code: def calc_gs_snu_ujy(b, ne, delta, sinth, width, elongation, dist, ghz):
      
      hz = ghz * 1e9
      eta = calc_gs_eta(b, ne, delta, sinth, hz)
      kappa = calc_gs_kappa(b, ne, delta, sinth, hz)
      snu = calc_snu(eta, kappa, width, elongation, dist)
      ujy = snu * cgs.jypercgs * 1e6
      return ujy
docs: Calculate a flux density from pure gyrosynchrotron emission.
  
      This combines Dulk (1985) equations 35 and 36, which are fitting functions
      assuming a power-law electron population, with standard radiative transfer
      through a uniform medium. Arguments are:
  
      b
        Magnetic field strength in Gauss
      ne
        The density of electrons per cubic centimeter with energies greater than 10 keV.
      delta
        The power-law index defining the energy distribution of the electron population,
        with ``n(E) ~ E^(-delta)``. The equation is valid for ``2 <~ delta <~ 7``.
      sinth
        The sine of the angle between the line of sight and the magnetic field direction.
        The equation is valid for θ > 20° or ``sinth > 0.34`` or so.
      width
        The characteristic cross-sectional width of the emitting region, in cm.
      elongation
        The the elongation of the emitting region; ``depth = width * elongation``.
      dist
        The distance to the emitting region, in cm.
      ghz
        The frequencies at which to evaluate the spectrum, **in GHz**.
  
      The return value is the flux density **in μJy**. The arguments can be
      Numpy arrays.
  
      No complaints are raised if you attempt to use the equations outside of
      their range of validity.