flux, weight
Set the estimated flux expected from a baseline of zero length.
EXAMPLE
-------

0>uvzero 10, 100
Zero-baseline flux set to 10 Jy. Weight=100.
0>

The second line is the response from the 'uvzero' command, confirming
the user's selection. To see the value of the current zero-spacing
flux omit all arguments:

0>uvzero
Zero-baseline flux set to 10 Jy. Weight=100.
0>

To cancel a previously set zero-baseline flux spefiy zero.

0>uvzero 0,0
Zero-baseline flux not set.
0>

PARAMETER
---------
flux   -  The estimated total flux of the observation (Jy). This will
          be treated as though it were the flux density of a normal
          visibility at U=0 and V=0.
weight -  The visibility weight to be assigned to the zero-baseline
          flux. This is the weight to be seen after application of
          wtscale and has the same form as the weights of normal
          visibilities. However note that the addition of a zero-baseline
          visibility is like the addition of a single extra sample in
          the UV plane and will have very little effect unless a large
          weight is used.

Whenever a new UV data set is read with the 'observe' command, the
default value of flux=0.0 is set.

CONTEXT
-------
If an observation is so defficient in short baselines that no value is
added to the pixel at the origin of the U,V plane grid, then the total
flux in the dirty map will equal zero (as required by Fourier
transform theory). For very extended sources this may result in low
brightness regions of the source appearing to be negative because the
flux in every pixel of the map is offset by a small negative
amount. The effect may be countered to some extent by adding a fake
visibility at the origin of the UV plane. Unfortunately, while the
total estimated flux of the source can be used to set the amplitude of
the visibility and the phase at the origin is known to be zero, the
weight to give the visibility is a matter of experimentation. A weight
value that is much higher than the average weight of the observed
visibilities will be needed if any effect is to be seen. The best
value will depend on the distribution of the observed visibilities and
their weights.

In practice it is probably easier to get rid of negative bowls
by model fitting rather than experimenting with the zero-spacing
flux.

SIDE EFFECTS
------------
Use of this command will cause the next 'clean', 'mapplot' etc..
to re-invert the modified UV data-set to produce an updated dirty
beam and residual map.