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Zeldovich-Sakharov program at RATAN-600

Zeldovich-Sakharov program at RATAN-600. “Cosmological Gene” project Ground based support of the Space CMB Missions Y.Parijskij et al Special Astrophysical Observatory Russian Academy of Science POSTER presentation, ORSAY, POLAR2005. Main Targets. Sub-mK in Tb Sub-mJy in f.d.

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Zeldovich-Sakharov program at RATAN-600

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  1. Zeldovich-Sakharov program at RATAN-600 “Cosmological Gene” project Ground based support of the Space CMB Missions Y.Parijskij et al Special Astrophysical Observatory Russian Academy of Science POSTER presentation, ORSAY, POLAR2005

  2. Main Targets • Sub-mK in Tb • Sub-mJy in f.d. • Up to confusion limit • I,U,Q information

  3. Main Targets • Sub-mK in Tb • Sub-mJy in f.d. • Up to confusion limit • I,U,Q information

  4. 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.

  5. 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)

  6. 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

  7. 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

  8. 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.

  9. 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

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

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

  12. Deep RATAN-600 Zenith Survey, 2005at DEC=DEC 3C84White Receivers noise component only

  13. The Need of High resolution for classification of the CMB polarization • Even one-dimensional resolution can help!

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

  15. Looking for cooperation, • Yuri Parijskij, par@sao.ru • See “Cosmological Gene” Russian Project • (http://www.sao/hq/CG.ru, http://brown.nord.nw.ru)

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