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

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

Orbital period 8.5 days. Perigee radius km, Apogee km. Inclination angle - 81 о. Maximum baseline km

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).

The main parameters of RadioAstron mission in flight Spectral band [GHz] [cm] P L C K Polarization number x bandwidth per polarization [MHz] 2 x 4 2 x 32 Smallest fringe spacing at baseline km [  as] Total flux / polarization flux sensitivity 1  [mJy] (GBT, 5 min for total and 3 hours for polarization) 33 / 7 3 / / / 1.7

Pushchino RadioAstron tracking station.

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) (KHz).

Giant pulse of Crab pulsar at 18 cm, 15 November RadioAstron Badary, IAA. Eupatoria, Ukraine.

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

Profiles of a single pulse of the pulsar PSR detected by RadioAstron and three ground radio telescopes. The insert presents the correlated signal between the space radio telescope and Arecibo for this single pulse.

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

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

The first fringes SRT - Eelsberg at 1.3 cm from the quasar (no red shift), May 12, Integration time: 65 s. Baseline projection length: 0.3 Earth diameter. The signal-to- noise ratio is shown versus residual delay and fringe rate.

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

SNR 2,0 D З 4,2 D З 5,2 D З Fringe SNR versus projected baseline , March 2012, 6.2 cm, SRT-Effelsberg

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

SOME CRITICAL EXPERIMENTS WITH RADIOASTRON: PROPOSALS FOR CORE SCIENCE PROGRAMM. 1.Near horizon SMBH physics. Structure. 2.Near horizon SMBH physics. Brightness temperature. 3.Near horizon SMBH physics. Polarization. 4.Near horizon SMBH physics. Variability and proper motion. 5.Near horizon SMBH physics. Binary systems. 6.Size, structure, brightness temperature, spectrum, polarization, Faraday RM, variability – red shift dependence and cosmology, grav. lenses, dark matter and energy, AGN evolution 6.Size, structure, brightness temperature, spectrum, polarization, Faraday RM, variability – red shift dependence and cosmology, grav. lenses, dark matter and energy, AGN evolution. 7.Multiverse, primordial black holes and wormholes. 8.Star formation, masers and Megamasers. 9.SN & GRB physics and beaming (alert mode observations). 10.Pulsar physics, interstellar plasma and interstellar interferometer. 10.Pulsar physics, interstellar plasma and interstellar interferometer. 11.Microquazars & magnetars (alert mode observations). 12.Earth gravity and special effects.