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Phys 262 introductory slides

Phys 262 introductory slides. The Keck 10m Telescopes on Mauna Kea, Hawaii. Segments of the Keck 10m Telescope Mirror. Outline. Introduction (The “Golden age of cosmology”) The Big Picture The Edge of the observable universe The mysterious dark side. Part 1

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Phys 262 introductory slides

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  1. Phys 262 introductory slides

  2. The Keck 10m Telescopes on Mauna Kea, Hawaii

  3. Segments of the Keck 10m Telescope Mirror

  4. Outline • Introduction (The “Golden age of cosmology”) • The Big Picture • The Edge of the observable universe • The mysterious dark side

  5. Part 1 Introduction:The golden age of cosmology

  6. The APM (Automatic Plate Machine) Survey (1992) Sky positions of 2,000,000 Galaxies

  7. The Sloan Digital Sky Survey (to locate over 100,000,000 galaxies, 3D positions for 1,000,000) A simulation of just 65,000 Sloan galaxies

  8. June 5 2001: First release of Sloan data (50,000 galaxies)

  9. Sloan Survey Status Imaging (Galaxy positions on the sky) 47% Complete Jun 21 2002  47,000,000 galaxy positions Spectroscopy (3D galaxy positions) 34% Complete Jul 15 2002  340,000 galaxy positions

  10. Sloan Survey Status Imaging (Galaxy positions on the sky) 97% Complete Jun 27 2004  97,000,000 galaxy positions Spectroscopy (3D galaxy positions) 67% Complete Jun 27 2004  670,000 galaxy positions

  11. Sloan Survey Status Imaging (Galaxy positions on the sky) 107% Complete Mar 13 2005  107,000,000 galaxy positions Spectroscopy (3D galaxy positions) 68% Complete Mar 15 2005  680,000 galaxy positions

  12. http://sdss.org

  13. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 2009 Simulated 2003 Simulated

  14. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 Updated after WMAP announcement, Feb 2003 2009 Real Data! 2003 Simulated

  15. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 Updated after WMAP announcement, Feb 2003 2009 Real Data! 2006 Simulated

  16. WMAP 3-yr map

  17. WMAP 5-yr map

  18. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 Updated after WMAP announcement, Feb 2003 2009 Real Data! 2006 Simulated

  19. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 Updated after Planck announcement, 2013 2013 Real Data! 2006 Real Data! Simulated

  20. Maps of the microwave sky (the “edge of the observable universe”) Real 1993 March 17 2014! Updated after Planck announcement, 2013 2013 Real Data! 2006 Real Data! Simulated

  21. http://www.esa.int/esaSC/120398_index_0_m.html http://www.rssd.esa.int/index.php?project=planck http://bicepkeck.org/

  22. Mass inferred from lensing: Must have dark matter

  23. 1996

  24. Using Hubble’s new “advanced camera for surveys” June 2002

  25. http://hubblesite.org/ http://www.nasa.gov/mission_pages/hubble/main/index.html

  26. Some Future Plans LSST (Large-aperture Synoptic Survey Telescope) SNAP (Supernova / Acceleration Probe ) JDEM  WFIRSTWFIRST/AFTA James Bock / NASA Jet Propulsion LaboratoryImaging Cosmic Microwave Background Polarization with EPIC We propose to study a mission concept, the Experimental Probe of Inflationary Cosmology (EPIC), based on a single-aperture telescope and receiver with high-sensitivity polarization-sensitive detector arrays.

  27. Some Future Plans LSST (Large-aperture Synoptic Survey Telescope) SNAP (Supernova / Acceleration Probe ) JDEM  WFIRSTWFIRST/AFTA James Bock / NASA Jet Propulsion LaboratoryImaging Cosmic Microwave Background Polarization with EPIC We propose to study a mission concept, the Experimental Probe of Inflationary Cosmology (EPIC), based on a single-aperture telescope and receiver with high-sensitivity polarization-sensitive detector arrays.

  28. Keck Telescope Hubble ACS (Advanced Camera For Surveys)

  29. Part 2: The big picture

  30. What we know about the big picture 1) On large scales the matter in the Universe is spread out very smoothly (“Homogeneous”) Mean density: 2) The Universe is expanding Hubble law:

  31. The homogeneity of the Universe Galaxy Isotropy of the microwave background (from the “edge of the observable universe”) to one part in 100,000

  32. The homogeneity of the universe We are here Radial Direction Galaxy surveys

  33. The homogeneity of the universe We are here Radial Direction From 1986 Galaxy surveys

  34. The Hubble law

  35. Hubble Expansion Hot, Dense past

  36. Time The History of the Universe Today Anti-Gravity?*! Galaxy Formation Last Scattering Nuclear & HEP Inflation? Extra Dimensions? High Energy & Temp

  37. Time The History of the Universe Today Anti-Gravity?*! Galaxy Formation Last Scattering Nuclear & HEP Inflation? Extra Dimensions? High Energy & Temp Research at UCD in all these areas!

  38. Part 3: The Edge of the observable universe

  39. The Edge of the Observable Universe: As we look back in space we look back in time. We see: Light traveling from far away =from distant past Here & Now Long ago (about 14 Billion years) the Universe was so hot and dense it was opaque: The edge of the observable universe

  40. Properties of the Edge of the Observable Universe: Similar to surface of Sun at time of emission • Today: • Only 2.726K above absolute Zero • “Microwave Radiation” (The “Cosmic Microwave Background”: CMB) • 1,000,000 times weaker than ambient radiation in a pitch dark room. Here & Now

  41. Observing the Microwave Background, Past, present and future:

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