Table 5
Comparison of the observed SEDs between 24 μm and 160 μm for the proposed FHSC candidates.
| 24 μm | 70 μm | 100 μm | 160 μm | |
| Spitzer | PACS/Spitzer | PACS | PACS/Spitzer | |
| Source | (mJy) | (mJy) | (mJy) | (Jy) |
|
|
||||
| MMS1a | 2.5 | .../200 | ... | ... |
| CB 17b | <11 | ... | 36 | .../0.8 |
| Per 58c | 0.88 | 67/65 | 407 | 1.58/2.87 |
| LDN 1451-mmd | <1.5 | <44/ <72 | <15 | 0.54/0.88 |
| Bolo 45e | ... | <71/... | <20 | 3.96/... |
| L1448-IRS2Ef | <18 | <45/ <120 | 165 | 3.32/ <2.7 |
| B1-bSg | <0.2 | 220/... | 2290 | 9.1/... |
| B1-bNg | <0.2 | <50/... | 610 | 3.24/... |
Notes. MMS1 is in Chamaeleon, CB 17 is a dark globule in the constellation of Camelopardalis, and all the other sources are in the Perseus star-forming region. PACS fluxes and upper limits are from this work with the exception of the PACS 100 μm flux of CB 17, quoted in Chen et al. (2012). Spitzer data are from the given reference with the exception of the 24 μm upper limit for B1-bS and B1-bN, derived by us. For Bolo 45, Schnee et al. (2012) report that this source was not detected in the Spitzer map, but no upper limit is given.
References.
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