"Some new information on RadioAstron and Millimetron missions". XXVIII GA IAU, Beijing, August "Some new information on RadioAstron and Millimetron missions". XXVIII GA IAU, Beijing, August 2012.

Baykonur, 18 July 2011, 6:31 a.m. (Moscow time). The start of the RadioAstron observatory.

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

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

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

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, , 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.

M87, jet position angle -77 deg, 5 GHz, VSOP

Cen A, jet position angle 51 deg, 5 GHz, VSOP

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.

R.C. Henry, 1999, ApJ, 516, L49.

The Space Observatory in the single-dish mode Telescope: Primary mirror diameter 12 m, surface RMS accuracy 10 m, diffraction beam 4 and field of view 4.5 at 1.5 THz. Bolometer arrays: wavelength ranges mm, and mm HPBW beam (at 1.5 THz) 4'' Low resolution spectropolarimeter: wavelength range mm spectral resolution R = 3 Medium resolution spectrometers: wavelength ranges mm, and mm spectral resolution R = 1000 High resolution spectrometer: wavelength ranges 0.05 – 0.3 mm spectral resolution R = 10 6 Bolometric sensitivity: at 1 THz, NEP = W(s) 0.5, A = 100 m 2, R=3 and 1 h integration Jy (1 )

Millimetron orbit around L 2 Т (days) B(10 3 km) λ=2 cm 1 mm 300 μm 365(L 2 ) λ/а = 2.8 fas 0.14 fas 41 nas Period of oscillation around L 2 is days. Observatory ecliptic latitude varied between b=+/- 55 deg L2L2

MM & SMM Ground-Space Interferometer MM & SMM Ground-Space InterferometerMillimetron ALMA GROUND RADIO TELESCOPES

The Space-Earth Interferometer Mode Frequency ranges: 18-26, 31-45, , , and GHz. VLBI RMS sensitivity: RMS 4 mJy (at 950 GHz, TN = 200 K) and 0.5 mJy (at 275 GHz, TN =50 K), bandwidth 1 GHz, 300 s integration and ground segment АLMA). Baseline projections: B γ = 7.8·10 4 – 2.5·10 6 km, at B γ =[-2kT max ·lnγ/(πF ν )] 0.5, 20 VLBI RMS sensitivity, F ν =(10-100) mJy, visibility γ = 0.5 and T max = K.

SOME CRITICAL EXPERIMENTS OF MILLIMETRON MISSION 1. Near horizon SMBH physics. 2.Proton-synchrotron emission, cosmic rays accelerators. 3. AGN angular size-redshift dependence and cosmological parameters, hidden matter and dark energy, AGN evolution. 4. Hidden matter objects, mirror matter. 5. AGN explosions physics, super luminal motion and expansion, proper motion of binary or nearby by AGNs. 6. Gravitational lensing and dark matter. 7. Super Massive Black Holes with Megamasers. 8. GRB physics and beaming. 9. Flat spectrum pulsars and pulsar physics. 10. Coldest objects on the border Solar system, at our and other galaxies. 11. First galaxies, just after recombination and dark age objects, primordial black holes and wormholes, Multiverse. 12. Stars and planetary systems evolution, life and SETI.