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University of Pennsylvania

The cosmic connection. From WMAP web site. Licia Verde. University of Pennsylvania. www.physics.upenn.edu/~lverde. History. You are here. Danielsson & t’Hooft talks. Cosmic archeology!. Expanding and cooling. Look inside Particle accelerators. (Wagner talk).

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University of Pennsylvania

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  1. The cosmic connection From WMAP web site Licia Verde University of Pennsylvania www.physics.upenn.edu/~lverde

  2. History You are here Danielsson & t’Hooft talks Cosmic archeology! Expanding and cooling

  3. Look inside Particle accelerators (Wagner talk) Exhibition in Pillared Hall Or.. theory… Russian doll looking at the sky

  4. Russian doll The cosmic connection: the big picture The cosmic connection: the details: an example.

  5. Matter (and energy) curves space-time 1915

  6. Vacuum energy L (also known as dark energy or cosmological constant) 1917 vacuum

  7. Humm.. Looks like the Universe is expanding My biggest blunder…..

  8. Some recent observations…

  9. A picture of the baby Universe 380,000 years after the big bang Cobe 1994 WMAP Today

  10. From W. Hu web site Fig. From WMAP web site

  11. Tiny ripples in density  seeeds of galaxies Hot and cold spots  Detailed statistical properties of these ripples tell us a lot about the Universe

  12. How’s that? The Universe back then was made of a very hot and dense “gas”, so it was emitting radiation This is the radiation we see when we look at the CMB Uniform , but with tiny (contrast x 100000) density (and temperature) ripples Ripples in a gas? SOUND WAVES! Truly a cosmic symphony… We are seeing sound! These tiny fluctuations, quantitatively, give rise galaxies We try to listen to the sound and figure out how the instrument is made Fundamental scale Fundamental mode and overtones like blowing on a pipe….

  13. Magnitude of temperature variations Size of spots smoothing + From WMAP

  14. Fundamental mode (Geometry) overtones (content, history) Primordial ripples

  15. From WMAP web site

  16. There is more mass than you can see!!! Abell 2218, direction of Draco (Hubble)

  17. Galaxy surveys: 2dF galaxy redshift survey

  18. How? Tools: statistics.

  19. accelerating decelerating Additional indications: Supernovae Standard candles Expansion history! Do like Hubble, just .. better Function of geometry and Content of Universe

  20. Figure from a scientific journal: Science for real Vacuum Energy density or Supernovae CMB Dark energy Galaxy survey Line of flatness Universe is FLAT

  21. The Universe is Flat From WMAP web site

  22. Looks curved Looks Flat !!??? . . Remember Inflation? What made the Universe so flat? What made the Universe so big? What made the universe so uniform? (Danielsson talk) What seeded the galaxies?

  23. We (and all of chemistry) are a small minority in the Universe. Components of Where’s the anti-matter? We do not know what 96% of the Universe is !

  24. Recap: We have a consistent and coherent picture of the Universe. “Things have clicked into place” Different observations agree quantitatively. They all point in the same direction: the “standard model” for cosmology The standard model for particle physics  The standard model for cosmology Some puzzles remain Baryons: where’s the anti matter? GUT? Dark matter: what is it? The standard model offers candidates If SUSY is discovered at colliders we could measure DM abundance and compare with cosmological results! Dark energy: not a clue…. Standard model predictions are 60 to 120 orders of magnitude larger than observations Inflation…

  25. the dark side of the Universe We have indications that: More than 90 % of the mass in the Universe is DARK About 85% of mass in the Universe is made of matter unknown to Earth About 80% of what’s in the Universe is not even matter!!!! We call it DARK ENERGY Wouldn’t it be nice to start figuring some of this out?

  26. The cosmic connection on all scales: example : neutrinos They ARE non-baryonic dark matter Only not all of it!

  27. There are neutrinos everywhere!!!! SuperNovae Relict from the big bang 3 per m Cosmic rays reactors accelerators

  28. 100’s million every second …? A neutrino needs to cross 200 Earths before having a chance to interact So… do not worry….

  29. They are incredibly Petite ? The standard model requires massless neutrinos But do they have mass?

  30. How does the sun Shines? Full details of how this happens called `Standard Solar Model’ How could we prove this? Detect and count solar neutrinos!

  31. To cut a long story short: Solar Neutrino Experiments First experiment by Davis et al in 1960’s Radiochemical Method (Chlorine): Found ~ 1/3 of `Standard Solar Model’ (SSM) rate

  32. The explanation? So they must have mass! At odd with the standard model prediction

  33. 2002: Got Nobel Prize Look at the ECFA exibition in Pillared hall for more neutrino stuff

  34. What you should take away: Cosmology and particle physics now are asking the same fundamental questions. They approach them in complementary ways THE END

  35. Further readings, figure sources etc. WMAP web site (basic): http://map.gsfc.nasa.gov/index.html WMAP web site (advanced): http://cmbdata.gsfc.nasa.gov/product/map/ 2dFGRS web page: http://www.mso.anu.edu.au/2dFGRS/ Scientific American article on CMB by Hu and White http://background.uchicago.edu/~whu/Papers/HuWhi04.pdf (in Scientific American February 2004) Wayne Hu web page: http://background.uchicago.edu/~whu/ Scientific American article on Supernovae: Scientific American vol. 290, February 2004

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