The consequences of using a smooth cosmic distance in a lumpy universe:
  II
  How do we appropriately fit a model based on an idealised
Friedmann-Lema\^itre Robertson-Walker (FLRW) spacetime to observations made
from one location in a lumpy Universe? We address this question for the
apparent magnitude of Type 1A supernova (SN1A) and the acoustic peaks in the
density field. We show that distance in a perturbed universe is given by the
FLRW spacetime on average, except in the immediate neighbourhood of an
observer. We demonstrate how this distinction impacts the determination of the
Hubble rate and the SN1A absolute magnitude.
