Table A.1
MM3-SED.
| Wavelength | Flux | Ref. |
|---|---|---|
| [μm] | [erg cm−2 s−1] | |
| 1.63 | 1.16 ± 0.07 × 10−12 | 1 |
| 2.13 | 1.67 ± 0.02 × 10−11 | 1 |
| 3.55 | 3.64 ± 0.02 × 10−10 | 2 |
| 4.49 | 6.10 ± 0.03 × 10−10 | 2 |
| 5.73 | 9.73 ± 0.05 × 10−10 | 2 |
| 7.0 | 6.90 ± 0.49 × 10−10 | 3 |
| 7.87 | 5.30 ± 0.04 × 10−10 | 2 |
| 11.6 | 3.54 ± 0.07 × 10−10 | 4 |
| 15.0 | 6.46 ± 0.20 × 10−10 | 3 |
| 22.1 | 5.13 ± 0.13 × 10−10 | 4 |
| 23.7 | 4.49 ± 0.13 × 10−10 | 5 |
| 889 | 1.34 ± 0.04 × 10−13 | 6 |
| 1282 | 2.43 ± 0.10 × 10−14 | 6 |
| 1420 | 1.50 ± 0.19 × 10−14 | 6 |
| 1532 | 1.06 ± 0.08 × 10−14 | 6 |
Notes. The fluxes at λ ≥ 889 μm, are MM3-fluxes, whereas the fluxes at λ ≤ 24 μm are total fluxes. The contribution of all the other sources, which are less evolved than MM3 at NIR wavelengths, can be neglected (as indicated in Fig. 5). For the fit of MM3 (see Sect. 5.2.1), we use the total fluxes at short wavelengths. Only in the FIR and (sub)mm regimes, where the contribution of the other sources is not negligible, we use the MM3-fluxes.Facilities and instruments are given behind corresponding references.
References. (1) Minniti et al. (2017) (VISTA/VIRCAM); (2) Ramírez et al. (2008) (Spitzer/IRAC); (3) Omont et al. (2003) (ISO/ISOCAM); (4) Cutri et al. (2014) (ALLWISE); (5) Gutermuth & Heyer (2015) (Spitzer/MIPS); (6) Brogan et al. (2019) (ALMA, SMA).
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