Short Map Analysis Script
The resulting output catalogue has a row for every input NDF, and contains the following columns:
TAI: The MJD (in the TAI timescale) associated with the NDF
UTC: The UTC date and time string
associated with the NDF SEQSTART - RTS index number of first frame SEQEND - RTS index number of
last frame DLON: The longitude offset at the centre of the source, in arc-seconds DLAT: The latitude offset
at the centre of the source, in arc-seconds AMP: The peak value in the source SUM: The total data sum in
the source. This is the integral of the Gaussian-like model calculated by KAPPA:PSF FWHM: The
seeing-disc size: the full width at half maximum across the minor axis of the source (arc-seconds)
AXISR: The axis ratio of the source: the ratio of the major axis length to that of the minor axis. GAMMA:
The radial fall-off parameter of the source. A gamma of two would be a Gaussian. ORIENT: The
position angle (measured from north through east) of the major axis of the source, in degrees. NDF:
The path to the NDF ROW: The row number for the bolometer (if known) COL: The column
number for the bolometer (if known) ARRAY: The array name for the bolometer (if known)
For comparison, a set of extra columns is appended to these that give the source properties as
calculated by KAPPA:BEAMFIT rather than KAPPA:PSF. These columns have the same names, but are
prefixed by the letter B. Note, BEAMFIT assumes a gamma value of 2.0 (i.e. a pure Gaussian) and so
there is no BGAMMA column in the output catalogue.
The SEQSTART and SEQEND columns will be set to ‘null’ if the supplied map does not contain these FITS
headers.
If the supplied data is for the Moon, then all the above is ignored and the output contains the following columns:
SUM: The integrated value within a 35 arc-minute aperture centred on (0,0)
ROW: The
row number for the bolometer (if known) COL: The column number for the bolometer
(if known) ARRAY: The array name for the bolometer (if known) SUM column values (the total data sum) should be the integrated data value
within a circular aperture centred on the source peak position, with radius specified by
“diam” (a numerical value in arc-seconds). This is calculated using KAPPA:APERADD. If
this option is not supplied, the SUM value is the integrated value under the model source
calculated by KAPPA:PSF. If “diam” is not supplied, defaults of 30 and 15 are used for 850 and
450 μm data
respectively. ROW, COL and AMP only. Using this option also implies
the “−p”
option. This reduces the run-time for script significantly. AMP column values (the peak value in the source) should be the maximum
data value within a box of size 20 pixels centred on the expected source position. If this option is not
supplied, the AMP value is the peak value of the model source calculated by KAPPA:PSF. MORE.SMURF.SHORTMAPS or MORE.SMURF.BOLOMAPS extension item, then the NDFs in the SHORTMAPS or
BOLOMAPS array are used in place of the supplied NDF (SHORTMAPS is used in preference
to BOLOMAPS if both are present). Note, all the data must be for the same wavelength. topcat -f ascii
<out-table>.
SUM (or AMP if the
“−b”
option is used) values for each bolometer is created with the name given by
<out-image>.
The FITS headers from the first input NDF are copied to the output NDF. If the supplied data contains
values from more than one sub-array, the name of the sub-array is appended the end of each output
NDF name.