Table B.1.
Average SLEDs for star-forming galaxies and AGN hosts at z ∼ 1.25.
| X-ray |
No X-ray |
|||||
|---|---|---|---|---|---|---|
| Transition | Ndet, Nup | Mean | Median | Ndet, Nup | Mean | Median |
 |
10, 4 |
 |
 |
21, 4 |
 |
 |
 |
1, 0 | − | − | 4, 0 |
 |
 |
 |
15, 1 |
 |
 |
26, 1 |
 |
 |
 |
6, 0 |
 |
 |
6, 0 |
 |
 |
 |
2, 0 |
 |
− | 8, 1 |
 |
 |
 |
6, 0 |
 |
 |
6, 0 |
 |
 |
| fAGN > 20% |
fAGN ≤ 20% |
|||||
| Transition | Ndet, Nup | Mean | Median | Ndet, Nup | Mean | Median |
 |
8, 4 |
 |
 |
23, 4 |
 |
 |
 |
2, 0 |
 |
− | 3, 0 |
 |
 |
 |
13, 0 |
 |
 |
28, 2 |
 |
 |
 |
4, 0 |
 |
 |
8, 0 |
 |
 |
 |
3, 0 |
 |
 |
7, 1 |
 |
 |
 |
4, 0 |
 |
 |
8, 0 |
 |
 |
Notes. The L′ luminosities are expressed in 1010 K km s−1 pc2. The average I fluxes in Jy km s−1 shown in Fig. 5 are computed adopting z = 1.25. The uncertainty on the median value is the interquartile range. ( † )Formally biased mean value as the first upper limit was turned into a detection for the calculation of the KM estimator (Kaplan & Meier 1958).
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