Single-dish data are analysed using CLASS by Gaussian fits with the
method CONTINUUM Beam_size which takes into account the dual-beam
pattern in elevation. Beam width, beam separation and beam ratios are fixed
for better sensitivity. One planets, these parameters are freed using the
GAUSS * * * command, since the planets are marginally resolved. The
beam-size is 56 
at 86 GHz.
A typical sequence of single-dish flux reduction is the following:
FIL IN 'date'.BUR FIL OUT 'flux-date'.BUR ! @ PR:INIT_FLUX Teles Line ! Initialize once R Scan ... R Scan ! Repeat for all scans in the file ! @ PR:INIT_FLUX Teles Line ! Repeat for other frequencies/Telescopes ... R Scan
The setup procedure PR:INIT_FLUX contains
! @ PR:INIT_FLUX Telescope Line ! Initialize a flux data reduction LAS\SET TEL &1 ! Select Telescope LAS\SET LINE &2 ! Select Observed Line LAS\SET TYPE CONTINUUM LAS\SET ALIGN POSITION LAS\SET ANGLE SECOND DEVICE ! Enter graphics device SIC\DEFINE REAL F SAY "Enter LO1 frequency in GHz (0 if not known or variable)" LET F IF (F.GT.80.AND.F.LT.118) THEN Say "The beam-size is:" '86*56|F' ANALYSE\METHOD CONTINUUM 86*56|F ! Fix the beam width ELSE ANALYSE\METHOD CONTINUUM ! Let it free if frequency not known ENDIF SYMBOL R "SIC\@ PR:FLUX"
R is a symbol calling the reduction procedure PR:FLUX.CLASS
! ! CLASS : Reduce a Pointing cross scan to get flux measurements ! ! Calling sequence : @ PR:INIT_FLUX ! Then R Scan_Number (R = "@ PR:FLUX") ! DEFINE INTEGER ISCAN DEFINE LOGICAL PLANET LET ISCAN &1 LAS\FIND/SCAN ISCAN LET PLANET (SOURCE.EQ."JUPITER".OR.SOURCE.EQ."VENUS".OR.SOURCE.EQ."MARS".OR.- SOURCE.EQ."SATURN") ! LAS\GET FIRST LAS\GET NEXT LAS\ACCUMULATE SET MOD X -110 110 LAS\PLOT SIC\IF PLANET THEN ANALYSE\GAUSS * * * ELSE ANALYSE\GAUSS ENDIF ANALYSE\FIT PAUSE "WRITE the result if it seems OK" LAS\GET NEXT LAS\GET NEXT LAS\ACCUMULATE SET MOD X -110 230 LAS\PLOT SIC\IF PLANET THEN ANALYSE\GAUSS * * * ELSE ANALYSE\GAUSS ENDIF ANALYSE\FIT PAUSE "WRITE the result if it seems OK" SET MOD X -110 110
When all the reduction is finished, print the fit results from the output file
FIL IN 'flux-date'.BUR FIND PRINT FLUX/OUT 'bur*-frequency-date'.FIT
The Gaussian fit results are written in a special file (produced by the new command CLASS PRINT FLUX /OUTPUT Filename) which contains all the fit parameters, the antenna number, the signal and image frequencies, the gain USB/LSB and the elevation of the source.
This file is then directly analysed using ASTRO with the new language FLUX which corresponds to the commands described in section 4.