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Galaxies
usually occur in galactic clusters or super-clusters, where from a few
tens to a few thousand galaxies move in huge orbits around some
gravitational center. But there are also galaxies inside the so-called
cosmic voids - just not too many of them.
For the purpose of this discussion we are going to consider two such
galaxies, sitting rather lonely inside a large void. So lonely that the
gravitational influence of other galaxies upon them are negligible and
we can say they just move with the Hubble flow. This means that they
should be drifting apart according to Hubble's law, at a speed of about
68 km/s per Mpc of their present separation.
To make things easy, let's say the two typical, identical galaxies (A
and B) are located near the center of the void and around 14.7 Mpc (or
47.5 million light years) apart. They should be receding from each other
at some 68 * 14.7 ~ 1000 km/s. Divide this by c (300,000 km/s) and we
get the expected redshift z=0.0033. This is the fractional increase
(Δλ/λ) in the wavelength of light emitted in one galaxy and observed in
the other, caused by cosmic expansion.
Now let's also say that astronomers living on a planet inside galaxy A
find, to their surprise, that galaxy B is observed at just about zero
redshift. This means the galaxy is neither receding from them, nor
falling towards them, just sitting at 47.5 Mly away. This could
obviously also mean that the galaxies are in circular orbit around each
other, because tangential speed will not show up in the redshift value.
If civilization and astronomy on that planet were to survive for
another million years, what do you reckon will happen to the redshift
observations between those two galaxies? Will they just remain at a
stable distance, or do you think the cosmic expansion will make them
move farther apart? No need for calculations, just give a gut-feel on
the possible outcomes.
-J
PS: I seem to have not tick all the boxes in the previous one, so it never showed up in the "New Blog Entries" list. Will try to remove the old one.
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