def calc_gs_snu_ujy(b, ne, delta, sinth, width, elongation, dist, ghz):
    """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.

    """
    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