E.12 Concluding remarks, early science

AIPS itself, and particularly this appendix, do not begin to cover all of the issues that will arise with EVLA data. The increased sensitivity of the EVLA will mean that imaging will no longer be able to ignore effects that are difficult to correct such as pointing errors, beam squint, variable antenna polarization across the field, leakage of polarized signal into the parallel-hand visibilities, etc., etc. These are research topics which may have solutions in AIPS or other software packages such as OBIT and CASA eventually.


Figure E.2: Early EVLA science: The spectrum of the hot core of Orion A at K band. Three separate observations of 8192 channels each 0.125 MHz wide were made using 12 antennas in the D array. Two hours total telescope time went into each of the two lower thirds of the spectrum and 1 hour was used for the highest third. The plot was made using ISPEC over a 54 by 60 arc second area. Line identifications provided by Karl Menten.