That sounds a lot like how entangled particles can't be used to communicate faster than light.

While you can make observations immediately, you can't turn them into useful information about the other end, at least not until you get missing data which has to reach you by normal means.

Hence the focus on using entangled particles as a kind of tamper-detector or "reusable random one-time pad", rather than for transmitting information.

Two entangled wormhole apertures function as Star Trek style transporter pads. Feed mass into one hole, scanning it as it goes in. Transmit the pattern to another aperture of the hole, using electromagnetic energy at the speed of light, and when that end ejects a mass, apply the pattern to it, so it resolves into an exact copy of what you put in.

The distance the mass travels may be shorter than the distance the energy travels, but it can't resolve exiting mass as that object until the information--that had to travel at the speed of light--arrives.

So you could potentially use a wormhole as a suicide machine that transports a copy of you, that thinks it actually is you, to a distant location no faster than the speed of light, in zero subjective time for the thing that will then think it's you.

Is that a reasonable interpretation?

Edit:Lol, someone else also had this link as a reply to a similar thought.

doesn't our universe expand at the same speed?

At least theoretically we should be able to receive signals from arbitrarily far away no matter the expansion of the universe. They'll be redshifted like hell though, as you say.

Space is dynamical. It can stretch and expand and even break, but it doesn't move. The result of this is a cosmological horizon that prevents these objects from communicating, because the distance between them is growing faster than light can cross it. This is the same reason you can't escape a black hole.

Astronomers in different galaxy clusters will agree that each sees a set of cosmological horizons, but do not agree on where it is and what's inside it.

Schematically:

    th<--g1<--<--yh--Them<--->You-->th-->g2-->yh

Every point in an expanding universe has its own set of cosmological horizons non-identical to its neighbouring points, and dramatically different from points at great distances in spacetime (that goes for great gaps in time at the same spacelike location, and great gaps in space at the same lookback time or scale factor).

For astrophysical black holes, a black hole horizon localizes around a particular clump of matter, and not around other nearby clumps of matter. Far from a super-dense clump of matter you will not find an astrophysical black hole horizon (barring primordial black holes, for which there is no evidence anyway).

Cosmological horizons focus on each infinitesimally small clump of matter, everywhere in the universe, even in deep extragalactic space where matter is extremely sparse. Indeed, even matter-free points have their own cosmological horizon, and we do have substantial evidence supporting that.

A theoretical black hole horizon arises in a family of solutions of the Einstein Field Equations, from exact ones like Schwarzschild or Kerr, to solutions that become those asymptotically (in the limit as a black hole formed by gravitational collapse ages, for example -- Schwarzschild and Kerr are eternal black holes that are never in an uncollapsed state).

A cosmological horizon arises in a different family of solutions of the Einstein Field Equations, from exact ones like the de Sitter vacuum or the expanding Robertson-Walker vacuum, to solutions that become those asymptotically (these are vacuum matter-free solutions, and one can get there with a solution with matter that dilutes away over time).

The two families of solutions are very different, although there is an overlap of solutions for black holes in expanding spacetimes, where there can be both a black hole horizon (or horizons) and a cosmological one (or more than one).

We can compare these different families of solutions most strikingly using the behaviour of test particles scattered through the spacetimes: near the BH event horizon particles may be entrained into stable circular orbits around the horizon of a theoretical black hole like Schwarzschild or Kerr, whereas this never happens around a cosmological horizon in a solution like de Sitter or expanding Robertson-Walker: the test particles all plunge right through the observer's horizon radially.

Once through the BH horizon a test particle will inevitably and very quickly by its own "wristwatch" collide with the gravitational singularity after passing through extremely curved spacetime. Our galaxy cluster has already passed through many cosmological horizons centred on distant galaxies who are now outside our horizon too. Neither our galaxy cluster nor the many distant ones have changed their essentially exclusive time-like trajectories, and there is no evidence we are soon going to end up colliding with a gravitational singularity. (Current evidence doesn't suggest we are going to end up facing a big rip either).

Now, in the cosmological model under time reversal galaxy clusters do tend to converge and naively collide and collapse into a singularity eventually. However, galaxies all plunge into it radially and matter does not get entrained into any sort of accretion disc or similar structure. (They disintegrate into clouds of gas and dust that heat up into the "un-recombination" surface of ionizing atoms (mostly hydrogen) which gets denser and hotter until neutrons and protons disintegrate, electroweak symmetries emerge, and so on, all at once. Black holes usually get to swallow clumps of matter from time to time, whereas the time-reversed big bang singularity gets everything landing on it all at once, rather than some clumps early, and some clumps earlier still).

Physically realistic models built on these theoretical systems are grossly different; the models are good for predicting future things in our sky, so we expect the astrophysical reality is different too.

The rough similarities tend not to survive real inspection. Different horizons are different in a bunch of ways that aren't overcome by the few ways in which they are somewhat similar (or similar under time-reversal).

Spatial discontinuities? Can you tell us more, please?

https://www.youtube.com/watch?v=9crggox5rbc

If you speed up, you can finish the race in the same amount of time. Light always finishes the race in the same amount of time from each observer's perspective. It can always speed up because it's massless, but you have mass and there is a limit to how much you can speed up. According to general relativity, an observer outside of the racetrack won't see light change speed, nor will you. But both of you will perceive distortions of space and time to accommodate light's "change in speed" to make it look as if nothing's changed.

Back to the cosmological horizon... We don't see a big jump in the racetrack because the distance between 100m and 200m isn't too massive; likewise, gravity and other forces hold objects together even though space is expanding and pulling them apart.

But there is a certain distance where gravity and other forces can't keep things together. Where that 1000k becomes a 10000k. The pull from one galactic cluster to another is just too weak. Anything past this point is moving away from us. That's why only galaxies close to us aren't redshifting away. But any observer anywhere in the universe would observe that they are at the epicenter of an expansion where everything is moving away from them.

I'd suggest clarifying this statement because it certainly gave me the wrong impression…

https://en.wikipedia.org/wiki/Metric_expansion_of_space