Simulation Strategy Session Afternoon 20 March

Image Library: Send candidate images by 27 March to Min.

Selection to occur by 3 April.

Images should be large 1024 x 1024, with good dynamic range and spatial frequency range. They will need to support imaging at 5-6 pixels per resolution element over 200 resolution elements at least.

Create uv sample visibilities

No errors to be added to data at this point; that evaluation to occur later.

Exception: Use median tau (???number???) for weights.

For speed, use FFT then interpolate.

Output to UVFITS

The antenna will be assumed to employ a 12db taper.

Use 5 degree mask.

Imaging and deconvolution at 345 Ghz frequency

Pick 5 resolutions (Yun, ALMA Project Book Chapter 15)

'A' 0.05"

'C' 0.22"

'E' 0.98"

Compact array: simulate snapshots only; long integrations less important (?)

Intermediate configuration(s): Scale image to ~200 beams

Snapshots and synthesis +/- 2 hrs of meridian for '1.5' km array.

Snapshots and synthesis +/- 2 hrs of meridian for '3' km array, intially.

Declination range: -23, -70 and +25 degrees

Arrays should accommodate e.g. a 1.1 NS stretch.

Multi-configurations may be simulated.

Final deconvolved image

Use Maximum Entropy and CLEAN, and whatever else your Pandora's box

contains.

Adrian will arrange with Steven Heddle (?) To have a 'black box' to run these

Imaging simulations all these ways in a parallel fashion.

After an initial run in AIPS simulations, with the limited errors discussed above, simulations will be run in AIPS++ with the more robust error treatment which Mark has designed. This should occur by August 2000.

Judgment Day:

rms difference maps

max, min in maps

Max fractional difference

FT difference image to find where artifacts arise

Compute MODEL/Difference maps for 'image fidelity'.