1. Moscow 2006 Astro Space Center P.N. Lebedev Physical Institute

2. DCR-1000 - cross 1000х1000 m, width 40 m, range 30-120 MHz.

3. BSA – array of 16384 dipoles,187х384 m, 16 separate beams, range 110±1 MHz.

4. RT-64, Kalyazin RT-22, Pushchino

5. Solar wind turbulence spectrum. Observations of radio signals scintillations of distant spacecrafts. In acceleration region was found flicker noise spectrum, in more distant quite region – cascade Kolmogorov spectrum (Chashey I.V. at collaboration).

6. Interstellar plasma turbulence spectrum by observation scintillation of pulsars radio emission in scales of few 10 3 km to 10 13 km. Spectrum is very near to Kolmogorov with index 11/3 (Chashey I.V. at al.).

7. Radio emission of two short period X-ray pulsars was found in the centers of supernova remnants. PSR J0205+6449 PSR J0205+6449 in the 3С58, very young neutron or quark star, age about 850 years. BSA observations at 111 MHz a) accumulation of five periods interval by observations of 1145 pulses. b) accumulated one period (65.68 ms) by observations of 5725 pulses. Radio flux 40 mJy, magnetic field 7*10 12 G, distance 6.4 kps. Malofeyev V.M., Malov O.I., Malov I.F., Teplykh D.A., Glushak A.P.

8. Super giant pulse of Crab nebula pulsar: flux 7·10 6 Jy at 2.2 GHz, T B = 10 40 K. E and H of the electromagnetic wave larger the pulsar magnetic field H~10 12 G. RT-64, Kalyazin (Popov M.V., Soglasnov V.A. et al.). 0246 мкс 0 2 4 6 8 МЯн 8 Радио Оптик а Рентген Period of neutron star rotation is 33 ms.

9. Flare of maser OH (1665 MHz) emission in the star formation region W75N, distance 2 kps (Slysh V.I. et al., 2005). VLBA Калязин Нансэ VLBA

10. More 25 years of H 2 O space masers monitoring at 22 GHz in PRAO. It’s the most long set observations. 125 sources are in the modern list for observation once in the month. Here two type sources: super compact (~1au) gaze clouds in star formation regions and envelopes of variable late spectra classes stars. In star formation regions was found periodicity of masers variations (few years periods). This sources have usually three spectral components and probably correspondent to proto planet disks formed around proto star. It was found that variability of masers in stars envelopes strong correlate with IR and optic variation of the star at definite delay. It’s confirm a shock model, which propagates from the star across envelope. Here demonstrated a maser and optics observations in 2000-2004 of variable star в 2000-2004 гг и оптического блеска переменной звезды V391 Cyg. Delay is 100-150 days. (RT-22, LPI and SAI collaboration, Samodurov V.A. et al.).

12. A.G. Doroshkevich, P.D. Naselsky, O.V. Verhodanov, D.I. Novikov, V.I. Turchaninov, I.D. Novikov, P.R. Christensen, L.-Y. Chiang, Inter. J. Modern Physics D (2005) New method of Universe parameters determination by SMB analysis. Project GLESP (Gauss-LEgendre Sky ) for. As expected this method will be used for determination of the dark matter and dark energy, neutrino mass, Hubble constant, spectrum of density perturbation, spectrum of primordial gravity waves, parameters of secondary ionization and others with accuracy 1%. Project GLESP (Gauss-LEgendre Sky Pixelization) for PLANCK mission (2007). As expected this method will be used for determination of the dark matter and dark energy, neutrino mass, Hubble constant, spectrum of density perturbation, spectrum of primordial gravity waves, parameters of secondary ionization and others with accuracy 1%.

13. Inflation stage Universe parameters determination. V.N.Lukash, E.V.Mikheeva, V.Muller, A.M.Malinovsky, MNRAS (2000) V.N.Lukash, E.V.Mikheeva, Inter. J. of Modern Physics A (2000) Е.В.Михеева, В.Н.Лукаш, Астроном. Журнал (2004); В.Н.Лукаш, УФН (2006) New model (Lambda-inflation) permit by observation data on density galactic clusters and CMB anisotropy to find limitations on model parameters and amplitudes of primordial gravitational waves (vertical axis) and spectral index density perturbations (horizontal axis).

14. LogN-logS distribution of gamma- bursts (most deep set) The circles – previous date. Crosses – a new distribution of 3906 all found bursts in BATSE archive data by new method.. B. Stern, Ya. Tikhomirova, D. Kompaneets, R. Svensson, J. Poutanen, ApJ (2001)

15. ARENA-2005 Kalyazin Radio Observatory. RT-64 beamwidths are ~11' at 1.4 GHz and ~7' at 2.3 GHz. The expected events should be near the limb of the Moon, so the pointing was at 14' apart from the center of the Moon (Dagkesamanskiy R.D. et al.). Position of the antenna beams on the Moon

16. LUNAR ORBITAL RADIO DETECTOR expected launch 2009 LPI, Lavochkin Association, MSU, IAS, JINR, ISP (Sweden) V.Tsarev, e-mail tsarev@sgi.lebedev.ru Detection of Ultrahigh-Energy Cosmic Rays and neutrinos by Radio Method

18. Arecibo Observatory Library Colloquium April 11, 2005 Radio Galaxy M87 (red shift 0.0044) Blazar Variability Workshop II Jansky Symposium, NRAO April 18, 2005June 10, 2005 Kovalev et al. (2005) The internal jet is strong vary with time but most compact unresolved detail is seeing always. It’s super massive black hole of 3 billion solar mass, diameter smaller 10 light days, flux 0.2 Jy. (VLBA at 15 GHz observations for RadioAstron mission).

19. Compactness (ratio of unresolved component flux to total flux) histogram: the most variable sources are more compact. 250 objects of VLBA observations at 15 GHz for RadioAstron mission program. (Kovalev Yu.Yu. et al., AJ, 130, 2473-2505 2005)

20. North hemisphere sources for RadioAstron program. Red points – sources with normal specters, green points the sources with inverted specters. (Larionov M.G. et al. 2005). (Ларионов М.Г. и др., 2005 г ).

21. “S PECTR -R” (Mission “ RadioAstron ”) Main scientific tasks of the mission – syntheses of high-precision images of various Universe objects, its coordinates measurements and search their variability with the time. A fringe width of the system is up to 7 micro arc seconds. Main characteristics of the space radio telescope Spectral band: wavelength (cm) - 92; 18; 6.2; 1.19-1.63 frequency (GHz) - 0.327; 1.66; 4.83; 18-26 Main organizations: on scientific complex - Astro Space Center of Lebedev Physical Institute of Russian Academy of Science; of spacecraft - Lavochkin Research Production Association of Russian Space Agency. Planned launch date of the mission is 2007. The orbit of the mission : apogee - 310 000 - 370 000 km perigee - 10 000 - 70 000 km declination - 51.6 ° period variation - 7 - 10 days Guarantied time of activity - 5 years Scientific payload mass - 2100 kg Pointing accuracy of radio telescope - 35" RADIO INTERFEROMETER MUCH LARGER THE EARTH

24. OBJECTS OF EXPLORATION BY RADIOASTRON MISSION 1. GALAKTIC NUKLEI (SYNCHROTRON EMISSION, COSMIC RAYS, MEGAMASERS, BLACK HOLES, WORMHOLES, NEW PHYSICS). 2. COSMOLOGY, DARK MATTER AND DARK ENERGY, TIME-SPACE METRIC BY OBSERVATIONS OBJECTS AND GRAVITATION LENSES AT DIFFERENT REDSHIFTS. 3. STAR AND PLANETARY SYSTEM FORMATION REGIONS (MASERS). 4.STELLAR MASS BLACK HOLES AND NEUTRON (QUARC?) STARS. 5. INTERSTELLAR AND INTERPLANETARY PLASMA. 6. HIGH ACCURACY COORDINATE SYSTEM AND FUNDAMENTAL ASTROMETRY. 7. HIGH ACCURACY BALLISTIC AND PRECISION EARTH GRAVITY FIELD.

27. Megamaser in the galaxy NGC4258 (6.4 million pc)

35. РТ-70 миллиметрового диапазона на плато Суффа.

41. Миллиметровый РТ-70.

43. MILLIMETRON. 12 m cryogenic mirror. λ = 0,01-20 mm. Bolometric sensitivity 5*10 -9 Jy (σ) (λ=0.3 mm, 1 hour int.). Space-ALMA VLBI sensitivity 10 -4 Jy (σ) (λ=0.5 mm, 300 s int.), fringe size up to nanoarcseconds.

44. Ground-space Interferometer Millimetron ALMA Suffa (Uzbekistan)

45. Space-based Interferometry