TeethWhitener
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The average density of the Local group is about twice the average density of the universe (Ref1 Ref2). I’m curious now as to whether that counts as a big perturbation to the FLRW metric. My gut says probably but I’m not an expert.PeroK said:I don't think it's valid to apply Hubble's law at all, because the local group of galaxies is not a region of space with the average energy density of the universe as a whole. Hubble's law applies to the universe at the largest scale, where the average energy density applies, but not to every region of the universe, where different equations govern the local galactic kinematics.
Interestingly, Hubble derived his law using data for relatively close galaxies. How did he do this? Here's what Steven Weinberg says in The First Three Minutes:
His conclusion was that there is a "roughly linear relation" between velocities and distances. Actually, a look at Hubble's data leaves me perplexed how he could reach such a conclusion - galactic velocities seem almost uncorrelated with their distance ... In fact, we would not expect any neat relation of proportionality between velocity and distance for these 18 galaxies - they are all much too close. It is difficult to avoid the conclusion that ... Hubble knew the answer he wanted to get.
Which is what I was unsure about: when you say Hubble’s law doesn’t apply, do you mean that the recessional velocity is insignificant/of the same order as local astronomical velocities, or do you mean that, because GR is nonlinear, the metric of an FLRW background plus local matter is sufficiently qualitatively different from the flat FLRW metric that Hubble’s law, or an analog of it, can no longer be derived from the metric?