Table 6
Photometric data points of mm cores with associated Spitzer IRAC sources in at least three bands (Fig. 2) and SED fit results (Fig. 4).
| Core | Spitzer | Herschel | SED fit | |||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| IRAC | MIPS | PACS | ||||||||||||||
| F3.6 | F4.5 | F5.8 | F8.0 | F24 | F70 | F100 | F160 | T1 | L1 | T2 | L2 | T3 | L3 | L | M/L | |
| (mJy) | (mJy) | (mJy) | (mJy) | (mJy) | (Jy) | (Jy) | (Jy) | (K) | (L⊙) | (K) | (L⊙) | (K) | (L⊙) | (L⊙) | (M⊙/L⊙) | |
| ISOSS J22478+6357 4 | … | 0.3 | 0.8 | 1.2 | … | 0.2 | 0.5 | 2.1 | 375 | 0.3 | 20 | 7.0 | … | … | 7.4 | 1.5 × 10−1 |
| ISOSS J22478+6357 5 | 1.5 | 2.5 | 3.3 | 3.8 | … | 0.3 | 0.8 | 1.4 | 548 | 1.0 | 24 | 7.9 | … | … | 8.9 | 3.8 × 10−2 |
| ISOSS J22478+6357 6 | … | 2.8 | 4.6 | 6.3 | … | 0.3 | 0.6 | 1.2 | 464 | 1.5 | 21 | 7.5 | … | … | 9.0 | 1.1 × 10−1 |
| ISOSS J22478+6357 13 | 44.7 | 67.0 | 95.0 | 105.4 | 234.0 | … | … | … | 552 | 27.3 | 54 | 47.0 | … | … | 74.3 | 2.6 × 10−3 |
| ISOSS J23053+5953 1 | 0.7 | 1.6 | 1.6 | 1.1 | … | 7.6 | 22.5 | 35.9 | 620 | 0.7 | 23 | 379.3 | … | … | 380.1 | 8.7 × 10−3 |
| ISOSS J23053+5953 2 | 2.7 | 8.1 | 11.5 | 12.4 | 1190.0 | 18.2 | 44.1 | 67.0 | 479 | 5.7 | 109 | 83.0 | 28 | 706.6 | 795.3 | 3.2 × 10−3 |
| ISOSS J23053+5953 9 | 1.5 | 6.6 | 14.7 | 24.3 | 391.0 | … | … | … | 374 | 11.4 | 48 | 333.7 | … | … | 345.1 | 8.1 × 10−4 |
Notes. The photometry of the Spitzer IRAC and MIPS data is described in Sect. 3.3. The Herschel PACS fluxes are taken from Ragan et al. (2012) by cross-matching the position of the clumps and the mm cores (Table 4). Due to poor angular resolutions at FIR wavelengths, core 13 in ISOSS J22478+6357 and core 9 in ISOSS J23053+5953 cannot be assigned to a Herschel clump and therefore their SEDs are not fitted in the FIR regime.In order to fit the full SED of the cores, two or three components are required. The temperature Ti and luminosity Li of the i-th component, as well as the total bolometric luminosity L = ∑iLi, are presented. The M/L ratio is calculated from the core mass Mcore divided by the total bolometric luminosity L.
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