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… to millimetron instrument WG

… to millimetron instrument WG. 12 m telescope Cooling: Y Single-dish & interferometry Wide freq range (FTS) Polarization mode Sensitivity: NEP sim 10^{-19} ToO: 1hr-time scale repointing Camera size: 10^4 simultaneous pixels. Emission line galaxies (deep-field)

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… to millimetron instrument WG

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  1. … to millimetron instrument WG • 12 m telescope • Cooling: Y • Single-dish & interferometry • Wide freq range (FTS) • Polarization mode • Sensitivity: NEP \sim 10^{-19} • ToO: 1hr-time scale repointing • Camera size: 10^4 simultaneous pixels

  2. Emission line galaxies (deep-field) • cosmology: BAO + LSS • blind search for SZE in clusters • astrophysics: SFR, metallicity, UVB • Global geometrical probesUCO + SLS • pec.V + cosmological proper motion • mod. G in extreme G environments • (close to BH event horizon) • probes of accretion flows and • B-field effect & topology & feedback • (BHs, microQSO, AGNs,QPO’s) • accretion flows and warping effects • (CO masers, AGNs, micro-QSOs) • Acceleration mechanisms around BH • and in jets (imaging and spectral • evolution, polarization) • double QSOs and X-shaped objects • interferomety,. Spectra, polariz.) • Search for WarmHoles and • observational probes (B-field, intensity • variations, interferometry, polariz.) • Dwarf stars • Rydberg atoms and B-field effects • (single-dish, spectra, polariz.) • Spectral and spatial microsctructure • of CM; B fluctuations (molecules at high-z) • (Dark Ages of the Universe) • probing SMBH (primordial BHs)at z>10 • SZE • spectro-polarimetry and imaging • clusters: cosmoogy, Dark Matter, • dark Energy, mod-G,… • RG lobes: evolution and acceleration • processes B_field effect: polarization • ToO: GRBs, SNRs, transients, .. (1hr • re-pointing)

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