Table 5.
Intrinsic photometry of the Emerald obtained from our new optical/near-infrared imaging with the CFHT, HST and Spitzer, and by correcting the source-integrated (sub-)millimeter flux densities presented in C15 for the contribution of Co–N and Co–S.
| Band | Flux density | Unit |
|---|---|---|
| CFHT/MEGACAM r | < 8.5 | nJy |
| CFHT/MEGACAM z | < 29.3 | nJy |
| HST/WFC3 F110W | 47.8 ± 3.8 | nJy |
| CFHT/WIRCAM J | 64.5 ± 5.3 | nJy |
| HST/WFC3 F160W | 110 ± 9 | nJy |
| CFHT/WIRCAM Ks | 345 ± 13 | nJy |
| Spitzer/IRAC 3.6 μm | 1.19 ± 0.01 | μJy |
| Spitzer/IRAC 4.5 μm | 1.86 ± 0.02 | μJy |
| WISE W3 | 9.5 ± 2.7 | μJy |
| WISE W4 | 204 ± 19 | μJy |
| Herschel/SPIRE 250 μm | 13.4 ± 0.3 | mJy |
| Herschel/SPIRE 350 μm | 11.6 ± 0.2 | mJy |
| Herschel/SPIRE 500 μm | 7.3 ± 0.2 | mJy |
| JCMT/SCUBA-2 850 μm | 1.4 ± 0.4 | mJy |
| IRAM/GISMO 2 mm | 123 ± 39 | μJy |
Notes. We demagnified the optical and near-infrared stellar continuum fluxes by the gravitational magnification factor μstars = 34.1 ± 6.8 and the dust continuum fluxes by μdust = 29.4 ± 5.9, both derived from our best-fitting lensing model. Since the stellar and dust components likely have similar contibutions to the observed WISE emission, we used the average value of μ to correct the fluxes in the W3 and W4 bands (as done in Timmons et al. 2016). We also give the 3σ upper limits of non-detection in MEGACAM r- and z-bands.
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