Table 2.
Representation of photometric galaxies within the true KV450 data and spectroscopic compilation, for variously defined spectroscopic samples, determined using our “full-sample” SOM and variable cell clustering per tomographic bin (see Appendix B).
| Spectroscopic | Training | fpix |  |
|||||
|---|---|---|---|---|---|---|---|---|
| compilation | size (all) | (all, %) | All | Bin1 | Bin2 | Bin3 | Bin4 | Bin5 |
| zB ∈ (0.1, 1.2] | (0.1, 0.3] | (0.3, 0.5] | (0.5, 0.7] | (0.7, 0.9] | (0.9, 1.2] | |||
| Full sample | 25373 | 91.9 | 99.5 | 82.7 | 83.9 | 84.6 | 82.7 | 94.0 |
| CDFS only | 2044 | 17.4 | 67.3 | 57.1 | 58.7 | 53.2 | 40.2 | 54.6 |
| zCOSMOS only | 9930 | 48.5 | 79.7 | 74.9 | 75.3 | 65.8 | 60.3 | 63.2 |
| DEEP2 only | 6919 | 43.7 | 73.8 | 17.8 | 5.5 | 35.2 | 68.8 | 89.5 |
| G15DEEP only | 1792 | 10.1 | 42.0 | 63.1 | 63.6 | 44.1 | 19.8 | 14.0 |
| VVDS only | 4688 | 34.7 | 81.4 | 54.9 | 72.8 | 70.7 | 57.3 | 70.2 |
| Without CDFS | 23329 | 89.1 | 98.9 | 81.5 | 82.6 | 82.2 | 81.0 | 93.0 |
| Without zCOSMOS | 15443 | 77.6 | 97.8 | 76.4 | 80.0 | 80.8 | 78.9 | 92.6 |
| Without DEEP2 | 18454 | 73.4 | 93.4 | 81.6 | 83.0 | 80.4 | 72.2 | 80.8 |
| Without G15DEEP | 23581 | 90.6 | 99.5 | 80.1 | 83.6 | 84.3 | 82.7 | 94.0 |
| Without VVDS | 20685 | 84.7 | 98.1 | 81.3 | 79.5 | 77.5 | 80.1 | 92.9 |
Notes. The table shows the overall sample size of each spectroscopic sample (“training size”), the fraction of SOM cells containing photometric sources which also contain spectroscopy (fpix), and the change in the effective number density of sources for cosmic shear studies, neff, that we get when only using photometric sources which are represented within each particular spectroscopic sample (
). The statistics are shown for the overall source samples (“All”), and for each of the individually defined tomographic bins (we note that the All cases are not averages or summations of the binned values; see Sect. 5.1). The best performing individual spectroscopic dataset (i.e. the middle section) is shown in bold (for each column), as is the worst performing joint spectroscopic compilation (i.e. the lower section). The table demonstrates the complementarity of our spectroscopic compilation: our three main spectroscopic samples (zCOSMOS, VVDS, and DEEP2) each uniquely dominate the description of the photometric data in the different tomographic bins (1 + 2, 3, and 4 + 5 respectively).
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