Astr/Phys 328/428 Homework #1
1. Volume of the
Step 1: Find
the volume of the
Universe out to a comoving distance r. Using the Robertson-Walker
metric, we can define the differential volume element as
which means the volume out to a comoving distance r is given by
Solve to get an analytic expression for V(r) for k=-1,0,1.
Step 2: Find the relationship between comoving distance r (which you've
calculated the volume for, but is unobservable) to redshift z (which is
Start by using the R-W metric and integrating along the path of a light
ray. Do this exercise
using a flat, matter dominated OmegaM=1 universe, remembering that R(t)~t2/3 in such a universe. While
this cosmology is certainly not the correct one, it is a useful
"benchmark" to compare to (and it is analytically tractable!). This
should give you a relationship
like this: r=f(R,t0). Then use the Lemaitre equation and the expression for t0 to turn it into
Step 3: Combine the relationship
in steps 1 and 2 to show that
- V(z) is different in different universes. For
example, using the same techniques, but with messier math, we can show
that for an empty (i.e., non-Lambda, OmegaM=0) universe, the volume is
While for positively curved, OmegaM=2 universe
- On one figure, plot the volume (in Mpc3) out to
a redshift z
in each universe, from z=0 to z=3. Use H0=70 km/s/Mpc for these
calculations and also use the astropy cosmology package to overplot the
volume in a LCDM universe with OmegaM=0.3 and OmegaL=0.7.
- If the distribution of galaxies in the universe
homogeneous, now plot the
relative number of galaxies you see (per unit redshift) at a redshift z as a function
of redshift in each of those four cases.
- If you could see all bright galaxies in the universe out to a
z=2, what would the median
redshift of the galaxies be in these four universes? Explain
qualitatively why this makes sense.
- Why is this test (called the count-redshift
test to perform? Think about observational issues, as well as the underlying physical assumptions behind the test.
2. Lookback Times and Age Constraints
Use either the astropy cosmology package or Ned Wright's Cosmology Calculator for this exercise.
3. The Flatness of the Universe
- It's 1990. You are a good, party-line
that Omega=1, and that there is no such thing as the cosmological
You also "know" that globular clusters are 14-16 Gyr old. What can you
say about H0?
- A few years later, you decide that the
measurements of H0
are getting better, so you need to believe them. So take H0=55, and
me what constraint you can place on Omega. What about if you believe
- And then Hipparcos comes along (around 1997)
that GCs are further away -- this means the ages of the globular
clusters get revised
downwards to 11-13 Gyr. Why does
the further distance mean a younger age? At the same time, you
decide, for better or worse,
that you like H0=65. Now what
constraints can you place on Omega?
- Later, in 1998 the high redshift galaxy
It lives at a redshift of z=1.55, and its was determined to have a
age of 3.5 Gyr. How does this
change your constraints on Omega?
- Six months later, the age of LBD53W091 was
and became 1.7 +/- 0.3 Gyr. NOW
how do your constraints on Omega change?
- Finally, this wacky Lambda idea starts to
off, so you
have to consider OmegaL as well. Given
your GC ages and H0, pick values
of OmegaL and, for those values, place limits on OmegaM. Make a plot of
your results on an OmegaL-OmegaM plane, showing regions of "allowed
your GC age constraints.
Starting with the Friedmann equantion for a Lambda=0 universe, show that the Hubble parameter can be written as:
- First, rewrite H in terms of rho0 and z.
- Then rewrite rho0 in terms of Omega0 and H0.
- Then rewrite the Friedmann equation as it is at z=0.
- Then combine together what you get via those three hints to get the expression we want.
Then use that to show that
- Start with writing Omega in terms of rho and H.
- Then substitute for H using the
expression you derived in the first part of the problem, and also
rewrite rho in terms of rho0 and z.
So we see that Omega varies with time. Now do the following:
- At large redshifts (ie in the early universe), show that the
Universe is essentially flat for any plausible choice of Omega0. Does
this argument also hold for universes with a cosmological constant?
- Take your expression for Omega(z) and rewrite it so that you
have an expression for Omega0 as a function of Omega(z) and z.
Calculate what Omega0 would be if, at a redshift of z=1000, Omega had
the value of 0.95, 1.000, or 1.001. What does this suggest about the
value for Omega?
this calculation twice. Once analytically for a OmegaM=1, OmegaL=0
universe (show your work!), and then use the astropy cosmology calculator to get the
values for a OmegaM=0.3, OmegaL=0.7 universe. Compare how the values differ in the different universes.
One of the most distant radio galaxies is 8C 1435+63, at a redshift of
z=4.25. Answer the following:
- How old was the universe at this redshift? Give the answer
both in years and in fraction of the age of the universe today.
- What is the present proper distance in Mpc?
- What was the proper distance when the light we see was
- What is the luminosity distance?
- What is the angular size distance? If the angular size of
the nucleus is 0.5", what is the linear size (in kpc) of the nucleus?
ASTR 428 additional items:
- Read the following (books on reserve in the Astronomy
A star cluster is made out of 106 solar-type
and is located 12 kpc from the Sun. It has a radius of 5 pc. Calculate
- Magnitudes & Colors: Zeilik, Gregory, and Smith
"Introductory Astronomy and Astrophysics", Chapter 11
- Stars: Zeilik, Gregory, and Smith "Introductory Astronomy
Astrophysics", Chapter 13-3
- Galaxies: Longair: 3.1-3.4, 3.7 (dont worry about the
The giant elliptical galaxy NGC 4874 sits at the center of
Coma cluster, has an apparent V magnitude of 11.73, and a B-V color of
0.87. Its effective radius is about 32 kpc. The recession velocity of
the Coma cluster is 7190 km/s. Calculate the following for NGC 4874:
- Its absolute V-band magnitude.
- Its apparent V-band magnitude.
- Its angular size (in arcseconds).
Using the relationship between magnitude and flux, show that
for small uncertainties, the uncertainty in magnitudes is essentially
the same as the relative flux error. In other words, show that
sigma(mag) ~ sigma(f)/f.
- Its distance modulus.
- Its B band luminosity (in solar luminosities).
- Its V band effective surface brightness (in magnitudes per