Data are in B1950; solar interference is present in calibrators and
source; worse at beginning of run. Used uvrange 0.7,0 for phase cal;
flux cal was observed at end of run so was less affected but still
flagged some short baselines for it. 
Galaxy data: UVPLT showed: 
Lots of high points at short bl (solar interference probably),and a
secondary spike at about 0.8 kl. RR is worst; range up to 25 Jy (solar
int) and 7 Jy for secondary spike; LL range up to ~ 10Jy (solar int) and
~ 2Jy for secondary spike. I'm quite sure the shortest baseline stuff is
solar; but I'm not sure about the secondary spikes. 

>> After group discussion, Elias suggests that this stage isn't the
   right place to do a lot of editing of the source data; we can see how
   much of the solar interference UVLSF takes out of the line
   data; then use UVPLT/TVFLG to look at worst channels (as found by
   imaging the cube) to find the shortest useful baseline; set UVRANGE
   to that to exclude bad baselines. 

When it comes time (imaging recipe) for using the source
   data, Elias recommends "DBCON, UVLSF, and IMAGR and see what the
   damage is, and check on a line free channel what the shortest
   baseline is that you can still tolerate. Often UVLSF does the
   trick. You can then do the UVCOP trick, run WIPER (and if required
   CLIP), and then go on with the recipe as usual." The UVCOP trick is
   to use UVCOP to copy over everything except the contaminated short
   baselines. 

>> Using TVFLG here to flag only NON-solar, non short-bl RFI stuff. 

WIPER on galaxy:  Bad baseline: 8-10; points > 40 Jy. Spike at ~.8 kl is from
>> 4-5; another smaller spike at ~8.5 kl is from 1-5; an even smaller
>> spike at ~.6kl is from 21-22. Used SPFLG to find it - channel 133;
flagged with uvflg. 

For imaging: >> Rerun WIPER after UVLSF to see if further clipping is
needed. I'd guess 5-6 Jy would be ok.