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Clusters of Galaxies in the Microwaves

Clusters of Galaxies in the Microwaves. Sunyaev & Zel'dovich Effect. Clusters of Galaxies in the Microwaves. CMB+CLUSTERS. Kinetic S-Z effect. Sunyaev & Zel'dovich Effect. Thermal S-Z Effect. Sunyaev & Zel'dovich Effect.

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Clusters of Galaxies in the Microwaves

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  1. Clusters of Galaxiesin the Microwaves

  2. Sunyaev & Zel'dovich Effect Clusters of Galaxiesin the Microwaves CMB+CLUSTERS

  3. Kinetic S-Z effect Sunyaev & Zel'dovich Effect Thermal S-Z Effect

  4. Sunyaev & Zel'dovich Effect 1) SZ effect depends on the projection of n along the line of sights 2) SZ effect is independent of redshift dI/d=0 1) Combination of SZ and X-ray observations gives important information on the gas structure ; Combination of SZ and X-ray observations provide information on the cluster Distance (estimate of H0) 2) SZ observations allow to observe (in principle) all the clusters in the universe

  5. Sunyaev & Zel'dovich Effect

  6. SZ Observation Techniques • Single dish • Bolometric array • Interferometer

  7. The OVRO (Owens Valley Radio Observatory)40-Meter and 5.5-Meter Telescope

  8. APEX-SZ • 330 element transition edge sensor (TES) monolithic bolometer array • 0.4 degree field of view • Single color observations at 2 and 1.4 mm wavelengths • Single-moded horn coupled array for RF and stray light shielding • SQUID readouts on individual bolometers • Survey 200 square degrees to 10 micro-K_CMB sensitivity per 0.8' pixel in two seasons at 2 mm wavelength • Single detector NET of 350 micro-K √ s • Pulse-tube cooler-based cryostat to eliminate liquid cryogens

  9. SuZIE The Sunyaev-Zel'dovich Infrared Experiment The SuZIE experiment measures the Sunyaev-Zel'dovich effect at multiple frequencies between 150 and 350 GHz, from the Caltech Submillimeter Observatory on Mauna Kea in Hawai'i.

  10. OVMMA (Millimeter-Wavelength Array)

  11. The Planck Mission

  12. The Planck Mission

  13. Cosmology with SZ Clusters

  14. SZ sky of Known Clusters Mazzotta 903 clusters

  15. SZ sky including all clusters not detected in X-rays Mazzotta 85,537,821 clusters M>1.E13

  16. Cold Fronts: implications for the kinetic SZ Effect and the CMB polarization Diego, Mazzotta, Silk, ApJL

  17. Kinetic SZ Effect and CMB Polarization

  18. Signal Variation with respect to the“Classic SZ effect”

  19. 300 km/s T=9keV; V=1500 km/s M=1 Dg/g=26 Polarization Dg/g=5 SZ DS/S=13 DS/S=2.5

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