Table 1
Calculated histogram difference, Hd, between the observed isolated massive sources by Mauerhan et al. (2010a) and different models.
| Hd | |||||||
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|
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| WR-L = 20 M⊙ | StdDev | WR-L = 40 M⊙ | StdDev | WR-L = 60 M⊙ | StdDev | ||
|
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| Qage = 4 Myr | 17.4 | σ4,20 = 4.38 | 4.48 | σ4,40 = 1.43 | 6.38 | σ4,60 = 1.03 | |
| Qage = 4.5 Myr | 26.55 | σ4.5,20 = 6.93 | 5.96 | σ4.5,40 = 1.15 | 5.63 | σ4.5,60 = 0.88 | |
| Qage = 5.0 Myr | 11.69 | σ5,20 = 1.79 | 3.784 | σ5,40 = 0.75 | 7.25 | σ5,60 = 0.81 | |
Notes. Compared models assume an age of 4, 4.5, and 5 Myr for the Quintuplet cluster and 2.5 Myr for the Arches. The initial mass for the massive stars is considered to be 20, 40, and 60 M⊙ in these models. The model, which assumes an age of 5 Myr for the Quintuplet cluster and an initial mass of 40 M⊙ for WR progenitors, is found to have the lowest Hd and is the most similar model to the observed distribution. The standard deviations for the Hd values are derived by individual comparison of the ten random realizations of each model.
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