# How was matter in other parts of the universe affected by the Big Bang and inflation in an infinitely sized universe?

I'm trying to understand how the idea of an infinite universe with presumably infinite matter works with the Big Bang and inflation.

I understand that if the universe is infinite, then it's always been infinite, and that when we talk about the initial universe being very very small, dense and hot we are referring to the observable universe (correct me if I'm wrong). So let's say in our infinitely sized universe, there's a galaxy (Graham's Number)^(Graham's Number)^(Graham's Number) light years away, or some huge distance like that.

Would this galaxy have also been very close, hot and dense with our observable universe? If so, what if I just keep increasing the distance since I've assumed the universe is infinitely big? And if not, would it have had its own separate big bang?

So my question is how really really far away regions of the universe were affected by the big bang, if the universe is infinite since they couldn't have all been close to each other in a very hot and dense state.

• Go incomprehensibly big. How about Tree(Graham's Number) light years away? May 19, 2020 at 21:37
• In a hypothetical “infinite” universe, using the Friedmann metric, any two separate regions, no matter how close to each other at the moment of the Big Bang, are causally disconnected. The existence of anything other than the initial infinitely small point of our observable universe is moot, non-falsifiable, and therefore unphysical. In the Friedmann cosmology, there is no directly observable difference between finite and infinite versions of the universe. See this for details: physics.stackexchange.com/questions/456071/… May 19, 2020 at 23:09
• when we talk about the initial universe being very very small, dense and hot we are referring to the observable universe (correct me if I'm wrong) That’s incorrect. May 20, 2020 at 3:49
• May 20, 2020 at 9:12

Penrose's basic construction is to connect a countable sequence of open Friedmann–Lemaître–Robertson–Walker metric (FLRW) spacetimes, each representing a Big Bang followed by an infinite future expansion. Penrose noticed that the past conformal boundary of one copy of FLRW spacetime can be "attached" to the future conformal boundary of another, after an appropriate conformal rescaling. In particular, each individual FLRW metric $$g_{a b}$$ is multiplied by the square of a conformal factor $$\Omega$$ that approaches zero at timelike infinity, effectively "squashing down" the future conformal boundary to a conformally regular hypersurface (which is spacelike if there is a positive cosmological constant, as is currently believed). The result is a new solution to Einstein's equations, which Penrose takes to represent the entire universe, and which is composed of a sequence of sectors that Penrose calls "aeons".