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 if the data directory of the SMA planetary models has been installed (see Installation of SMA Planetary Models):

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.