Table 3
Fits of the mock data.
|
αcl |
Bol. stochastic αbol, MK,αbol,py |
Bol. Larson αbol,MK,αbol,py |
Hα stochastic αHα,MK,αHα,py |
Hα Larson αHα,MK,αHα,py |
|---|---|---|---|---|
| 2.3 | 1.90, 1.93 | 2.17, 2.18 | 1.62, 1.66 | 1.93, 1.94 |
| 2.0 | 1.82, 1.86 | 1.96, 1.98 | 1.58, 1.62 | 1.79, 1.81 |
| 1.7 | 1.75, 1.80 | 1.81, 1.86 | 1.53, 1.58 | 1.69, 1.72 |
Notes. As in previous tables, the first fit is with the Maschberger & Kroupa (2009) method and the second is with the powerlaw.py algorithm (Alstott et al. 2014). First column is the spectral index of the injected GMC or cluster mass distribution. The following columns provide the spectral indices α of the fits to the bolometric luminosity distribution and the Hα luminosity distribution for the stochastic and Larson (1982) IMFs. This is the data used as input to Fig. 10.
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