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RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August 2012.

RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August 2012. 18.07.2012. Orbital period 8 . 5 days . Perigee radius 67 000 km , Apogee - 282 000 km. Inclination angle - 81 о. Maximum baseline 282 000 km.

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RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August 2012.

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  1. RadioAstron space VLBI mission: early results.XXVIII GA IAU, Beijing, August 2012.

  2. 18.07.2012. Orbital period 8.5 days. Perigee radius 67 000 km, Apogee - 282 000 km. Inclination angle - 81о. Maximum baseline 282 000 km

  3. The sketch view of the RadioAstron Observatory. The solar panels are exposed in the Y-direction, i.e. perpendicular to the sketch plane. Component H is the-high precision Hydrogen frequency standard (H-maser).

  4. The main parameters of RadioAstron missionin flight

  5. Pushchino RadioAstron tracking station.

  6. Radioastron auto spectrum in Left Circular Polarization (LCP) –on left, and in Right Circular Polarization (RCP) –on right; Day = 330, Date = 30/10/2011, UTC = 08:35, τ = 120 sec, Resolution = 500 Hz, Fsky = Freq (KHz) + 1665300 (KHz).

  7. Giant pulse of Crab pulsarat 18 cm, 15 November 2011. RadioAstron Badary, IAA. Eupatoria, Ukraine.

  8. THE FIRST FRINGES Baseline projection RadioAstron - Effelsberg: 50 Mλ or 0.6 Earth diameters, Integration 30 s. Correlating flux 1.2 Jy. VLBA, 2 см.

  9. Profiles of a single pulse of the pulsar PSR0950+08 detected by RadioAstron and threeground radio telescopes.The insert presents thecorrelated signal between the space radio telescope and Arecibo for this singlepulse.

  10. Pulsar PSR0950+08, 92 cm, January 25, 2012, the baseline projection SRT – Arecibo is 220 000 km. Significant variations of the signal in one hour is due to interstellar plasma scintillations. io

  11. Interference signal from the water maser in the star forming region W51 detected by RadioAstron-Eelsberg on May 12, 2012, at a projectedbaseline 1.14 Earth diameters. Integration time: 240 seconds. Correlated signal (color, signal-to-noise ratio) is shown versus spectralfrequency and fringe rate.

  12. The first fringesSRT- Eelsberg at 1.3 cm from the quasar 2013+370 (no red shift), May 12, 2012. Integration time: 65 s. Baseline projectionlength: 0.3 Earth diameter. The signal-to-noise ratio is shown versus residual delay and fringerate.

  13. OJ 287; 06.04.2012; 6.2 cm; RadioAstron-Effelsberg, 7.26 D; 65 sec integration. BL Lac; 26.06.2012; 6.2 cm; RadioAstron-Effelsberg, 7.25 D; 65 sec integration.

  14. Fringe SNR versus projected baseline 0716+714, 14-15 March 2012, 6.2 cm, SRT-Effelsberg 2,0 DЗ 4,2 DЗ 5,2 DЗ SNR

  15. Imaging of quasar 0716+714 (z=0,3);March,14, 2012; SRT – Effelsberg, WSRT, Jodrell Bank, Yebes, Medicina, Svetloe, Zelenchuk, Badary; baseline projection <1, 1,5-4,5 and5,5Earth diameters; chanal 6,2cm. VLBA, 2 см,24.05.2012. 2,0 DЗ 4,2 DЗ 5,2 DЗ SNR

  16. SOME CRITICAL EXPERIMENTS WITH RADIOASTRON: • PROPOSALS FOR CORE SCIENCE PROGRAMM. • Near horizon SMBH physics. Structure. • Near horizon SMBH physics. Brightness temperature. • Near horizon SMBH physics. Polarization. • Near horizon SMBH physics. Variability and proper motion. • Near horizon SMBH physics. Binary systems. • Size, structure, brightness temperature, spectrum, polarization, Faraday RM, variability – red shift dependence and cosmology, grav. lenses, dark matter and energy, AGN evolution. • Multiverse, primordial black holes and wormholes. • Star formation, masers and Megamasers. • SN & GRB physics and beaming (alert mode observations). • Pulsar physics, interstellar plasma and interstellar interferometer. • Microquazars & magnetars (alert mode observations). • Earth gravity and special effects.

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