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Each row shows a grey-scale image of the Spitzer 3.6 #8201; #956;m observations, superimposed with grey contours indicating the 1.4 #8201;GHz observations and black contours showing the 4.8 #8201;GHz (left panel) and 8.6 #8201;GHz (middle panel) observations. The IFRS are always the sources at the image centres. Contours start at 3 #963; and increase by factors of 2. The 1.4 #8201;GHz restoring beam and the 4.8 #8201;GHz/8.6 #8201;GHz restoring beams, which are the same size, are indicated with ellipses in the lower left corners of the images. The right panel shows the flux density measurements available for a source and 3 #963; upper limits where no detection was made (indicated with arrows). The solid line indicates the best available spectral index, and dashed lines indicate a power-law with an index 1 #963; larger and 1 #963; smaller than determined by the data. We note that all sources have a signal-to-noise ratio of more than 9 in the 1.4 #8201;GHz observations, so there is no doubt that they are real sources and not spurious.
|Open with DEXTER|
|In the text|
|Bins||Stellar mass or redshift intervals used to divide galaxies into sub-populations for stacking analysis.||S2.1|
|Layer||A subset of a real/mock sky image (or map) attributed to only the sources in the corresponding stellar mass or redshift bin.||S2.1, S2.2|
|Scatter||In this paper, we exclusively define "scatter" as the standard deviation of flux density or luminosity in the source population, which is characterized and represented by σS in Equation (4).||S2, Appendix A, Equation (4)|
|(Un)perturbed||Fluxes being assigned to the sources in a specific layer are drawn from a distribution with the mean equal to the best-fit value given by SIMSTACK and some (zero) nonzero width defined by the scatter.||S2.2, Appendix A, Equation (4)|
|Real/Mock||"Real" refers to the actual sky image, whereas "mock" refers to the image reconstructed using source locations and perturbed mean fluxes from SIMSTACK. More specifically, in our analysis we construct the mock sky image by merging (1) a layer of interest perturbed according to a distribution with a tunable scatter and (2) background layers perturbed by a distribution with a fiducial scatter of 0.3 dex.||S2.2, Equations (5), (6)|
|Base||The "base" map, different from the mock image, is obtained by merging (1) an unperturbed layer of interest and (2) background layers perturbed by a distribution with a fiducial scatter of 0.3 dex.||S2.2, Equations (5), (6)|
|Residual||The difference between the real or noise-added mock sky image and a "base" one.||S2.2, Equations (5), (6)|
|,||A small cutout image a few pixels by side, where each pixel measures the standard deviation of a data cube obtained by thumbnail-stacking the residual map at the positions of the sources in each i, j layer.||S2.2, Equations (5), (6)|
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