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GRAVITATIONAL LENSING

GRAVITATIONAL LENSING. History, Discovery and Future Measuring Mass of Dark Matter. Vahe ’ Petrosian Stanford University Yerevan, April 23, 2009. Measuring Mass In the Universe. HOW? 1. Visible Ordinary Matter: Stars and Galaxies Measure light, Infer Mass

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GRAVITATIONAL LENSING

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  1. GRAVITATIONAL LENSING History, Discovery and Future Measuring Mass of Dark Matter Vahe’ Petrosian Stanford University Yerevan, April 23, 2009 Yerevan, Armenia

  2. Measuring MassIn the Universe HOW? 1. Visible Ordinary Matter: Stars and Galaxies Measure light, Infer Mass 2. Invisible Ordinary Matter: Hot Gas, Small Stuff X-ray Emission in Clusters of Galaxies 3. Dark Matter: a. How Much? b. What is it made of? WIMPS or MACHOS? Yerevan, Armenia

  3. Measuring MassIn the Universe HOW? 1. Visible Ordinary Matter: Stars and Galaxies Measure light, Infer Mass 2. Invisible Ordinary Matter: Hot Gas, Small Stuff X-ray Emission in Clusters of Galaxies 3. Dark Matter: a. b. What is it made of? WIMPS or MACHOS? Yerevan, Armenia

  4. Measuring MassIn the Universe HOW? 1. Visible Ordinary Matter: Stars and Galaxies Measure light, Infer Mass 2. Invisible Ordinary Matter: Hot Gas, Small Stuff X-ray Emission in Clusters of Galaxies 3. Dark Matter: a. b. What is it made of? WIMPS or MACHOS? Yerevan, Armenia

  5. Measuring Dark MatterNewton and Einstein Gravitational Influence 1. On Other Matter: Motions and Orbits Planets, Stars, Galaxies 2. On Light: Gravitational Lensing Arcs in Clusters of Galaxies Yerevan, Armenia

  6. A Brief History of Gravitational LensingBasis: Deflection of Light By Matter NEWTON (Optics 1704) “Do not bodies act upon light… and bend it?” SOLDNER (1801) Deflection of Light Einstein (1911)based on Special Relativity Yerevan, Armenia

  7. A Brief History of Gravitational Lensing EINSTEIN (1915) General Relativity Yerevan, Armenia

  8. A Brief History of Gravitational Lensing EDDINGTON (1919) Confirmation Double Image Yerevan, Armenia

  9. EINSTEIN’s RING If Source, Lens and Observer aligned CHOWLSON (1924) Ring Image EINSTEIN (1936); suggested by Mendel Ring Ang. Radius Yerevan, Armenia

  10. Star-Star Lensing: Einstein RadiusImage Magnification Magnification Probability of Alignment Einstein: Hopeless. Can scarcely approach alignment and resolve the ring. Yerevan, Armenia

  11. Galaxy Lensing: ZWICKY (1937) • Galaxy-Galaxy • Galaxy-Cluster “….difference in redshifts……will immediately betray the presence of gravitational lens effect” Yerevan, Armenia

  12. Revival of the Field RESDAL, KILMER, LIEBS (1963) Details, Measuring Hubble Constant, Mass BARNOTHY’s (~1967) Quasars as Magnified Seifert Galaxies Several PhD Thesis (Gunn, Petrosian, Kontowski) Dealing with Statistical Lensing Nowadays called WEAK LENSING Yerevan, Armenia

  13. OBSERVATIONS • DOUBLE QUASARS Walsh, Carswell and Weymann (1979) 2. ARCS IN CLUSTERS OF GALAXIES Lynds and Petrosian (1986) Originally Discovered Circa 1976 Yerevan, Armenia

  14. Discovery of Gravitational LensRoger Lynds and VahePetrosian: circa 1976 Yerevan, Armenia

  15. Hubble Space Telescope View Yerevan, Armenia

  16. Examples of Strong Lensing Galaxy at z =1.7 multiply imaged by a cluster at z = 0.4. A complete Einstein ring. Multiply imaged quasar (with time delays).

  17. Some Significant Applications 1. Arcs and Strong Lensing Mass & Distribution of Dark Matter 2. Weak Lensing from Image Distortions Large Scale Structure of Universe 3. Microlensing: Detecting ‘Dark Stars’ & Planets Yerevan, Armenia

  18. 1. ARCS & STRONG LENSING Mass of Dark Matter in Clusters (Bergmann \& Petrosian 1990) Distribution of Dark Matter Different than Hot Gas : Narrower and More Peaked (Saraniti & Petrosian 1997) Yerevan, Armenia

  19. Yerevan, Armenia

  20. 1. ARCS & STRONG LENSING Mass of Dark Matter in Clusters (Bergmann \& Petrosian 1990) Distribution of Dark Matter Different than Hot Gas : Narrower and More Peaked (Saraniti & Petrosian 1997) Yerevan, Armenia

  21. Hubble Image of Cluster and Arcs

  22. Reconstruction of Dark Matter Distribution (Tyson et al.) Yerevan, Armenia

  23. Dark Matter in a Merging Cluster From: Bradac et al. 2006 Yerevan, Armenia

  24. Weak Lensing of Distant Galaxies Simulation by S. Colombi (IAP, France). Lensing is sensitive to all matter

  25. Primary mirror diameter Field of view 0.2 degrees 10 m 3.5 degrees Keck LSST Large Area Synoptic Telescope Yerevan, Armenia

  26. Simulation of Lensing: Moving Clusters~Few Billion Years Clumpier Dark Matter Distribution Smoother Dark Matter Distribution From T. A. Tyson Yerevan, Armenia

  27. SDSS LSST Yerevan, Armenia

  28. 3.MICROLENSING:Finding Dark “Stars” or MACHOS The MACHO Project Yerevan, Armenia

  29. Microlensing:Finding Dark “Stars” or MACHOS Yerevan, Armenia

  30. Microlensing:Finding Dark “Stars” or MACHOS Yerevan, Armenia

  31. Some Observed Light CurvesFrom The Macho Project Yerevan, Armenia

  32. DETECTINGPLANETS with masses of a FEW EARTH MASSFrom Waumbgassen Yerevan, Armenia

  33. SUMMARY • Strong and Weak Gravitational Lensinghave proven to be one of the most important pillars ofModern Observational Cosmology and for measuring Dark Matter and Dark Energy • Microlensing has shown that Most of the Dark Matter is made of WIMPS And has the potential of discovering Rocky Planets Yerevan, Armenia

  34. Measuring Mass of the Sun Yerevan, Armenia

  35. Measuring Mass of The Milky Way Using Satellite Galaxies Yerevan, Armenia

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