1. The Big Bang The Big Bang
Tempature and density history of the Universe
Cosmic Background Radiation
Contents of the Universe

2. Big Bang
Our conclusion that the Universe actually began at some point in time is based on extrapolating back the observed Hubble expansion of galaxies
Is there any other evidence?

3. Big Bang
If the Universe was smaller in the past, but had roughly the same amount of matter and energy, then the density of matter and energy must have been higher in the past.

4. The Universe was hotter in the past
lower T
higher T
Temperature is proportional to the average kinetic energy per molecule
k = Boltzmann constant = 1.3810-23 J/K = 8.6210-5 eV/K

5. Big Bang

6. Big Bang

7. Big Bang

8. Big Bang First protons and neutrons at about 1 second.
Helium nuclei formed at about 100 seconds.
Observed ratio of Helium/Hydrogen matches Big Bang prediction.
Universe is opaque.

9. Opaque

10. Big Bang
At one million years, electrons combine with nuclei and atoms form.
Universe becomes transparent.

11. Transparent
Transition occurs at around T = 3740 K.

12. Cosmic Microwave Background
The Universe glows at 2.7 K in every direction.

13. CMB
Discovered by Arno Penzias and Robert Wilson in while employed by AT&T’s Bell Labs and attempting to find the source of noise in an antenna used to bounce telephone signals bounced off metallic balloons high in the atmosphere.
They won the Nobel prize in 1978.

14. CMB
Radiation is a blackbody spectrum originally emitted at 3000 K but red shifted by a factor of 1000.

15. Three pieces of evidence for the Big Bang model
Hubble expansion: galaxies are moving away from us with speed proportional to distance.
The cosmic microwave background: a 2.7 K glow seen in all directions.
The ratio of Helium to Hydrogen in gas clouds unaffected by stars.

16. Cosmic Microwave Background
Small fluctuations are due to sound waves at recombination.

17. Fluctuations in CMB
Properties of the CMB are set by physics of ionized plasma at ~4000 K – well known physics.
Temperature variations in the Cosmic Microwave Background (CMB) are observed to be about K, agrees with calculations of sound waves propagating through plasma.
The expected physical size of the hot/cold regions can be calculated. What can we do with this?

18. Angular size in curved space
We can draw triangles!
Angles in triangles in curve space do not equal 180°.
This affects the angular size

19. Angular size of CMB fluctuations
In positively curved Universe, fluctuations appear larger than calculated
In negatively curved Universe, fluctuations appear smaller
In flat Universe, fluctuations appear at expected size

20. Curvature of the Universe
The curvature of the Universe is determined by the density parameter 0
0 < 1  negative curvature
0 > 1  positive curvature
Measurement of CMB fluctuations gives

21. Contents of the Universe
Normal matter
Stars
hot gas
anything made of atoms
Total is 4% of C

22. Rotation curve of Milky Way

23. Mass of the Milky Way

24. Dark Matter Dark – it doesn’t produce light (any kind)
Does have mass, produces gravity
Nature is unknown
Most likely it is elementary particles

25. Contents of the Universe
Normal matter is 4% of C
Dark matter is 23% of C
Total of normal and dark matter is M = 0.3
But, we need 100% of C since Universe is flat
Remainder, 73%, is “Cosmological constant” or “dark energy”  = 0.7

26. Contents of the Universe

27. Why can't we see radiation produced during the first 300,000 years after the Big Bang?
It was absorbed soon after it was emitted.
It hasn't reached us yet.
It has been deflected by black holes.
It passed by our part of the universe a few billion years ago.

28. Review Questions Give three pieces of evidence for the Big Bang model.
What will happen to the Universe if the density is less than the critical density?
A few seconds after the big bang did hydrogen atoms exists? Why or why not?