| Abstract
| - We present numerical simulations for a selection bias in the extragalactic Cepheid method (as detected in Teerikorpi & Paturel [CITE]), which results in underestimated distances for host galaxies. The selection effect involves the Cepheid detection magnitude limits in V and I, the dispersion in $\langle M(P) \rangle$, and importantly, variation amplitude, observable upper period limit, and also extinction. It influences both the bias curve fitting method and the method where short-period Cepheids are removed. When V, I, and P-limits exist, one expects a typical bias pattern in the $\log H$ vs. $M_{\mathrm{lim}}$ diagram. A full bias correction is possible only for special favourable situations, but there always appears a nearly unbiased plateau. The simulated bias varies from galaxy-to-galaxy roughly as was revealed by the strong and puzzling observed trend for galaxies in TP02.
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