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Fig. 6.


Source-plane reconstruction of the gas, dust and stellar emission from the Emerald, using the best-fitting lens model of the massive foreground cluster. Top row: (a) PdBI map summed over the frequency channels of the CO(4–3) line. The black lines show contours at −2σ (dashed lines), +2 and +5σ (solid lines). The beam of the PdBI at the redshifted frequency of CO(4–3) is plotted in the lower-left corner. (b) Best-fit source model ray-traced to the image plane and convolved with the PdBI beam (see details in the text). Orange and blue solid lines show the critical and caustic curves at z = 2.236, respectively, obtained from the best-fitting lens model. The box indicates the size and position of the enlarged region in the rightmost panel. (c) CO(4–3) residual and contours at −2, +2 and +5σ. (d) Best-fit model of the CO source, truncated at its FWHM (yellow ellipse). The bar in the lower-right corner illustrates the physical scales at z = 2.236. Center row: (e) SMA 850 μm image in the extended configuration and −2, +2 and +5σ contours (black lines). The SMA beam is shown in the lower-left corner. (f) Best-fit model convolved with the SMA beam in the image plane. (g) 850 μm residual and contours at −2, +2 and +5σ. (h) Best-fit azimuthally-averaged model of the 850 μm source, truncated at its FWHM (red circle). Bottom row: (i,j,k) Same as before, for the HST F110W imaging, within the field-of-view indicated in panel (e). (l) Best-fit model of the rest-frame optical stellar continuum in the source plane (blue ellipse), compared with those of CO(4–3) and 850 μm continuum. We also show the direct ray-tracing of the WFC3 F110W emission to the source plane (dark blue contours drawn at +2, +3 and +4σ), and the highly elongated PSF of the WFC3 image in the source plane (dark blue ellipse in the lower-left corner).

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