Zeldovich-Sakharov program at RATAN-600

“Cosmological Gene” projectGround based support of the Space CMB Missions

Y.Parijskij et alSpecial Astrophysical Observatory

Russian Academy of Science

POSTER presentation, ORSAY, POLAR2005

Main Targets

• Sub-mK in Tb

• Sub-mJy in f.d.

• Up to confusion limit

• I,U,Q information

Main Targets

• Sub-mK in Tb

• Sub-mJy in f.d.

• Up to confusion limit

• I,U,Q information

Deep Synchrotron DATA at high bII

• Small l and WMAP interpretation• Result: WMAP polarization data should be corrected

• Synchrotron at Medium l (50-80) and Relic G.W. experiments

• Result: No problem for B-mode but at HFI only

• E-mode scale (l=1000) and Synchrotron• Result: No problem even at few cm.

CMB U,Q polarization

• History• Pulkovo Radio Telescope, 1968-1970• <1mK, 1arcmin scale, 3.2cm• RATAN-600, 1980-1981 DATA• <0.1mK, 4.5-9 arcmin scale, 7.6cm• RATAN-600, 1998-2000 DATA• <0.03mK, l=1000 scale, 3.9cm

• See ref. in http://www.brown.nord.nw.ru (“Cosmological Gene Project”, “CG” in M.Tegmark list)

Strategy

• Multi-frequency observations with l>1000 resolution in the Low Frequency part of the CMB Window

• “Extra-resolution approach”, much higher that CMB scales. It gives– Better Atmosphere filtration (near-field effect)– Better PS filtration (with up to 72000 beams /sq.deg)

– RATAN-600 has practically no aberration near local ZENITH and up to 3000 elements matrix receivers array may be used

Now and Future

• Three SKY regions were observed from 1980 to 2005, and they can be visible on the recent WMAP map in equatorial coordinates

Much greater than in WMAP experiment pixel integration time resulted in the high

pixel sensitivity • As an example, 2.7cm• Data are shown here, with

NET=3-5 mKs^1/2

• We are below WMAP now, but only white noise component is here.

From mK at dm to micro-K at cm

• We accumulated pixel sensitivity down to mK at 0.6GHz, 1GHz, 2.4GHz, 3.9GHz and for each pixel we have spectrum. Nearby pixels have the same spectrum, but there is big trend on the bigger scale. Now we can predict upper level of Galaxy polarization by only small extrapolation in frequency and with no extrapolation in scales

From Cl correction to the “Phase, Amplitude” one in each pixel

Sky cut with multi-frequency receivers array, no interference case

Deep RATAN-600 Zenith Survey, 2005at DEC=DEC 3C84

White Receivers noise component only

The Need of High resolution for classification of the CMB

polarization • Even one-dimensional resolution can help!

• In the most cases, integrated polarization is ZERO, but even ONE-DIMENTIONAL resolution can help to identify E-topology

Looking for cooperation,

• Yuri Parijskij, par@sao.ru

• See “Cosmological Gene” Russian Project

• (http://www.sao/hq/CG.ru, http://brown.nord.nw.ru)