Equation to give the lookback time as a function of redshift

In summary, the lookback time can be calculated as a function of redshift using cosmological equations that account for the expansion of the universe. The equation incorporates the Hubble parameter and the matter-energy content of the universe, allowing astronomers to determine how far back in time we are observing based on the observed redshift of distant astronomical objects. This relationship is essential for understanding the history and evolution of the universe.
  • #1
happyparticle
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Homework Statement
Inverting ##z = H_0(t_0 - t_e) + (1 + \frac{q_0}{2}H_0^2(t_0 - t_e)^2)## to give the lookback time as a function of redshift ##t_0 - t_e = H_0^{-1}[z - (1 + \frac{q_0}{2})z^2]##
Relevant Equations
##H_0## is the Hubble's constant
##q_0## is the deceleration parameter
##z## is the redshift
Hi,
I'm currently reading the introduction to cosmology second edition by Barbara Ryden and at the page 105, the author says we get ##t_0 - t_e = H_0^{-1}[z - (1 + \frac{q_0}{2})z^2]## by inverting ##z = H_0(t_0 - t_e) + (1 + \frac{q_0}{2}H_0^2(t_0 - t_e)^2)##.

However, I can't figure out how she got this result.
Any help will be appreciate.

Thank you
 
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  • #2
happyparticle said:
Homework Statement: Inverting ##z = H_0(t_0 - t_e) + (1 + \frac{q_0}{2}H_0^2(t_0 - t_e)^2)## to give the lookback time as a function of redshift ##t_0 - t_e = H_0^{-1}[z - (1 + \frac{q_0}{2})z^2]##
Relevant Equations: ##H_0## is the Hubble's constant
##q_0## is the deceleration parameter
##z## is the redshift

Hi,
I'm currently reading the introduction to cosmology second edition by Barbara Ryden and at the page 105, the author says we get ##t_0 - t_e = H_0^{-1}[z - (1 + \frac{q_0}{2})z^2]## by inverting ##z = H_0(t_0 - t_e) + (1 + \frac{q_0}{2}H_0^2(t_0 - t_e)^2)##.

However, I can't figure out how she got this result.
Any help will be appreciate.

Thank you
I believe you have some typographical errors. The formula for ##z## should read $$z \approx H_0(t_0-t_e) + \left(\frac{1+q_0}{2} \right)H_0^2(t_0-t_e)^2.$$
This is an approximate expression that assumes ##H_0(t_0-t_e)## is small. So, the equation expresses ##z## to second order in ##H_0(t_0-t_e)##.

For convenience, let ##x = H_0(t_0-t_e)## and ##b = \large \frac{1+q_0}{2}##. So, we may write the relation as $$z \approx x+ bx^2$$ where ##x## is a small first-order term. When inverting this, you only need to get an approximate expression for ##x## in terms of ##z## that is accurate to second order in ##z##.

Can you see a way to do that?
 
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I can't see it. I tried a taylor's series but I don't get the same result.

I made a mistake. I think it works with a Taylor's series around z=0.

Thank you! I would not have seen it without your help.
 
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FAQ: Equation to give the lookback time as a function of redshift

What is lookback time in cosmology?

Lookback time is the time difference between the present and the time at which light from a distant object was emitted. It essentially tells us how far back in time we are observing the universe when we look at distant objects.

How is redshift related to lookback time?

Redshift measures how much the wavelength of light from a distant object has been stretched due to the expansion of the universe. The higher the redshift, the further back in time we are looking. Lookback time is a function of redshift, meaning that for a given redshift, we can calculate how long ago the light we are seeing was emitted.

What is the basic equation to calculate lookback time as a function of redshift?

The lookback time \( t_L \) as a function of redshift \( z \) can be calculated using the integral:\[ t_L(z) = \int_0^z \frac{dz'}{(1+z') H(z')} \]where \( H(z) \) is the Hubble parameter as a function of redshift, which depends on the cosmological parameters.

What are the cosmological parameters needed for the calculation?

The key cosmological parameters needed are the Hubble constant \( H_0 \), the matter density parameter \( \Omega_m \), the dark energy density parameter \( \Omega_\Lambda \), and possibly the curvature parameter \( \Omega_k \). These parameters define the Hubble parameter \( H(z) \) at different redshifts.

Can you provide an example of calculating lookback time for a specific redshift?

Sure! For example, if we assume a flat universe with \( \Omega_m = 0.3 \), \( \Omega_\Lambda = 0.7 \), and \( H_0 = 70 \, \text{km/s/Mpc} \), the lookback time for a redshift \( z = 1 \) can be approximated by numerical integration of the equation:\[ t_L(1) \approx \int_0^1 \frac{dz'}{(1+z') \sqrt{0.3(1+z')^3 + 0.7}} \]Performing this numerical integration yields a lookback time of approximately 7.8 billion years.

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