μ red  ) and with a narrower distribution (smaller σ red ), while blue galaxies are redder (larger  μ blue  ) but with a broader distribution (larger σ blue ). There are residual correlations of  f  red  and  μ blue   with  0.5–1 Mpc  scale density, which imply that total or partial truncation of star formation can relate to a galaxy's environment on these scales. Beyond  1 Mpc (0.5 Mpc  for  μ red  ) there are no positive correlations with density. However  f  red   anticorrelates  with density on  &gt;2 Mpc  scales at fixed density on smaller scales, and  μ red   anticorrelates with density on  &gt;1 Mpc  scales. We examine these trends qualitatively in the context of the halo model, utilizing the properties of haloes within which the galaxies are embedded, derived by Yang et al. and applied to a group catalogue. This yields an excellent description of the trends with multiscale density, including the anticorrelations on large scales, which map the region of accretion on to massive haloes. Thus we conclude that galaxies become red only once they have been accreted on to haloes of a certain mass. The mean colour of red galaxies  μ red   depends positively only on  &lt;0.5 Mpc  scale density, which can most easily be explained if correlations of  μ red   with environment are driven by metallicity via the enrichment history of a galaxy within its subhalo, during its epoch of star formation.

A multiscale approach to environment and its influence on the colour distribution of galaxies