Table 1
PACS 100 μm photometry.
| Source ID | RA (J2000) | Dec (J2000) | Flux | Comments |
| (deg) | (deg) | (Jy) | ||
|
|
||||
| S CrA | 285.285750 | −36.955429 | 17.7 ± 2.6 | SMM7 (Nutter et al. 2005) |
| CrA-466 | 285.32887 | −36.97450 | 0.32 ± 0.05 | G-113 |
| #6 | 285.385710 | −36.894553 | 0.34 ± 0.08 | Chini et al. (2003), extended |
| G-85 | 285.390750 | −36.962428 | 0.42 ± 0.06 | Sicilia-Aguilar et al. (2008) |
| #8 | 285.409360 | −36.890428 | 12 ± 2 | Chini et al. (2003), extended |
| G-122 | 285.421760 | −36.953843 | 0.61 ± 0.09 | Sicilia-Aguilar et al. (2008) |
| G-65 | 285.417650 | −36.862488 | 19 ± 3 | Sicilia-Aguilar et al. (2008), mostly cloud emission |
| IRS 2 | 285.422790 | −36.975106 | 82 ± 12 | |
| IRS 2+ring | 285.422790 | −36.975106 | 104 ± 15 | Including ring-like structure |
| HBC 677 | 285.423070 | −36.997754 | 0.089 ± 0.014 | |
| IRS 5a+b | 285.450130 | −36.955705 | 19.4 ± 2.8 | Unresolved binary |
| FP-25 | 285.45193 | −36.95413 | 15 ± 3 | Probably extended, IRS 5 N |
| IRS 5ab + FP-25 | 285.450130 | −36.955705 | 71 ± 10 | Multiple system without spiral structure |
| IRS 5+spiral | 285.450130 | −36.955705 | 92 ± 13 | Multiple system plus spiral structure |
| IRS 6a+b | 285.459790 | −36.943242 | 9.2 ± 1.3 | Unresolved binary |
| V 710 | 285.46066 | −36.96934 | 97 ± 14 | SMM3 (Nutter et al. 2005), IRS 1 |
| IRS 7w | 285.47973 | −36.95577 | 476 ± 69 | Uncertain due to proximity of IRS 7e, FP-34 |
| IRS 7e | 285.48414 | −36.95843 | 162 ± 24 | Uncertain due to proximity of IRS 7w , FP-34 |
| SMM 1A | 285.48138 | −36.961325 | 148 ± 22 | Nutter et al. (2005), source #13 (Chini et al. 2003) |
| SMM 2 | 285.493130 | −36.952151 | 12 ± 2 | Nutter et al. (2005) |
| T CrA | 285.494140 | −36.963643 | 12 ± 2 | |
| B185839.6-3658 | 285.50792 | −36.899722 | 0.12 ± 0.03 | BD candidate |
| CrA-159 | 285.637520 | −36.972469 | 0.111 ± 0.016 | |
| IRAS 18598 | 285.743990 | −37.126549 | 52 ± 5 | IRAS 18598 |
| VV CrA | 285.778000 | −37.213581 | 80 ± 12 | Extended? |
| CrA-45 | 285.816690 | −37.235688 | 0.92 ± 0.13 | YSO (Peterson et al. 2011) |
| R CrA | 285.47343 | −36.952274 | 71 ± 10 | Strongly contaminated by IRS 7 |
| SMM 1A s | 285.47859 | −36.97195 | 13 ± 2 | Groppi et al. (2007) |
| #19 | 285.5521 | −36.9544 | 0.72 ± 0.11 | Chini et al. (2003), part of large cloud structure |
Notes. Photometry of the known cluster members detected by Herschel/PACS at 100 μm. For extended sources, the photometry was obtained around the peak (or peaks), but the extended material results in a large uncertainty. In the “Comments” column we include the references of the source name and/or other naming conventions, and whether the source is extended or potentially contaminated.
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