Table 2
Best fit results on the observables toward the 4 regions monitored in the EROS spiral arms program, compared with previous simulations (model 1) and observations published in Rahal et al. (2009b).
| Target | θ Mus | γ Nor | γ Sct | β Sct | |
|
|
|||||
| measured | 0.25 ± .037 | 0.23 ± .035 | 0.28 ± .042 | 0.34 ± .051 | |
|
±7.3% common systematics | ||||
| simple model | 0.22 | 0.26 | 0.28 | 0.32 | |
| Besançon | 0.23 | 0.26 | 0.30 | 0.33 | |
|
|
|||||
| measured | 1.95 ± .15 | 1.86 ± .15 | 2.36 ± .15 | 2.20 ± .15 | |
|
±0.16 common systematics | ||||
| simple model | 1.83 | 2.02 | 2.35 | 2.13 | |
| Besançon | 1.94 | 2.11 | 2.52 | 2.22 | |
|
|
|||||
| measured | 0.71 | 0.78 | 0.71 | 0.75 | |
| σ V − I | simple model | 0.72 | 0.73 | 0.83 | 0.74 |
| Besançon | 0.73 | 0.74 | 0.81 | 0.73 | |
|
|
|||||
| Nevent(u0<.7) | observed | 3 | 10 | 6 | 3 |
| model 1 | 2.8 | 9.9 | 7.1 | 6.3 | |
|
simple model | 4.0 | 8.6 | 3.6 | 2.2 |
| Besançon | 4.0 | 9.9 | 3.5 | 2.4 | |
|
|
|||||
| measured |
|
|
|
|
|
| τ × 106 | model 1 | 0.42 | 0.52 | 0.71 | 0.57 |
| simple model | 0.23 | 0.38 | 0.43 | 0.45 | |
| Besançon | 0.22 | 0.34 | 0.44 | 0.40 | |
|
|
|||||
| measured | 97 ± 75 | 57 ± 10 | 47 ± 6 | 59 ± 9 | |
| model 1 | 73.8 | 67.9 | 37.9 | 60.2 | |
 (day) |
simple model | 79.4 | 54.4 | 49.1 | 53.8 |
| with Kroupa IMF | 64 | 43 | 38 | 42 | |
| Besançon | 68.5 | 51.9 | 43.0 | 49.3 | |
Notes. Surface density (per square degree) of stars brighter than I = 18.4, mean and width of CMD color distribution, number of microlensing events, optical depth, and mean duration.
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