Table 5.
Comparison of the reference model (SFH delayed: t/τ2 exp(−t/τ) with τ = 500 Myr) to all the others using the BIC.
| DL2014 vs. PL+OT_MBB | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| τmain[Myr] | k | Agemain[Myr] | τburst[Myr] | Ageburst[Myr] | δ | Mean | SD | Min | Max |
| 500 Myr | 2 ≤ k ≤ 5 | 101 values in [2, 1200] | −0.95 | 1.58 | −7.28 | 4.08 | |||
| DL2014 | |||||||||
| τmain[Myr] | k | Agemain[Myr] | τburst[Myr] | Ageburst[Myr] | δ | Mean | |||
| 20 000 Myr | 2 ≤ k ≤ 5 | 101 values in [2, 1200] | −3.35 | 11.21 | −68.37 | 1.39 | |||
| 10 values in [100, 1000] | 3 ≤ k ≤ 6 | 101 values in [2, 1200] | −0.75 | 5.83 | −3.15 | 41.64 | |||
| 500 | 3 ≤ k ≤ 6 | 101 values in [100, 1200] | 20 000 | 2, 5, 10, 20, 50 | −1.62 | 5.87 | −9.23 | 16.89 | |
| 500 | 3 ≤ k ≤ 6 | 101 values in [2, 1200] | 7 values in [−0.70, 0.70] | 1.49 | 7.12 | −3.59 | 43.43 | ||
| PL+OT_MBB | |||||||||
| 20 000 Myr | 2 ≤ k ≤ 5 | 101 values in [2, 1200] | −3.49 | 11.40 | −68.37 | 1.55 | |||
| 10 values in [100, 1000] | 3 ≤ k ≤ 6 | 101 values in [2, 1200] | −0.67 | 6.00 | −3.15 | 41.64 | |||
| 500 | 3 ≤ k ≤ 6 | 101 values in [100, 1200] | 20 000 | 2, 5, 10, 20, 50 | −1.05 | 6.57 | −9.23 | 19.16 | |
| 500 | 3 ≤ k ≤ 6 | 101 values in [2, 1200] | 7 values in [−0.70, 0.70] | 1.51 | 7.20 | −3.04 | 42.94 | ||
Notes. This comparison was performed by fitting all the objects in our sample. We note that the IR composite SED is not used in this analysis, but only individual ALMA measurements (detections and upper limits). We first assumed a DL2014 model for the IR template. The, we assumed a PL+OT_MBB for the IR template. The BIC values do not change much for the two options for the IR template. The range in the number of parameters k is also indicated for each series of run. To the parameters listed in the table, we need to add the amount of dust attenuation, i.e., E_BVs_young. The sample has at least five photometric points in the rest-frame UV and optical as well as one photometric point in the rest-frame far-IR, so n ≥ 7. More precisely, the complete sample of individual galaxies have 7 ≤ n ≤ 24 with ⟨n⟩ = 13.3 ± 4.3 and 11/119 objects have more than ten photometric points.
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