|basic usage questions:
which circumstances do I have to use the /galactic option ?
can I check whether the deglitching flagged some real
sources or not ?
can I efficiently mask residual glitches, hot pixels or
in the final map that may have escaped detection ?
||What is the meaning of the
different planes of the output ?
||The processing aborts during
the destriping step, but only for a
subset of my observations.
What could be the cause ?
||What is the best way to
process very small maps in which the source fills the
with nominal coverage ?
||How should the relative gain
corrections be applied to SPIRE data ?
||How are the average SPIRE
beams affected by the projection method ?
||Why are there some streaks
with slightly lower coverage in some weight maps ?
||What are the PACS
distortion flatfields ?
|advanced usage questions:
field of view contains a lot of extended emission that I
want to recover as well as possible,
and the observation is long. How can the slicing into several sub-fields be avoided ?
would like to obtain the best possible time resolution
to compute the average brightness
drift, but the minimum timescale set by the code for the average drift is much longer
than that set for the individual drifts, because the observation is long.
I am also not interested in recovering large-scale gradients in the map, and the field
does not contain any bright extended emission. What can I do ?
several observations of the same field taken at
different epochs best be combined ?
have observations of adjacent fields that overlap by an
area much smaller than the area
of each field. Yet, I would like to take advantage of the increased redundancy in this
small overlap area to improve the processing. How can I manage this ?
||Is it possible to combine
data taken at different scan speeds or sampling rates ?