Coordinate Distance of Object at Redshift z: Solving w/ k=0, n<1

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In summary, the conversation discusses finding the coordinate distance of an object seen at a redshift z in a universe with k=0 and (a/a_0) = (t/t_0)^n where n<1. The solution involves using the equation r=\frac{ct_0}{(1-n)a_0}[1-(1+z)^{1-1/n}] and integrating with respect to time, taking into account the factor of n.
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Logarythmic
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Homework Statement


For a universe with [tex]k=0[/tex] and in which [tex](a/a_0) = (t/t_0)^n[/tex] where [tex]n<1[/tex], show that the coordinate distance of an object seen at redshift z is

[tex]r=\frac{ct_0}{(1-n)a_0}[1-(1+z)^{1-1/n}][/tex].2. The attempt at a solution
I have used

[tex]r=f(r)=\int_{t}^{t_0} \frac{cdt}{a(t)}=\frac{ct_0}{(1-n)a_0}\left(t_{0}^{1-n}-t^{1-n}\right)[/tex]

but then what? I know that [tex]1+z=\frac{a_0}{a}[/tex] but I can't get it right.
 
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You're missing a power of "n".
[tex]f(r)=\int_{t}^{t_0} \frac{cdt}{a(t)}=\frac{1}{a_0}\int_{t}^{t_0}\fract_0^n t^{-n}dt= \frac{t_0^n}{a_0(1-n)}\left(t_0^{1-n}- t^{1-n}\right)[/tex]
 

Related to Coordinate Distance of Object at Redshift z: Solving w/ k=0, n<1

1. What is the equation for calculating the coordinate distance of an object at redshift z?

The equation for calculating the coordinate distance of an object at redshift z is:
DC = c/H0 * ∫0z [1/√(Ωm(1+z)^3 + ΩΛ + Ωk(1+z)^2)] dz
where c is the speed of light, H0 is the Hubble constant, Ωm represents the matter density, ΩΛ represents the dark energy density, and Ωk represents the curvature density.

2. What does the value of k=0 signify in the equation?

The value of k=0 signifies a flat universe, where the total density of matter and energy is equal to the critical density. In this case, the curvature density (Ωk) is equal to 0 and the equation for calculating the coordinate distance simplifies to:
DC = c/H0 * ∫0z [1/√(Ωm(1+z)^3 + ΩΛ)] dz.

3. What is the significance of having n<1 in the equation?

Having n<1 in the equation indicates a universe with a decelerating expansion rate, also known as a matter-dominated universe. This means that the matter density (Ωm) is greater than the dark energy density (ΩΛ). As the universe expands, the matter density slows down the expansion due to its gravitational pull, resulting in a decelerating expansion rate.

4. Can the coordinate distance of an object at redshift z be measured directly?

No, the coordinate distance of an object at redshift z cannot be measured directly. It can only be calculated using the equation mentioned above, which takes into account various parameters such as the Hubble constant and the density parameters of the universe. However, it can be indirectly measured through observations of the object's redshift and the expansion rate of the universe.

5. How does the coordinate distance of an object at redshift z relate to its luminosity distance?

The coordinate distance and luminosity distance of an object at redshift z are related by the following equation:
DC = (1+z)*DL,
where DL is the luminosity distance. This means that the coordinate distance is equal to the luminosity distance multiplied by a factor of (1+z). This factor takes into account the stretching of light due to the expansion of the universe, and thus, the coordinate distance is always larger than the luminosity distance for objects at the same redshift.

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