Cosmology W13 - Physics Department, UCSB

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Plan • Part 0: basic phenomenology (today; L2-‐4) • Part I: the (smooth) average universe (L5-‐10) • Part II: the growth of fluctuaôns (L11-‐L15) • Part III: very early universe (L20) • Part IV: class presentaôns
Some useful concepts/units • Parsec (pc) = distance that gives a parallax of 1 arcsecond ~3.08e16m • Solar Mass = 2e30kg • Solar Luminosity = 3.8e26 W • Redship z=λ/λ 0 -‐1 M
Page 1 and 2: Lecture 1: January 9 2013 Cosm
Page 3 and 4: Physics 236 • Textbook: - Gala
Page 5 and 6: Physics 236: the big quesôn
Page 7 and 8: Physics 236: more specifically
Page 9 and 10: Tradiônal Observaônal Foundaôn
Page 11 and 12: Physics 236: open problems with
Page 13: Cosmological Principle • Physic
Page 17 and 18: Olbers’ paradox. The night sky
Page 19 and 20: Olbers’ paradox. What does the sk
Page 21 and 22: Olbers’ paradox. The Big-Bang sol
Page 23 and 24: Cosmic Microwave Background
Page 25 and 26: Cosmic Microwave Background
Page 27 and 28: Anisotropies of the CMB BenneZ
Page 29 and 30: Basic Phenomenology: LSS
Page 31 and 32: Basic Phenomenology: galaxies
Page 33 and 34: Basic Phenomenology: galaxies
Page 35 and 36: Spiral galaxies • Like our ve
Page 37 and 38: Luminosity funcôn
Page 39 and 40: Stellar mass funcôn What about
Page 41 and 42: Examples of cluster in the op^
Page 43 and 44: Examples of cluster in the X-
Page 45: The end

Cosmology W13 - Physics Department, UCSB

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