All Tables

Table 1: The number of light curves surviving the cuts C1 to C12 as described in the text.
Table 2: Events found in the analysis of the full sample of EROS-2 stars (Tisserand 2004). Only event EROS2-SMC-1 is in the Bright-Star Sample and passes the cuts C1-C12 and therefore is used for limits on the optical depth. All fits assume zero blending and no intrinsic variability. The two values of the fitted parameters t₀, $t_{\rm E}$ and u₀ are for $B_{\rm eros}$ (first line) and $R_{\rm eros}$ (second line). (There are no $R_{\rm eros}$ points during the event for EROS2-LMC-12.) The time of maximum, t₀ is given as JD-2450000.
Table 3: The 17 microlensing candidates of the MACHO collaboration (Alcock et al. 2000b). Candidates 20, 22 and 27 (marked B) are low signal-to-noise candidates not satisfying the MACHO "A'' requirements. Candidate 9 is due to a binary lens and does not satisfy their A requirements. The values of $t_{\rm E}$ and maximum amplification $A_{\rm max}$ are from the MACHO fit assuming no blending, and t₀ is given as JD-2 450 000. Candidates 18 and 25 are each within $1~{\rm arcsec}$ of an object of similar magnitude that is resolved by the MACHO analysis but blended in the EROS analysis. Candidates 14 and 20 occurred during EROS-2 observations, and the EROS-2 values of $t_{\rm E}$ and $A_{\rm max}$ are shown in parentheses (averages of $R_{\rm eros}$ and $B_{\rm eros}$ measurements).
Table 4: The 11 events of the EROS collaboration used in the past to set upper limits on the microlensing optical depth toward the LMC and to measure the depth toward the SMC. Candidates marked "B-S'' in Col. 2 occur on stars in the EROS-2 Bright-Star Sample. All candidates except EROS2-SMC-1 have been eliminated as variable stars or as supernovae.