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The Early Universe I

The Early Universe I. AST 112. Review: Hubble’s Law. Space is expanding in all directions This is carrying everything away from everything else This does not apply to objects that are bound by gravity When light is emitted by an object, it travels in expanding space

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The Early Universe I

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  1. The Early Universe I AST 112

  2. Review: Hubble’s Law • Space is expanding in all directions • This is carrying everything away from everything else • This does not apply to objects that are bound by gravity • When light is emitted by an object, it travels in expanding space • Its wavelength gets stretched • It becomes more red

  3. The Age of the Universe • Galaxy A is 1 MLY (9.46 x 1018 km) away and receding at 22 km/s (6.94 x 108 km/yr). At that speed, how long has it been expanding away from us? 13.6 billion years • Galaxy B is 2 MLY away and receding at 44 km/s. At that speed, how long has it been expanding away from us? 13.6 billion years

  4. The space in which galaxies live has beenexpanding since the beginning. Everything has been expanding awayfrom everything else. If we “rewind”, what happens?

  5. The Early Universe • Galaxies hadn’t formed when the Universe was significantly more crammed than it is • But there was still plenty of matter and energy. What would it have been like?

  6. The Early Universe • Nuclear physicists at Princeton were starting to figure this out • Hot, dense primordial “fog” of H and He • George Gamow calculated that the fog in the early universe could only consist of H and He • Not able to fuse into heavier elements

  7. Looking Back In Time If the Universe used to be a thick, glowingfog of hydrogen and helium, shouldn’t we beable to see the glow? (What color is a hot, dense objectat 6000 oF?)

  8. Looking Back In Time Photons leftover from the hydrogen fog are everywhere. We can observe them.Why can’t we walk outside and see it?

  9. The Early Universe • So what do we see when we look at the youngest galaxies? • H and He! • What do we see when we try to look past the youngest galaxies? • We run into the fog! • The fog is opaque. • The fog is redshifted into microwaves. • So there’s a glowing fog that we cannot see (not in visible light), into which we cannot see. • So what do we see?

  10. Looking Back In Time • Can only look so far back • Universe used to be opaque • Can’t see light from before then • Particle physics and computers tell us what happened beyond where we cannot see

  11. An Annoying Hiss, A Pigeon, and the Early Universe • Arno Penzias and Robert Wilson (1965): • Set up a sensitive microwave antenna for satellite communications • Kept finding “noise” in all directions

  12. An Annoying Hiss, A Pigeon, and the Early Universe

  13. An Annoying Hiss, A Pigeon, and the Early Universe

  14. An Annoying Hiss, A Pigeon, and the Early Universe

  15. An Annoying Hiss, A Pigeon, and the Early Universe

  16. An Annoying Hiss, A Pigeon, and the Early Universe After tightening screws, removing the pigeon,and removing the pigeon again…The hiss remained!

  17. An Annoying Hiss, A Pigeon, and the Early Universe • Penzias and Wilson planned to “bury” this nuisance in a paper • Meanwhile: • Princeton physicists calculated characteristics of radiation from Big Bang • Should fill the Universe, can see it in all directions • Should be detectable with…

  18. … a microwave detector!

  19. Cosmic Microwave Background (CMB) • On an airplane trip, Penzias sat by someone who knew of the Princeton calculations • “Compared notes”: This “noise” in the antenna IS the leftover radiation from the Big Bang!

  20. Cosmic Microwave Background (CMB)

  21. Cosmic Microwave Background (CMB) • This is an image of “hydrogen fog radiation” over the entire sky

  22. Cosmic Microwave Background (CMB) • 1990’s: COBE launched • Cosmic Background Explorer • The curve is the expected thermal spectrum • The points are what COBE measured

  23. Cosmic Microwave Background (CMB) This graph is exactly what we wouldexpect for a single mass of hot plasma that cooled off.

  24. Cosmic Microwave Background (CMB) • If you take an antenna-fed TV: • Turn to a channel for which there is no local station, and you get snow • 1% of this snow is from photons in the CMB

  25. Receding CMB • The particles responsible for the CMB are 45.7 billion LY away • The observable universe ends at 62 billion LY • As space expands, the CMB will disappear from the observable universe!

  26. The Big Bang • The two strongest, most cited pieces of evidence for the Big Bang: • Hubble expansion • Cosmic microwave background

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