[ Basic Info | References | User Guide ]
Basic Information on smaflux
Purpose: Set the flux scale of a vis dataset given a planet obs.
SmaFlux is a MIRIAD program which corrects the flux density scale
in visibility datasets. In doing this, it assumes that the flux
density scale is out by a constant factor. SmaFlux looks for
observations of planets, and given its model of the planetary
visibility function, it computes the factor needed to correct
the flux density scale of the data set. The values of the Planck
whole disk brightness temperature from the SMA planetary model
(http://sma1.sma.hawaii.edu/planetvis.html) are adopted for
brightness temperature of a planet or a moon which is included
in the following list:
Mercury, Venus, Mars, Jupiter, Saturn, Uranus, Neptune, Pluto,
Ganymede, Callisto, Titan, Ceres, Pallas, Vesta.
To fix the flux density scale, SmaFlux creates or modifies calibration
tables attached to each dataset.
To run this program, the data directory for the SMA planetary
model needs to be installed by excuting the following script:
Input visibility datasets. Several datasets can be given (wildcards
are supported). The datasets should include observations of a planet.
Normal uv-selection parameter. This selects the data in the input
datasets to analyse. See the help on ``select'' for more information.
smaflux will use any data that has a source name which it recognises
as a planet. You may wish to select just the shortest spacing, where
the planet is strongest.
location of MIRIAD's home directory;
The default is $MIR.
Extra processing options. Several can be given, separated by commas.
vector Use the real part (rather than amplitude) of the data and
model. This option should be used if the visibility data
are phase calibrated.
noapply Do not apply the scale factor (just evaluate it).
nofqav When dealing with amplitude data, SMAFLUX normally
averaging in frequency first, to avoid noise
biases. The nofqav disables this averaging.