… to millimetron instrument wg
DESCRIPTION
… 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) - PowerPoint PPT PresentationTRANSCRIPT
… 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) cosmology: BAO + LSS blind search for SZE in clusters astrophysics: SFR, metallicity, UVB
• Global geometrical probes UCO + 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)