A bolometer measures other contributions (e.g. the atmospheric emission), which usually domintes the measured signal. Moreover, MAMBO bolometers have a finite time response. The strategy to map a source must take care of both effects. One way is to wobble the secondary in the scanning direction. We note that it is customary to scan in the azimuthal direction because this allows to scan at nearly constant airmass (i.e. at constant elevation). However, when mapping an elongated source (e.g. an edge-on galaxy disk), the restoration algorithms work best when scanning along the smallest source size. In addition, the observing mode (wobbling) introduces strong boundary conditions, which in general implies that the whole array must scan over the full source size. In addition, a portion of blanked sky (typically 3 times the full width at half maximum of the telescope beam) must be be observed to baseline the data.
In summary, if the PI wants to map a source of size
, the total scanned size will have to be
with
| (10) | ||||
| (11) |