Table 1.
Awarded time (in h) for KMOS observations.
| Field | P99 | P100 | P101 | P102 | Total |
|---|---|---|---|---|---|
| COSMOS | 7.6 | 10.8 | 0 | 10.8 | 29.2 |
| (2H + 1.5YJ( ⋆ )) | (3H + 2K) | (5H) | (10H + 2K) | ||
| ECDFS | 0 | 0 | 2.2 | 0 | 2.2 |
| (1H) | (1H) | ||||
| SXDF | 0 | 8.7 | 5.4 | 10.8 | 24.9 |
| (2H + 2K) | (1H + 1K) | (3H( ⋆ ⋆) + 1K) | (6H + 4K) | ||
| VVDS | 6.5 | 10.8 | 6.5 | 8.7 | 32.5 |
| (2H + 1K) | (3H + 2K) | (2H + 1K) | (2H + 2K) | (9H + 6K) | |
| Total | 14.1 | 30.3 | 14.1 | 30.3 | 88.8 |
Notes. The table lists: number of hours, in parenthesis, the number of the observed pointings is indicated, together with the selected filter, for example, 3H + 2K means that three pointings have been observed in the H-band and two pointings have been observed in the K-band. ( ⋆ )We had initially planned to target sources with 1.8 < zphot < 2.0, for which the OII doublet is in the YJ-grating. The detection of OII is challenging in high-redshift galaxies, and our first observations in P99 had a low success rate. We therefore decided to start in P100 to exclusively concentrate on the detection of Hα in the H- and K-gratings. ( ⋆ ⋆)The observation of the last three H-band pointings in the SXDF field (see Table 2 for details) was carried over P103.
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