2000ApJS..131..391A

We present the results of a comprehensive set of simulations designed to quantify the selection function of the Bright SHARC survey for distant clusters. The statistical significance of the simulations relied on the creation of many thousands of artificial clusters with redshifts and luminosities in the range 0.25<z<0.95 and 0.5<L_X<10x10⁴⁴ ergs.s^–1 (0.5-2.0 keV). We created one standard and 19 varied distribution functions, each of which assumed a different set of cluster, cosmological and operational parameters. The parameters we varied included the values of Ω₀, Ω_Λ, β, core radius (r_c), and ellipticity (e). We also investigated how nonstandard surface brightness profiles (i.e., the Navarro, Frenk, & White, or NFW, model); cooling flows; and the ROSAT pointing target, influence the selection function in the Bright SHARC survey. For our standard set we adopted the parameters used during the derivation of the Bright SHARC Cluster X-Ray Luminosity Function (CXLF), i.e., Ω₀=1, Ω_Λ=0 and an isothermal β model with β=0.67, r_c=250 kpc, and e=0.15. We found that certain parameters have a dramatic effect on our ability to detect clusters, e.g., the presence of a NFW profile or a strong cooling flow profile, or the value of r_c and β. Other parameters had very little effect, e.g., the type of ROSAT target and the cluster ellipticity. At distant redshift (z>0.8), elliptical clusters are significantly easier to detect than spherical ones in the Bright SHARC survey. We show also that all the tested parameters have only a small influence on the computed luminosity of the clusters (``recovered luminosity'' in the text) except the presence of a strong cooling flow. We conclude that the CXLF presented by Nichol et al. in 1999 is robust (under the assumption of standard parameters), but stress the importance of cluster follow-up, by Chandra and XMM, in order to better constrain the morphology of the distant clusters found in the Bright SHARC and other surveys.