Sparky_ said:
Phinds –
I understand we can see / measure back 13.7 billion light years.
I am asking about is it possible to calculate how big the “entire universe” is – how big it is today –
I was thinking one could use the expansion rate and say it has been expanding for 13 billion years and so on?
Bottom line – I’m asking about the seen +unseen volume or radius.
Thanks
-Sparky_
There was a NASA report a few years back that gave a lower bound ASSUMING the entire thing was finite and analogous to the surface of a sphere (but 3D).
An earlier poster pointed out that infinite volume is a reasonable assumption, and you can assume that and base your calculations on that. But then you don't get any finite answer.
So what they did was present the data that they had collected in two different ways. Assuming infinite, and also assuming that spatially it would resemble the 2D surface of a sphere but would be 3D----it would be a hypersphere with a certain curvature and a certain circumference.
And then they calculated in effect a LOWER BOUND on the size with 95% confidence. They found that with 95% confidence the circumference of this thing would have to be AT LEAST
650 billion light years.
That is, if you could freeze the expansion process today (so the circumf would not change while you were measuring) and send a flash of light off in one direction, it would take at least 650 billion years for it to get back to you from the other direction, having made a tour.
Something like 650. Maybe 630, I don't remember exactly.
Keep in mind that this figure is derived from the data on observed curvature and it is ASSUMING that she is spatially finite----like the surface of a 2D balloon, where the inside and the outside of the balloon do not exist, all existence is on the 2D surface---and then think of the 3D analog of that.
Basically creatures that live on a 3D hypersurface have a hard time telling if it is an infinite "flat" 3D or if it is just very very big and very slightly curved hyperspherical hypersurface.
The measurement/estimation of largescale curvature is delicate and difficult. One methode is by counting galaxies at each distance and seeing how the number changes with distance.
If there is slight positive curvature then the number you find at distance R will not grow quite as fast as R
2. But if she is infinite it will grow like R
2. the difference could be very slight.
If you want a link to the technical report, just say. The paper was by Komatsu et al (many big names Spergel, Wright, ...) and this info was embedded in a table with a lot of other results of analyzing the 5-year data from the WMAP mission mapping the microwave background.