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Presentation transcript:

AIPS

WSRT & VLA Y-shape array A - 21 km B - 10 km C - 3.6 km D - 0.6 km 27 telescopes Ø25m east - west array ~ 2.8 km 14 telescopes Ø25m

GMRT & MERLIN random centre & Y-shape array 30 km 30 telescopes Ø45m Lovel Ø76m

VLBA & EVN & VLBI 10 telescopes Ø25m

UV-coverage

dirty & clean Image

UV coverage & Image 12 hours WSRT observations

Clean Image I

Clean Image II

Why Calibration and Editing? Synthesis radio telescopes, though well-designed, are not perfect (e.g., surface accuracy, receiver noise, polarization purity, stability, etc.) Need to accommodate engineering (e.g., frequency conversion, digital electronics, etc.) Hardware or control software occasionally fails or behaves unpredictably Scheduling/observation errors sometimes occur (e.g., wrong source positions) Atmospheric conditions not ideal (not limited to “bad” weather) RFI radio frequency interference

That's why! BAD GOOD

visibilities = amplitude[t] * e(i[t]) VLA observations amplitude versus time good diagnostic for bad data amplitude versus UV distance

www-astro.physics.ox.ac.uk/~hrk/AIPS_TUTORIAL/HRK_AIPS_1.html