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Cosmic collisions: dark matter, dark energy & inflation

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  1. Cosmic collisions: dark matter, dark energy & inflation Max Tegmark, Penn/MIT

  2. 100dpi

  3. Smorgasbord

  4. Measuring clustering

  5. exp9911 CMB 1992-94 2004

  6. February 11, 2003: Add WMAP results 105dpi CMB

  7. Boomzoom De Bernardis et al 2000, Lange et al 2000 CMB

  8. Boomzoom Tegmark, Jr., 2001 CMB

  9. History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

  10. CMB FRONTIERS: • Polarization • Small scales (AKBAR, CBI, Planck, APEX, ACT, SPT, …)

  11. Atacama Cosmology Telescope (ACT): Ground based experiment at Atacama desert, Chile. 150 GHz n= 145, 225 & 265 GHz. Scans only in azimuth with the ability to cross-link elevations. 1.4° FWHM=1.7, 1.1 & 0.93’. Sensitivity/pixel ~ 2, 8 & 16mK (64 nights of quality data). MBAC on ACT 1.7’ beam w/ 2X noise SZ Simulation PLANCK Team: D. Benford, S. Boughn, J. Chervenak, A. de Oliveira-Costa, M. Devlin, R. Doriese, L. Ferrarese, J. Fowler, M. Halpern, D. Hughes, J. Hughes, K. Irwin, B. Jain, N. Jarosik, R. Jimenez, J. Klein, A. Kosowsky, R. Lupton, A. Miller, H.Moseley, B. Netterfield, L. Page (P.I.), B. Partridge, H. Quintana, A. Reiseneggar, U. Seljak, D. Spergel, M. Spergel, S. Staggs, C. Stahle, M. Tegmark, L. Verde, T. Williams, G. Wilson, E. Wollack. More info at http://www.physics.upenn.edu/act

  12. Atacama Cosmology Telescope (ACT): Ground based experiment at Atacama desert, Chile. 150 GHz n= 145, 225 & 265 GHz. Scans only in azimuth with the ability to cross-link elevations. 1.4° FWHM=1.7, 1.1 & 0.93’. Sensitivity/pixel ~ 2, 8 & 16mK (64 nights of quality data). MBAC on ACT 1.7’ beam w/ 2X noise SZ Simulation PLANCK Measure the primary anisotropy beyond the WMAP & Planck resolutionlimits. Find galaxy clusters at z<1 through SZ effect. Measure the amplitude of the CMB gravitational lensing, and therefore probe the mass power spectrum at 1Mpc scales at z~1-2. Detect signature of reonization at z~15 through Vishniac effect. Find all extragalactic mm-wave point sources in 100(o)2 to a sensitivity of 1mJy. More info at http://www.physics.upenn.edu/act

  13. Boomzoom z = 1000

  14. Boomzoom z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  15. Boomzoom z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  16. Boomzoom z = 0 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  17. 000619 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

  18. 1parmovies LSS

  19. 1parmovies Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  20. 1parmovies CMB Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  21. 1parmovies CMB Clusters LSS Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  22. Boomzoom Lyman Alpha Forest Simulation: Cen et al 2001 LyaF Quasar You

  23. 1parmovies CMB Clusters LSS Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  24. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  25. Boomzoom Gravitational lensing Lensing

  26. Boomzoom Lensing

  27. Boomzoom Lensing

  28. Boomzoom Lensing

  29. Boomzoom Lensing

  30. distortion Lensing

  31. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  32. 000619 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

  33. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  34. Cmbgg OmOl

  35. Cmbgg OmOl Mark Whittle 2004

  36. Cmbgg OmOl

  37. LSS frontiers/SDSS propaganda

  38. APO SDSS

  39. 100dpi

  40. Cmbgg OmOl

  41. 100dpi

  42. 100dpi

  43. Cmbgg OmOl Cool new/imminent LSS-measurements: LSS • P(k) from full 2dF data set (~250k gals) • SDSS DR3 goes public this fall • P(k) from SDSS DR3 (>300k gals) • P(k) from SDSS LRG’s (Eisenstein et al) • Angular galaxy clustering from SDSS • Clustering dependence on SDSS galaxy properties (Zehavi et al) • SDSS LyaF analysis (McDonald et al, Seljak et al) • See also Pope et al (2003), Budavari et (2004)

  44. Cmbgg OmOl LSS Data & image processing by Robert Lupton & David Schlegel

  45. Cmbgg OmOl Angular clustering LSS

  46. Cmbgg OmOl Angular clustering LSS

  47. This was from just 400 square degrees: Dodelson et al 2002, for SDSS collab. Tegmark et al 2002, for SDSS collab. Now we have an order of magnitude more, and photometric redshifts.

  48. 1parmovies CMB Clusters LSS Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  49. Measuring parameters