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
IMAGING THE BLACK HOLE SILHOUETTE OF M87: IMPLICATIONS FOR JET FORMATION AND BLACK HOLE SPIN, A. E. Broderick & A. Loeb, ApJ, 697, 1164, M0 represents our canonical jet model, having parameters that are broadly consistent with numerical simulations and direct observations of M87. In this case, the black hole is rapidly rotating, has a footprint of rfp=10GM/c^2 and collimation index of ξ = 1/2. Spectra and images are produced by viewing the jet at 25° from the jet/spin axis, as inferred from observations of superluminal knots (Heinz & Begelman 1997ApJ,490,653 ). M87 M0
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
10. Pulsar physics, interstellar plasma and interstellar interferometer. 10. Pulsar physics, interstellar plasma and interstellar interferometer. Interstellar scintillations and nanoarcsecond resolution in radio astronomy; Shishov, V. I.; ARep. V.54, p.724S, Interstellar interferometry of the pulsar PSR ; Wolszczan A. & Cordes, J.M.; Ap.J., 320, L35-L39, Pulsar with 4 planets, P=1.4 s, D=560 pc, Arecibo, 430 MHz.
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.
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.
Askaryan method. Luna-Glob mission planned for launch in 2016 with LORD (Lunar Orbital Radio Detector). Vladimir Ryabov Limits for CR and neutrino fluxes Results obtained for different experiments and projects associated with ultrahigh energy cosmic-ray and neutrino detection. As is seen in the energy range above – eV, the performances of the LORD are the best ! Frequency band MHz, antennas: gain 7.5 db, LP & RP polarization. h= km.
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
The single-dish mode Telescope: Primary mirror diameter 10 m, surface RMS accuracy 10 m, field of view 100 at 1.5 THz, 400 at 1 THz, 1450 at 0.5 THz. Bolometer arrays: wavelength ranges mm, and mm HPBW beam (at 1.5 THz) 5'' 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 = 60 m 2, R=3 and 1 h integration Jy (1 )
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.