Calibration for The Flux Density Scale

After calibrations for the fringe amplitude (with $\rm T_{sys}$), bandpass, antenna gains, and baseline-based errors, one might proceed to bootstraping the flux density scale from an observed planet to the visibility data using smaflux which relys on the SMA Planetary Models. The catalog directory of the SMA Planetary Models in Miriad contains two sets of data for each planet (1) a file of the Planck whole disk brightness temperature from SMA Planetary Models and (2) the planet ephemeris from JPL's HORIZONS System. Based on the disk brightness temperature and the ephemeris data, smaflux calculates the visibility structure using a uniform disk approach. In comparison the observed visibility with the model, smaflux determines the flux-density scale. The beta version of SMA Miriad contains the SMA Planetary Models. For the old version (Miriad CVS), one need to install the SMA Planetary Models separately (see Installation of SMA Planetary Models). The usage of smaflux is given here,

smaflux% inp
  Task:   smaflux
  vis      = uvdata_rx0.usb.tsys.bp.bl.av %the uvdata set calibrated
                                          %for Tsys, bandpass, antenna
                                          %gains, baseline-based errors
  select   = source(ceres)                %select the planet observed 
                                          %for flux density scale 
                                          %calibration.
  mirhome  = $MIR                         %the home directory of one's
                                          %Miriad installation which
                                          %leads the program to find
                                          %the data directory of the
                                          %SMA planetary models.

smaflux reports the scaling factor of the flux density for the uvdata set and creates/modifies the gain table.