If the PI wants to reach the same rms noise (
) on
sources
(they must share the same calibrator sources), during a given elapsed
telescope time (
), we have
The calibration time can be written as
The time spent per source (
) is linked to the integration time
(
) through the succession of
subscans, each subscan
having an on-source integration time of
and an overhead time of
. The
subscans are grouped into scans, with
an additional overhead time of
per scan. If one scan can
contain at most
subscans, the number of scans (
) and
the residual number of subcans (
) are computed through
| (5) | ||||
| (6) |
| (7) | ||||
| (8) |