PHT03 and PHT22
For each AOT request the observer has to specify the following parameters:
FILTER: specify central wavelength of each filter requested
APERTURE (for PHT03 only): for each filter an aperture has to
be provided
POINT OR EXTENDED SOURCE: specification of source type;
this
parameter defines whether the EXPECTED SOURCE FLUX is given in Jy or
MJy
STARING OR CHOPPING MODE: definition of the observing mode
if CHOPPING MODE is selected (see Sect. 3.1 and
6.2 for details):
CHOPPER MODE: rectangular, triangular or sawtooth chopping
CHOPPER THROW: angular separation (in arcsec) between target and
reference position
CHOPPER AVOIDANCE DIRECTION: direction to be avoided by the
chopper
FULL AVOIDANCE ANGLE: angular region to be avoided by the chopper
if STARING MODE is selected:
RASTER MAP: in staring mode a raster may be performed (see
Sect. 3.3)
if RASTER MAP is selected:
M RASTER POINTS: number of raster positions along scan leg (1-32)
N RASTER LEGS: number of raster legs (1-32)
DELTA M: separation of raster points (between half the aperture or array
size and 180
)
DELTA N: separation of raster legs (between half the aperture or array
size and 180)
RMAP ORI FLAG: definition of raster orientation: orientation can be chosen
parallel to spacecraft Y axis or arbitrarily with respect to direction to
celestial North Pole. In the latter case the angle between the raster
orientation and the local North direction has to be defined.
EXPECTED SOURCE FLUX: best available estimate of source flux
(see Sect. 6.2)
UNCERTAINTY IN SOURCE FLUX: uncertainty of source flux estimate
MAXIMUM BACKGROUND FLUX: expected background flux in
MJy at source
position including all components (see Sect. 6.2)
PEAKING UP REQUEST: for small apertures and high pointing
accuracies peaking up on the source is necessary (see ISO OBSERVER'S
MANUAL)
INTEGRATION TIME or S/N: the user specifies the integration
time requested or, alternatively, the required signal-to-noise ratio
PHT05 and PHT25
In addition to the observing parameters given above, for these AOTs the observer selects a reference flux for the FCS. The possible range for this flux is between 1/10 and 10 times the sum of the source flux and the background level.