1 / 22

Quantum steps in Radio Astronomy:

Quantum steps in Radio Astronomy:. LOFAR, SKA & ALMA. Renaissance of Low-Frequency Radioastronomy:. LOFAR. LOFAR: 13000 dipoles clustered in  100 stations  simple frontend hardware, but complex digital correlation ...  400 km across frequency coverage 10 MHz - 200 MHz

anniej
Download Presentation

Quantum steps in Radio Astronomy:

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Quantum steps in Radio Astronomy: LOFAR, SKA & ALMA

  2. Renaissance of Low-Frequency Radioastronomy: LOFAR

  3. LOFAR: • 13000 dipoles clustered in  100 stations  simple frontend hardware, but complex digital correlation ... •  400 km across • frequency coverage 10 MHz - 200 MHz • collecting area  1 km2 • b = 2” - 40” • correlation via optical fibers

  4. Science: - re-ionization 5 < z < 20  ‘step’ at 70 ···240 MHz expected - high-z universe - bursting and transient universe, GRBs - 327 MHz deuterium line - solar-terrestrial relationships

  5. SKA

  6. SKA: • 1 km2 collecting area (different concepts) • frequency coverage: 150 MHz - 20 (43) GHz • max. Baseline  1000 km • b  0.1” @ 1.4 GHz • f.o.v.  1 0 @ 1.4 GHz

  7. Science: - epoch of 1st HI signatures at z > 10? - 1st energy sources QSOs? - LSS: deep surveys Ly forest in HI line high-z CO - deep continuum fields: sub-Jy sky - DM with lensing - AGN - circum-nuclear megamasers - starbursts: brightest M82 sources detectable at z  0.4 - ISM / B-fields - GRBs

  8. ALMA

  9. ALMA: • location: Atacama desert at Chajnantor; 5000 m altitude • operation: 1st few antennas 2006, full array 2009 (?) • 64 dishes with Ø = 12 m  Atot = 7000 m2 (Plateau de Bure: 6  15-m dishes, 1000 m2) • surface accuracy (25 m) permits observations up to  1 THz or down to  280 m! • frequency coverage 70 - 900 GHz • b  10 mas (e.g.  = 1 mm, Dmax = 14 km)

  10. - CMB anisotropy - SZ - SF galaxies out to z = 20 (negative K-correction helps); first galaxies after the ‘dark age’ - DM1: gravitational lenses; map arcs in molecular lines - DM2: rotation curves in CO and CII at high z - QSO mol. absorption lines (> 30 lines already detected against systems out to z = 0.9) - AGN: in ‘depth’ (low synchrotron and dust opacity) - normal galaxies: to be studied out to z = 1 - 2 molecular transition ladder ensures to see lines at all redshifts - Magellanic Clouds: studies of molecules down to 50 AU (!) scale - harvest planets out to kpc distances

More Related