Table 11.
Number 
of contaminant stars for which 
, which supposes photometry with no background correction, as a function of the number NT of telescopes observing the host star and the aperture model.
| NT | Binary mask | Gradient mask | Gaussian mask |
|---|---|---|---|
| (I + II)=(V + VI) | (I + III) | (V + VII) | |
| 24 | 40 135 | 48 005 | 55 520 |
| 18 | 36 835 | 43 690 | 50 785 |
| 12 | 32 830 | 38 485 | 44 565 |
| 6 | 26 545 | 31 050 | 35 995 |
| weighted | 31 591 | 37 178 (+17.7%) | 43 073 (+36.3%) |
Notes.
The presented values were determined from our dataset of ∼3.25 million contaminant stars. The 
was computed with δback, k ∼ 0.1 mag, td = 4 h, η = 7.1, and ntr = 3. The roman numerals correspond to the areas indicated in Fig. 19. The percentiles indicate the amount of deviation of the values from weighted masks with respect to those from binary mask. The weighted values in the lower row correspond to the effective 
, obtained by assuming uniform star distribution and a fractional field of view as given in Table 1.
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