4
$\begingroup$

By lookback time distance I mean the same as light-travel distance. Can it be calculated from just knowing the redshift?

$\endgroup$

4 Answers 4

5
$\begingroup$

No you can't. Other information is required.

For low redshifts - let's say smaller than 0.1 - and by that I mean the wavelength increases by 10 percent, you might get away with using Hubble's law to estimate the distance and then get the look back time by dividing by the speed of light. $$ t \simeq \frac{\lambda - \lambda_0}{H_0 \lambda_0},$$ where $H_0$ is the present day Hubble parameter of about 70 km/s per Mpc, $\lambda$ is the measured wavelength and $\lambda_0$ is the rest wavelength.

So far so good, you just need to know $H_0$. However for larger redshifts it gets horribly complicated because the Hubble parameter changes with time in a way that depends on the curvature of the Universe and hence on the cosmological parameters defining the matter density and dark energy density.

There is indeed a highly complicated, non- linear formula involving integrals that I will look up a reference for. But possibly the better way to proceed is to use a simple look-up table produced from such calculations with certain assumed values for ratios of matter and dark energy densities with respect to the critical density; a.k.a. $\Omega_M$ and $\Omega_{\Lambda}$.

The plot below is an example taken from http://www.astro.caltech.edu/~eran/MATLAB/Cosmology.html which shows look back time versus redshift for two different cosmologial models (but with the same value of $H_0$). The curves are very different at high redshifts, but converge at small redshifts.

Here is a cosmological calculator that can do the job for you. Enter the redshift and your assumptions about the Hubble parameter and other cosmological parameter and it will tell you the age of the universe at that redshift as well as the lookback time.

Lookback time versus redshift

$\endgroup$
1
$\begingroup$

@RobJeffries has covered most points, but just to add a little. The lookback distance is directly proportional to the cosmological time elapsed since emission, whereas the cosmological red-shift depends on [basically] how much scale factor, which is a function of cosmological time, has changed since emission. If the Universe has been expanding for its history up to the present then the scale factor to present will be a strictly increasing function of cosmological time, so there will be a one-to-one correspondence between red-shift and lookback distance. NB this will not be true if, for example, the Universe was initially expanding but is currently contracting.

However how the scale factor changes is governed by the stress-energy of the contents of the Universe so the relationship between red-shift and lookback distance will not generally be simple.

$\endgroup$
1
$\begingroup$

Lookback time, T, and distance, D, can be calculated from the object’s redshift, z, and cosmological parameters.

Lookback time, or (less appropriately) light travel time, answers the following similar questions:

-How old are the photons presently recorded in the object's spectrum?

-How long did it take the light to traverse the distance between the object and the observer?

-What distance did the light have to travel through an expanding universe in order to arrive at the present time?

-When we observe a remote object, how far back in time do we see?

The relation between redshift and lookback time is quite complex, and is presented here with simple equations derived by regression analysis from actual results. Correlation coefficients are better than 0.999. The equations are based on the following cosmological parameters:

Omega Matter = 0.272

Omega Radiation = 8.12E-5

Omega Lambda = 0.728

Hubble Constant now = 70.4

The result is given in billions of years (By)

T = ( 19292 x Z ) / ( 1.3878 + Z ), for Z between 0 and 0.2

T = ( 0.589 + 13.87 x Z^1.25 ) / ( 0.852 + Z^1.25), for Z between 0.2 and 20

Solving the second equation for quasar APM 8279, with Z = 3.911, T = 12.10 By

Lookback time also describes the distance the quasar's light travelled through an expanding universe before reaching the observer. This lookback time distance, D, determines by how much the object's light intensity falls off due to distance and due to intergalactic medium extinction.

D = C x T, where C = 1, describes D in light years,

D= ( C x T ) / 3.26, where C = 1, describes D in parsecs

$\endgroup$
2
  • 1
    $\begingroup$ The lookback time can't be calculated knowing only the redshift. You also need the cosmological parameters, as you say yourself (and as stated in the answer by Rob Jeffries, four years ago). $\endgroup$
    – pela
    Commented May 16, 2019 at 19:06
  • 1
    $\begingroup$ You are absolutely correct. I edited my post accordingly. $\endgroup$ Commented May 18, 2019 at 2:23
1
$\begingroup$

One way is this:

d = -(1 / (1 + z) - 1) c / H_0

I added this as the red line to Rob's image:

enter image description here

I noticed that when you compare redshift z to the energy observed, that while positive values of z can go all the way to infinity, that negative values only go to -1. Making the range were z is an actual redshift is infinitely larger than the range where is considered a blue shift.

enter image description here

The situation is reversed when you invert the equations of redshift, for example:

b = E_obs / E_emit - 1

Now blueshifts are infinite and redshifts only go to -1:

enter image description here

I found that with this difference in range of values, a negative blueshift distance relation could be attempted:

d = -bc / H_0

And it looks pretty useful. Since:

b = 1 / (1 + z) - 1

Then:

d = -(1 / (1 + z) - 1) c / H_0
$\endgroup$

You must log in to answer this question.

Not the answer you're looking for? Browse other questions tagged .