1. Learning Goals:
4. Complex Knowledge: demonstrations of learning that go aboveand above and beyond what was explicitly taught. 3. Knowledge: meeting the learning goals and expectations. 2. Foundational knowledge: simpler procedures, isolated details, vocabulary. 1. Limited knowledge: know very little details but working toward a higher level.
I will:
understand the properties of different types of galaxies.
understand how the universe came to be what we observe today.
understand how astronomers use astronomical objects (standard candles)
Understand how we use a distance ladder to estimate the size of the universe and to measure large distances in the universe.
understand how astronomers determine the age and size of the universe?.

2. Hi, I am a black hole. I live in the galaxy M37, ~55 million ly from earth near the Virgo cluster. I weigh 6.5 billion times more than the Sun and am bigger than the orbit of Neptune

6. Evidence for the Big Bang
The abundance of light elements, hydrogen and helium found in the universe exactly matches what theory predicts
Galaxies appear to be moving away from us at speeds proportional to their distance; this is “Hubble’s Law”
If the universe was initially very small, it would also be very hot and we should be able to find some remnant of the heat

7. 1. Big Bang Nucleosynthesis
The Big Bang was a very hot place. roughly 10 billion degrees
filled with a sea of neutrons, protons, electrons, anti-electrons (positrons), photons and neutrinos.
As the universe cooled, the neutrons either decayed into protons and electrons or combined with protons to make deuterium.
During the first three minutes of the universe, most of the deuterium combined to make helium. Trace amounts of lithium were also produced at this time. 
The predicted abundance of deuterium (25%), helium (24%) and lithium (.3%) is in very good agreement with observations and is another major triumph for the Big Bang theory.

8. 2. The Universe Is Expanding
So we run the clock backwards….

9. Cosmic Microwave Background Radiation
CMBR

10. the CMBR (part I):
1948
Gamov  early universe should be hot & dense
Should radiate as a black body
1949
Alpher and Herman  large redshift would stretch the wavelength into the IR, Microwave, and radio spectrum

11. Picture it:
1960s,
two physicists (Penzias & Wilson) studying the sky in radio wavelengths,
Their measurements showed a “peculiar noise”
They thought it was bird droppings…
After cleaning the antennae of all the bird poop, the “noise” remained…

12. Princeton physicist Robert Dicke realized that, with the technology available, we should just now be able to detect this redshifted radiation (the CMBR)…
When Penzias & Wilson heard of Dicke’s work, they realized that’s what they saw!
Still… as scientists, we don’t like to jump to conclusions…
We would like to have other observations confirm or reject this…

13. This CMBR should be all over the sky & come from everywhere…
Specifically, theory (math) predicted that it should look like the radiation coming from a black body at a temperature of ~ 3K (in the IR…)
1992,
COBE satellite
Measured black body radiation with a temp. of / K
So the average temperature of space is 2.725K or F

14. History of the CMB 1965: Penzias and Wilson
1992: Cosmic Background Explorer (CoBE) Satellite
2003: Wilkinson Microwave Anisotropy Probe (WMAP)
2013: Planck Satellite

16. EdPuzzle: Space Used to be Orange
On Canvas
Due at Midnight