clusters of galaxies in the microwaves
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
Clusters of Galaxies
in the Microwaves
Clusters of Galaxiesin the Microwaves
Sunyaev & Zel'dovich EffectCMB+CLUSTERS
Sunyaev & Zel'dovich Effect
Thermal S-Z Effect
Kinetic S-Z effect
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
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
dI/d=0
Sunyaev & Zel'dovich Effect
SZ Observation Techniques
Single dish Bolometric array Interferometer
The OVRO (Owens Valley Radio Observatory)
40-Meter and 5.5-Meter Telescope
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
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.
OVMMA (Millimeter-Wavelength Array)
The Planck Mission
The Planck Mission
Cosmology with SZ Clusters
SZ sky of Known Clusters
903 clusters
Mazzotta
SZ sky including all clusters not detected in X-rays
85,537,821 clusters M>1.E13
Mazzotta
Cold Fronts: implications for the kinetic SZ Effect and
the CMB polarization Diego, Mazzotta, Silk, ApJL
Kinetic SZ Effect and CMB Polarization
2t
r
v
vgS
Signal Variation with respect to the“Classic SZ effect”
300 km/s
M=1
T=9keV; V=1500 km/s
Dg/g=5 SZ Dg/g=26 Polarization
DS/S=2.5 DS/S=13