C M B S e c o n d a r y A n i s o t r o p i e s a t

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C M B S e c o n d a r y A n i s o t r o p i e s a t R e i o n i z a t i o n Detecting distant clusters with lensing of the OV Effect Jose M. Diego & D. Herranz, 2008 (IFCA, Santander, Spain)

Ionized cloud CMB SZt (nT) SZk, OV (nV) Bremstrahlung or FF and Relativistic electrons (n2T-0.5) Thomson scattering of CMB photons also produce polarization

Polarization Double scattering CMB quadrupole Kinetic polarization Kamionkowski & Loeb 1997 Lavaux, Diego, Mathis & Silk 2004

N = No(1+z)3

Z = 14

Z = 7.5

Z = 3.9

Z = 2.5

Z = 1

Z = 0.15

Z = 0

Z OV Z SZ

CMB and the OV effect V z ~ 10 Observer Dark Ages CMB at z=1100

Science with the OV effect Probes re-ionization history. Anticorrelates with 21-cm line (SKA, LOFAR) Can be used as a background for lensing studies. Detection of high-redshitf clusters or proto-clusters Estimation of masses of clusters. Crucial for cosmology studies A new window to study the end of the “Dark Ages”.

Small scale anisotropies due to the OV effect Similar to Kinetic SZ but due to reionization. Strength of signal depends on reionization history. Few microK on scales of 10-30 arcsec. Posible detection with next generation experiments. 6 arcmin

Lensing by a galaxy cluster

Lensing by galaxy clusters Direct way to measure total mass (baryonic and non-baryonic). Masses necesary for cosmological studies. Needs high resolutions Lensing studies have been dominated by optical data. Are observations of lensing of CMB anisotropies realistic ?

Ostriker Vishniac effect 6 arcmin

Ostriker Vishniac effect 6 arcmin

Ostriker Vishniac effect 6 arcmin

Optimal Filters (Stokes Parameters) Q U

Optimal Filters (2D maps) Q U

Example of optimally filtered data (noise+beam) OF data OV effect

RESULTS Signal-to-noise depends on cluster masses and instrumental noise. Massive distant clusters should be seen by experiments with 0.3 microK per arcmin.

RESULTS Signal-to-noise depends also on the angular resolution of the experiment. Resolutions of 10 arcsec or less are necessary to observe the effect.

But, point sources will be the main limiting factor. RESULTS But, point sources will be the main limiting factor. Sources need to be removed down to the microJy level.

But can we see this at all ? Not yet but soon. One needs: High resolution. 50 meter or larger antena Or interferometers. Today’s standard. High sensitivity. 0.2 microK per arcmin or better. Improve one order of magnitude. Point source substraction. About a hundred point sources need to be removed or accounted for per arcminute. Biggest challenge but possible with interferometric techniques. ALMA ?

Conclusions OV effect can be used as a background source for lensing studies of galaxy clusters. Optimal filters can be designed to improve the detection rate of lensing signals. This signal could be detected with ALMA ? Same technique can be applied to 21-cm line background. V E R Y E X C I T I N G Y E A R S A H E A D !

Science Fiction Science is Here Let’s destroy the entire Universe ! What should we do with all this new technology Spock ? We are out of photonic torpedos !