PLANCK()

       To calculate the Planck function in units of ergs/cm2/s/A

       bbflux = PLANCK( wave, temp)

       WAVE   Scalar or vector giving the wavelength(s) in **Angstroms**
               at which the Planck function is to be evaluated.
       TEMP   Scalar giving the temperature of the planck function in degree K

       BBFLUX - Scalar or vector giving the blackbody flux (i.e. !pi*Intensity)
               in erg/cm^2/s/A in at the specified wavelength points.

       To calculate the blackbody flux at 30,000 K every 100 Angstroms between
       2000A and 2900 A
       IDL> wave = 2000 + findgen(10)*100
       IDL> bbflux = planck(wave,30000)
       If a star with a blackbody spectrum has a radius R, and distance,d, then
       the flux at Earth in erg/cm^2/s/A will be bbflux*R^2/d^2

       The wavelength data are converted to cm, and the Planck function
       is calculated for each wavelength point. See Allen (1973), Astrophysical
       Quantities, section 44 for more information.

       See the procedure planck_radiance.pro in
       ftp://origin.ssec.wisc.edu/pub/paulv/idl/Radiance/planck_radiance.pro
       for computation of Planck radiance given wavenumber in cm-1 or
       wavelength in microns

       Adapted from the IUE RDAF               August, 1989
       Converted to IDL V5.0   W. Landsman   September 1997
       Improve precision of constants    W. Landsman  January 2002

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