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“ The truth would be literally nothing but the shadows of the images.”

Fundamental Cosmology : 1.Introduction. “ The truth would be literally nothing but the shadows of the images.” -Plato, The Republic (Book VII). 1.1: A Very Brief History of Time. 宇宙論に求めたいのは？ How did the Universe Begin ? How old is the Universe ? How big is the Universe ?

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“ The truth would be literally nothing but the shadows of the images.”

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  1. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 Fundamental Cosmology : 1.Introduction “ The truth would be literally nothing but the shadows of the images.” -Plato, The Republic (Book VII)

  2. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.1: A Very Brief History of Time 宇宙論に求めたいのは？ • How did the Universe Begin ? • How old is the Universe ? • How big is the Universe ? • Where are we in the Universe ? • What is the Universe made of ? • Will the Universe end ?

  3. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.1: A Very Brief History of Time How did the Universe BEGIN ? How OLD is the Universe ?

  4. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 10-43s 1031K 10-35s 1027K 10-12s 1015K 10-6s 1013K 10-4s 1012K 0.01s 1011K 1s 109K 4s 5x109K 3mins 109K 3x105yrs 3000K 107yrs 300K 109yrs 30K 1010yrs 2.73K He q+ m+ n Matter Clumping W± ? n m- Zo q- n n Atoms Initial Singularity Formation of Solar System and Birth of Life Hadron-Lepton Reactions shift -> Proton First Stars and Galaxies (re-ionization) Primordial Nucleosynthesis quark - antiquark annihilation Epoch of Galaxy Formation Epoch of Recombination n-p ratio freezes E-W Phase Transition Planck Time m- m+ annihilation ne decouple Inflation 0.1: A Very Brief History of Time t=0 T=∞

  5. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.2: The Scale of the Universe How BIG is the Universe ?

  6. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.2: The Scale of the Universe Deeper and Deeper

  7. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1026 1024 1021 1018 1016 1013 1011 108 104 100 10-3 10-6 10-9 10-10 10-12 10-15 10-18 10-35 1.2: The Scale of the Universe

  8. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang WHERE are we in the Universe ?

  9. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang 町 My Town Greenwich グリニッジ市 20km

  10. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London グリニッジ市 ロンドン ロンドン大都市 London 100km

  11. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England グリニッジ市 ロンドン イギリス 英国 United Kingdom 100km

  12. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth グリニッジ市 ロンドン イギリス 地球 The Earth 地球 6400km

  13. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Solar System グリニッジ市 ロンドン イギリス 地球 ソーラーシステム Solar System ソーラーシステム 太陽 - 地球 地球 1A.U.~1.5x1011m~7lm

  14. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang 天の川 オリオン渦巻腕 （うずまき） Greenwich London England Planet Earth Solar System Spiral Arm of Orion グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕 The Milky Way 1000ly 太陽

  15. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Solar System Spiral Arm of Orion The Milky Way Galaxy グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕 天の川銀河系 The Galactic System 天の川銀河系 10,000ly 50kpc ngc2997l 太陽 http://www.anzwers.org/free/universe/

  16. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Solar System Spiral Arm of Orion The Milky Way Galaxy The Local Group グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕 天の川銀河系 局部銀河群 局部銀河群 （きょくぶぎんがぐん） The Local Group 0.5Mpc ~ 1.6x106ly

  17. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Solar System Spiral Arm of Orion The Milky Way Galaxy The Local Group near the Virgo Cluster グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕 天の川銀河系 局部銀河群 乙女座の銀河団の辺　 乙女座の銀河団の辺 （おとめざのぎんがだん） The Local Neighbourhood 50x106ly 局部銀河群 http://www.anzwers.org/free/universe/

  18. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 近い宇宙 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Soalar System Spiral Arm of Orion The Milky Way Galaxy The Local Group near the Virgo Cluster Local Supercluster グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕天の川 天の川銀河系 局部銀河群乙女座の銀河団の辺 局部超銀河団 Local Supercluster 局部超銀河団 （きょくぶちょうぎんがだん） 108ly 乙女座の銀河団の辺

  19. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.3: From the Solar System to the Big Bang Greenwich London England Planet Earth Solar System Spiral Arm of Orion The Milky Way Galaxy The Local Group near the Virgo Cluster Local Supercluster THE UNIVERSE グリニッジ市 ロンドン イギリス 地球 ソーラーシステム オリオンの渦巻腕 天の川銀河系 局部銀河群 乙女座の銀河団の辺 局部超銀河団 宇宙　〒０００　００１ 宇宙 The Universe 109ly 3000Mpc http://www.anzwers.org/free/universe/

  20. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe WHAT is the Universe made of ?

  21. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 100,000th Hubble 90億光年QSO HDF (ISO 15mm) Mk241 (VSOP) 3C216 (VSOP 5GHz) GALEX M51 visible UV g-線 microwave Sub-mm 電波 X-線 赤外 波長 1cm 1mm-200mm 100nm 1km-1m 200mm-2mm 700-400nm 1nm 0.1A COBE HDF (SCUBA 850mm) HDF 1.4: The Multiwavelength Universe

  22. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe 電波波長 : n = 3x102 - 3x109 Hz : l = 1000km - 10cm : E=1peV - 0.01meV • Examples • Cas A supernova remnant • Radio galaxies (e.g. Cyg A) • Sgr A (the Galactic centre) • Extragalactic Populations • AGN (Quasars) • Radio Galaxies (Ellipticals) • Starburst Galaxies (Spirals)

  23. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe マイクロ波波長 : n = 3x109 - 3x1011 Hz : l = 10cm - 1mm : E=0.01meV - 1meV • Examples • Orion Nebula Masers • Megamaser in NGC 4258 • CMB • Extragalactic Populations • CMB

  24. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe Sub-mm 波長 : n = 3x1011 - 1.5x1012 Hz : l = 1mm - 200mm : E~1meV - 6meV • Examples • Galactic Centre Sgr* • Dusty Galaxies • Extragalactic Populations • Ultraluminous Galaxies • Starburst Galaxies

  25. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe 遠赤外線 波長 : n = 1.5x1012 - 5x1013 Hz : l = 200mm - 7mm : E~6meV - 200meV • Examples • Orion Nebula • M82 • ARP220 • Extragalactic Populations • Normal Galaxies • Starburst Galaxies

  26. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe 赤外線　波長 : n = 5x1013 - 3x1014 Hz : l = 7mm - 1mm : E~0.2eV - 1eV • Examples • Old Stars • Globular Clusters • Extragalactic Populations • Elliptical Galaxies • Normal Galaxies (Buldges)

  27. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe 光　波長 : n = 3x1014 - 7x1014 Hz : l = 1mm - 0.4mm : E~1eV - 3eV • Examples • Stars • Galaxies • Extragalactic Populations • Normal Galaxies

  28. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe UV　波長 : n = 7x1014 - 3x1016 Hz : l = 4000Å - 100Å : E~3eV - 100keV • Examples • Hot Stars • Quasars • Extragalactic Populations • Starburst Galaxies • Quasars

  29. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 Red = low energy Green = medium energy Blue = high energy Supernova remnant Cassiopeia A (Chandra) 1.4: The Multiwavelength Universe X-線　波長 : n = 3x1016 - 3x1020 Hz : l = 100Å - 0.01Å : E~0.1keV - 1MeV • Examples • Accreting Binary Systems (inc. Black Holes) • Active Stars • Clusters of Galaxies • AGN • Extragalactic Populations • AGN & Quasars

  30. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 COMPTEL instrument onboard NASA's orbiting Compton Gamma Ray Observatory EGRET (CGRO) catalog 1991 Gamma-ray intensity is represented by a false color map - low (blue) to high (white). The brightest source, the Crab pulsar (near the plane of the Galaxy on the far right) The Vela pulsar (from the Crab, more than halfway toward the galactic center) The galactic center Black hole candidate Cygnus X-1 (near the plane, halfway from the center to the left edge) Distant gamma-ray emission due to distant active galaxies (above and below the plan) 1.4: The Multiwavelength Universe g-線　波長 : n = 3x1020 - 3x1023 Hz : l = 0.01Å - 10-5Å : E ~ 1MeV - 1GeV • Examples • Crab Pulsar • GRBs • 3C273 • Extragalactic Populations • AGN • BL Lacs/Blazars

  31. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 Optical light spans barely an order of magnitude !! 0.4: The Multiwavelength Universe n=1030 Hz l=10-15m E=109eV n=102 Hz l=106m E=10-12eV ~30 powers of 10

  32. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe • THE MULTIWAVELENGTH MILKY WAY

  33. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe • THE MULTIWAVELENGTH MILKY WAY

  34. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 OPTICAL (Colour) INFRARED (IRAS) OPTICAL (DSS) Dust lanes within central regions of the galaxy. Obscuring dust near the nucleus scatters light. Orthogonal stretch due to rectangular shape of IRAS detectors. VLA/MERLIN interferometry reveals the chaotic structure of emission from M82. X-ray emission is concentrated in the central region. Bright spots are supernova remnants and MXB. Diffuse emission = hot outflow gas Young blue stars preferentially born within the arms of a spiral galaxy. Most luminous region is the center of Galaxy. The ring is also clearly visible. Not strong X-ray source. Many of bright spots are distant AGN The central core of Andromeda and the ring bright (red=bright). Spatial distribution of radio emission tracks IR emission A pair of narrow "jets" shooting out from nucleus. Orientation perpendicular to dust disk. Central peak of long-wavelength emission is stretched along the same orientation as the dust disk. X-ray jet extends 25kly. Dimmer jet extends opposite direction (geometry effect). SBH at centre? An obscuring band of dust and young stars (右上) more like a spiral galaxy. Dust band is heavily warped. M82 looks like normal edge-on galaxy. Typical spiral galaxy: bright central bulge, spiral arms Bright stellar content of the galaxy looks like an elliptical galaxy RADIO X-RAY 1.4: The Multiwavelength Universe THE CHANGING FACES OF GALAXIES M82 Starburst Galaxy M31 Andromeda Galaxy Centaurus A Radio Galaxy http://coolcosmos.ipac.caltech.edu/cosmic_classroom/

  35. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 I band B V I Red circles - sources in the 6.7umcomplete sample Pink circles - sources in the 6.7um supp. sample Green circles - sources in the 15um complete sample Cyan circles - sources in the 15um supp. sample SCUBA ISO 15um Green - complete Blue - supp Green - complete Blue - supp ISO 7um 1.4: The Multiwavelength Universe Hubble Deep Field

  36. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.4: The Multiwavelength Universe The Cosmic Background Radiation

  37. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.5: Summary HOW can we find out more ?

  38. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.5: Summary Cosmology seeks to answer such questions about the Universe Only ONE Universe !! Unfortunately only have one experiment The Evolution of Cosmology has gone hand-in-hand with what we can see ! • Early Cosmology: Limited to visible light • 1800 Herschel discovers IR radiation • 1801 Johann Ritter discovers UV radiation • 1931 Karl Jansky shows our galaxy emits radio waves • 1948 Rocket Experiment detects X-rays from the Sun For the COMPLETE picture of the Universe require: • observation at all wavelengths • Observations from Ground and Space

  39. Chris Pearson : Fundamental Cosmology 1: Introduction - ISAS -2003 1.5: Summary 終 Fundamental Cosmology 1. Introduction 次： Fundamental Cosmology 2. Homogeneity & Isotropy

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