Table 2.
Quality of the reconstructed field and cosmic filaments as a function of S/N.
| R = 1000, LT = 4 Mpc | R = 2000, LT = 2.5 Mpc | |||||||
|---|---|---|---|---|---|---|---|---|
| S/N | σf | dskl [Mpc] | ρorig, rec(fil) | ρorig, rec(nod) | σf | dskl [Mpc] | ρorig, rec(fil) | ρorig, rec(nod) |
| 2 | −0.14,+0.12 | 3.2 | 0.07 | 0.03 | −0.19,+0.15 | 2.3 | 0.10 | 0.06 |
| 3 | −0.13,+0.12 | 2.8 | 0.14 | 0.06 | −0.17,+0.14 | 2.0 | 0.15 | 0.09 |
| 4 | −0.11,+0.10 | 2.5 | 0.18 | 0.13 | −0.15,+0.12 | 1.8 | 0.20 | 0.10 |
| 6 | −0.09,+0.08 | 2.2 | 0.24 | 0.17 | −0.13,+0.12 | 1.6 | 0.24 | 0.14 |
| 8 | −0.09,+0.08 | 2.0 | 0.27 | 0.13 | −0.12,+0.11 | 1.5 | 0.25 | 0.16 |
| 10 | −0.08,+0.08 | 2.0 | 0.28 | 0.25 | −0.12,+0.12 | 1.5 | 0.26 | 0.16 |
| 4, 25 | −0.12,+0.11 | 2.8 | 0.12 | 0.08 | – | – | – | – |
| 4, CT | – | – | – | – | −0.13,+0.12 | 1.5 | 0.22 | 0.14 |
| No noise | – | – | – | – | −0.11,+0.11 | 1.3 | 0.27 | 0.21 |
| No noise + uniform | – | – | – | – | −0.05,+0.05 | 0.6 | 0.51 | 0.40 |
Notes. The quality of the reconstruction is estimated from the standard deviation σf of δorig − δrec (see Fig. 4) and the median distance dskl between the skeleton extracted from the original (smoothed) and the reconstructed field (see Fig. 5). We also provide the Spearman correlation coefficients between the closest distances of the galaxies to filaments and nodes (ρorig, rec(fil) and ρorig, rec(nod)) as measured from the skeletons computed on the original and reconstructed fields (see Figs. B.3 and B.4). All the values are computed for two configurations: the low-resolution case with R = 1000 (and LT = 4 Mpc) and the high-resolution case with R = 2000 (and LT = 2.5 Mpc). We also show the results of the reconstruction for several additional configurations (see Sect. 2.1.4 for the details of these configurations).
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