Table 2
Median IGM transmission and dispersion around the median as observed from the VUDS spectra fitting.
| VUDS galaxies | QSOs | ||||||||
|
|
|||||||||
| Median IGM transmission Tr(Lyα) | Dispersion | IGM transmission | IGM dispersion | ||||||
| Redshift | Median z | Dust E(B−V) ≤ 0.15 | Dust E(B−V) ≤ 0.05 | ±68% | (Becker et al. 2013) | Faucher-Giguère et al. (2008b) | |||
| BC03 | with M05 | BC03 | M05 | BC03 | M05 | ||||
|
|
|||||||||
| 2.5 <z< 3.0 | 2.75 | 0.79 |
0.78 |
– | – |
|
|
0.80 | 0.12 |
| 3.0 <z< 3.5 | 3.22 | 0.69 |
0.67 |
– | – |
|
|
0.70 | 0.13 |
| 3.5 <z< 4.0 | 3.70 | 0.59 |
0.59 |
– | – |
|
|
0.59 | 0.13 |
| 4.0 <z< 4.5 | 4.23 | 0.55 |
0.56 |
0.49 |
0.50 |
|
|
0.47 | 0.12 |
| z> 4.5 | 4.77 | 0.46 |
0.45 |
0.42 |
0.42 |
|
|
0.35 | 0.13 |
Notes. The dispersion is computed as 68% of the distribution. The transmission values are indicated for the GOSSIP+ fits performed using the BC03 and M05 composite stellar population models. Comparing these results shows that IGM transmission and dispersion values do not depend on the stellar population used in the fit. At z > 4 we indicate two different measurements, one is obtained when the dust extinction in galaxies is let free to vary up to E(B−V) = 0.15, while the other is for dust constrained to E(B−V) ≤ 0.05 (see Sect. 6.2) . Results from the VUDS galaxies LOS are compared to the mean IGM transmission from Becker et al. (2013) and to the IGM dispersion measured by Faucher-Giguère et al. (2008b).
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