\zeta\, {\rm PSF_{\rm peak}}\, \Omega\, A\, T\, \Delta \lambda,$$ where $\zeta$ is the uniform contrast level of suppressed starlight measured relative to the PSF peak per unit solid angle, ${\rm PSF_{\rm peak}} = \pi D^2/4 \lambda^2$ expresses the theoretical Airy pattern peak per unit solid angle under the assumption of a diffraction-limited PSF, and $\Omega = \pi(X\lambda/D)^2$ is the solid angle subtended by the photometric aperture. Expanding all dependencies on $\lambda$ and $D$, Equation \[CRbstar\_equation\] can be expressed as $$\label{CRbstar_equation_expanded}
    {\rm CR_{b,\star}} = F_0\, 10^{-0.4{\rm m}_V}\, \zeta\, \frac{\pi^2 X^2}{4}\, \frac{\pi D^2}{4}\, T\, \Delta \lambda,$$ such that the leaked starlight’s count rate is proportional to the collecting area of the telescope.

The local zodiacal light is expressed as $$\label{CRbzodi_equation}
    {\rm CR_{b,zodi}} = F_0\, 10^{-0.4z}\, \Omega\, A\, T\, \Delta \lambda,$$ where $z$ is the typical surface brightness of the zodiacal light in magnitudes per unit solid angle at $V$ band. Expanding all dependencies on $\lambda$ and $D$, we find $$\label{CRbzodi_equation_expanded}
    {\rm CR_{b,zodi}} = F_0\, 10^{-0.4z}\, \frac{\pi^2 X^2}{4}\, \lambda_V^2\, T\, \Delta \lambda,$$ such that the local zodiacal light’s count rate is independent of telescope diameter.

Finally, the exozodiacal light is given by $$\label{CRbexozodi_equation}
    {\rm CR_{b,exozodi}} = F_0\, n\, 10^{-0.4x}\, \Omega\, A\, T\, \Delta 