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Measuring Cosmic Expansion

Posted August 18, 2010 11:00 PM by Jorrie
Pathfinder Tags: cosmic expansion Redshift

To know the expansion curve is to know a lot about cosmic expansion, e.g., the age of the universe and the distance to galaxies with a measured redshift.

The expansion curve is normally drawn for the cosmic expansion factor a(t) against cosmic time. The expansion factor is just a measure of by how much smaller (in terms of ratio) the cosmos was at some time in the past. It is very simply related to the redshift factor (z), as is clear from the right- and left-hand axes of the graph, i.e: 1 + z = 1/a(t). The redshift factor z is the change in wavelength, expressed as a fraction of the original wavelength emitted.

Curve (i) is a plot for the perfectly parabolic expansion of the Einstein-de Sitter model, where matter density exactly equals the critical density for a 'flat' cosmos. Curve (ii) is for the present Lambda-Cold-Dark-Matter model, where normal plus dark matter together makes out about 25% of the critical density and the rest is vacuum energy (Einstein's cosmological constant). Both curves were plotted for a Hubble constant H0 ≈ 72 km/s/Mpc.

The two black bullets, where the z=1 line cuts the two curves respectively, represent a galaxy that is observed at redshift z=1. The markers now(i) and now(ii) represent the age of the universe according to the respective models (about 10 and 14 billion years respectively). The two arrows s1 and s2 are the look-back distances of the galaxy according to the two models, roughly 6 and 8 billion light-years. This, according to the model employed, is the distance that light has traveled since being emitted. It is not the 'real distance' of the galaxy, which has changed over time due to the cosmic expansion.

In order to determine the shape of the expansion curve, cosmologists measure the redshift of a large number of galaxies, near and far. This alone is however not good enough - they also need the look-back distance (or time), which is easier said than measured. The distance to many stars in our own galaxy can be measured by means of parallax over the course of a year, as Earth moves around the Sun. Other galaxies pose a problem though - at their distances the parallax is just too small to be of any use. This is where proper motion, Cepheid variable stars and supernovae come in.

The way these standard methods are being utilized to build a 'distance ladder' is quite intriguing, but a bit too lengthy to describe here. At the risk of infuriating loyal readers, I'll have to refer you to a .pdf or a .doc (about 9 pages in length) on my website, containing a non-technical description of each method.

Jorrie

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#1

Re: Measuring Cosmic Expansion

08/20/2010 1:40 AM

Jorrie, nice article, but I've got a basic question - hope you don't mind my woolly-headedness, because I think you have explained this before!

According to Hubble's law, a specific redshift should be equivalent to a specific distance - it is km/s per Mpc, which is equivalent to redshift per million light years, is it not?

I can see the 6 and 8 billion light years on your diagram, but I can't understand how those values relate to Hubble's law.

SL

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#2
In reply to #1

Re: Measuring Cosmic Expansion

08/20/2010 4:36 AM

Hi SL, you asked about Hubble's law: "I can see the 6 and 8 billion light years on your diagram, but I can't understand how those values relate to Hubble's law."

Hubble's law only holds well for small redshift (up to z=0.1, or so), where we can use the approximations z ≈ v/c and look-back distance s ≈ 978 z / H0. For higher redshift, H0 is just a constant in a more complex equation. The only accurate way that I know of is to numerically integrate the full 'equation of motion' of cosmic expansion and then extract the look-back distance from the data. This is what the cosmological calculator does for us.

There is however a reasonable Doppler approximation, as described in the original full .pdf, equations 16.1, 16.21 and the calculations that follow after them.

-J

Note 1.

The complexity shown here arises from extracting apparent recession velocity from redshift in the relativistic case.

H0=71 km/s/Mpc has clearly been used, not the 65 mentioned in the original text. That's what the balloon says in the eBook...

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#3
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Re: Measuring Cosmic Expansion

08/21/2010 1:30 AM

Jorrie, it makes some sense, thanks.

What still has me puzzled is the velocity that I calculate from your equations 16.1, 16.2. For z=1 it comes out as 0.6c. However, when I use your cosmic calculator for z=1, it gives two recession speeds, one for 'now' (0.79c) and one for 'then' (0.66c). I suppose it means the recession speed was 0.66c when the light left the galaxy and the recession speed of that galaxy is now 0.79c due to the accelerated expansion? But, the 0.6c from the equation does not fall in this range, so what the heck is it supposed to represent?

I understand that 16.2 is an approximate (empirical?) equation, but the form looks like Doppler shift and for Doppler shift the velocity must mean something.

Another puzzle is why the two different models that you pictured, using the same Hubble constant, give such widely different ages for the cosmos (10 and 14 b.yr). I thought Hubble time (1/H_0) is Hubble time, irrespective of model.

SL

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#4
In reply to #3

Re: Measuring Cosmic Expansion

08/21/2010 5:17 AM

Hi SL, you wrote: "But, the 0.6c from the equation does not fall in this range, so what the heck is it supposed to represent?"

In short: it is the relative (opening) speed in free, non-expanding space that will give a Doppler shift ratio of z = Δλ/λo = 1 (a 100% Doppler shift). The cause of the cosmological redshift is not quite a Doppler shift, IMO, although there are cosmologists who prefer to describe it as an accumulation of a large number of tiny Doppler shifts, all along the path of the photons. What's more, they do get the right answer, so in a way it is just a different interpretation of the observables. That's fine with me.

But, equation 16.2 is indeed empirical for the cosmological application and it only works closely for the present values of the ΛCDM model. As you can easily check, it will not work for the flat, matter-only case (like in the very distant past) and it will also not work in the very distant future, when the cosmological constant presumably completely overshadows all other energies. We just happen to live in an epoch where equation 16.2 works reasonably well, it seems.

Hubble time (tH = 978/H0 Gyr) actually has little bearing on the age of the universe, because the age also depends on all the energy densities, which changed over the history of the universe. It is (perhaps) a coincidence that today the predicted age of the cosmos is very close to tH = 978/71 = 13.8 Gyr. It has to do with the nearly linear top part of expansion curve (ii) (pasted again below). Curve (i) is parabolic all the way, so the argument does not work there.

Hope this clears some issues.

-J

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#5
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Re: Measuring Cosmic Expansion

08/24/2010 11:55 AM

Tx again.

When I have more time, I'll look into this fascinating stuff again :)

SL

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Re: Measuring Cosmic Expansion

08/26/2010 8:12 PM

This was an elegant answer in my opinion for is said there are two ways to skin a cat, and the cat may well be either a kitten, or an old cat.

Then there may be many cats.

We are not in agreement far as multiple universes, and I can't read equations, but if I could read Absolam Absolam and understand it, I can read this stuff, and understand it.

Thing I really like about this Jorrie post is that it is very pragmatic, concise, and you need to read it closely to get the sense of it.

It also shows an openness to new ideas, I was wondering about. Now I see that Jorrie where Jorrie is coming from a bit better.

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