Table 2.
Properties of the two stacks performed.
| # Quasar | Mean | S/N | EW MgII | EW MgII | MgII | Col Den 2796 | Col Den 2803 | Frequency | |
|---|---|---|---|---|---|---|---|---|---|
| Sample | Spectra | MgII | MgII | 2796 | 2803 | Doublet | log N(MgII) | log N(MgII) | Weighted 2796 |
| Redshift | sample | Å | Å | Ratio | cm−2 | cm−2 | log N(MgII) cm−2 | ||
| MgII selected | 32/16224 = 0.2% | 0.51 | 73 | 0.35 ± 0.015 | 0.19 ± 0.015 | 1.8 | ≥12.92 | 12.95 ± 0.1 | ≥10.22 |
| Blind | 16224 = 100% | 0.45 | 195 | 0.056 ± 0.015 | 0.024 ± 0.015 | 2.3 | 12.12 ± 0.1 | 12.05 ± 0.1 | 12.12 ± 0.1 |
Notes. Table 2 lists the number of background quasar spectra stacked. The column of the number of quasar spectra corresponds to the fraction of quasars over the entire number of spectra with its representative percentage. The column density for the MgII-selected sample is frequency-weighted, considering the number of spectra used. Possible saturation (at EW2796 > 0.15 Å) leads to a lower limit on the column density of the MgII-selected sample. MgII absorption is tentatively detected in the blind stack. This tentative detection provides a measure of the column density, which relates to the amount of cold gas in galaxy clusters.
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