33_-_Microwave_Background - The Cosmic Microwave...

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The Cosmic Microwave Background, CMB 2 Objectives • Investigate the CMB in terms of: 1. temperature 2. spatial distribution • Where do the ripples come from? • What can we learn from the ripples about the early Universe? • What’s next? http://background.uchicago.edu/~whu/physics/tour.html 3 Universe is hot, electrons are free, light scatters off electrons until ~380,000 years after BB. Universe is cooler e - and p + form hydrogen Light travels freely A Brief History of the Universe 4 Graphic from WMAP website
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5 The First Detection (McKellar 1940) • There was absorption in the CN R(1) line, something was “heating” the CN molecules. • The temperature implied was 2.3K. • The importance was not recognized for more than two decades. Intensity Wavenength R1 R0 6 Graphic from WMAP website 7 Only if You’re NOT on Cable! • 400 photons per cubic cm ! Graphic by Wayne Hu, http://background.uchicago.edu/~whu/beginners/introduction.html 8 1965 1992 2003 2007 Discovery COBE WMAP The History of CMB Observations
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9 The Frequency Spectrum • Universe was almost in equlibrium so the radiation is almost a blackbody at 3,000K. • We observe a near (to within 10
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This note was uploaded on 04/05/2009 for the course ASTRO 3332 taught by Professor Houck,j during the Spring '09 term at Cornell University (Engineering School).

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33_-_Microwave_Background - The Cosmic Microwave...

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