Table 3.
UV emission lines detected In MUSE-Wide and MUSE-Deep TDOSE spectra via FELIS template matches.
| Line | z-range | Objects within full z-range (1.5 < z < 6.4) | |||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| All fields | MUSE-Wide | UDF mosaic | UDF10 | ||||||||||
| Any detection | 1.5000–6.4432 | 103 | 2052 | 5.02% | 24 | 1100 | 2.18% | 49 | 719 | 6.82% | 30 | 233 | 12.88% |
| N V | 2.8918–6.4432 | 7 | 1997 | 0.35% | 3 | 1094 | 0.27% | 3 | 688 | 0.44% | 1 | 215 | 0.47% |
| C IV | 2.1114–4.9699 | 45 | 1710 | 2.63% | 15 | 947 | 1.58% | 17 | 590 | 2.88% | 13 | 173 | 7.51% |
| He II | 1.9379–4.6411 | 16 | 1465 | 1.09% | 7 | 817 | 0.86% | 8 | 495 | 1.62% | 1 | 153 | 0.65% |
| O III | 1.8969–4.5632 | 18 | 1451 | 1.24% | 2 | 803 | 0.25% | 7 | 496 | 1.41% | 9 | 152 | 5.92% |
| Si III | 1.5514–3.9067 | 13 | 1000 | 1.30% | 0 | 530 | 0.00% | 8 | 347 | 2.31% | 5 | 123 | 4.07% |
| C III | 1.5241–3.8548 | 52 | 985 | 5.28% | 5 | 520 | 0.96% | 29 | 343 | 8.45% | 18 | 122 | 14.75% |
| Line | z-range | MUSE redshift desert (1.5 < z < 2.9) | |||||||||||
| All fields | MUSE-Wide | UDF mosaic | UDF10 | ||||||||||
| Any detection | 1.5000–6.4432 | 49 | 55 | 89.09% | 5 | 6 | 83.33% | 28 | 31 | 90.32% | 16 | 18 | 88.89% |
| N V | 2.8918–6.4432 | 0 | 0 | 0.0% | 0 | 0 | 0.0% | 0 | 0 | 0.0% | 0 | 0 | 0.0s% |
| C IV | 2.1114–4.9699 | 11 | 28 | 39.29% | 2 | 5 | 40.00% | 5 | 14 | 35.71% | 4 | 9 | 44.44% |
| He II | 1.9379–4.6411 | 8 | 34 | 23.53% | 2 | 5 | 40.00% | 5 | 19 | 26.32% | 1 | 10 | 10.00% |
| O III | 1.8969–4.5632 | 12 | 38 | 31.58% | 0 | 5 | 0.00% | 7 | 22 | 31.82% | 5 | 11 | 45.45% |
| Si III | 1.5514–3.9067 | 11 | 53 | 20.75% | 0 | 5 | 0.00% | 7 | 31 | 22.58% | 4 | 17 | 23.53% |
| C III | 1.5241–3.8548 | 37 | 54 | 68.52% | 1 | 5 | 20.00% | 22 | 31 | 70.97% | 14 | 18 | 77.78% |
| Line | z-range | Lyα emitters (2.9 < z < 6.4) | |||||||||||
| All fields | MUSE-Wide | UDF mosaic | UDF10 | ||||||||||
| Any detection | 2.9–6.4432 | 54 | 1997 | 2.70% | 19 | 1094 | 1.74% | 21 | 688 | 3.05% | 14 | 215 | 6.51% |
| N V | 2.9–6.4432 | 7 | 1997 | 0.35% | 3 | 1094 | 0.27% | 3 | 688 | 0.44% | 1 | 215 | 0.47% |
| C IV | 2.9–4.9699 | 34 | 1682 | 2.02% | 13 | 942 | 1.38% | 12 | 576 | 2.08% | 9 | 164 | 5.49% |
| He II | 2.9–4.6411 | 8 | 1431 | 0.56% | 5 | 812 | 0.62% | 3 | 476 | 0.63% | 0 | 143 | 0.00% |
| O III | 2.9–4.5632 | 6 | 1413 | 0.42% | 2 | 798 | 0.25% | 0 | 474 | 0.00% | 4 | 141 | 2.84% |
| Si III | 2.9–3.9067 | 2 | 947 | 0.21% | 0 | 525 | 0.00% | 1 | 316 | 0.32% | 1 | 106 | 0.94% |
| C III | 2.9–3.8548 | 15 | 931 | 1.61% | 4 | 515 | 0.78% | 7 | 312 | 2.24% | 4 | 104 | 3.85% |
Notes. The number of reliable secondary UV emission lines detected in the objects from the MUSE-Wide, the UDF mosaic and UDF10. The top part provides numbers when including all available sources studied in this work, the central part list the statistics for the object in the so-called MUSE redshift desert, and the bottom part provides the statistics for LAEs. Each subsample (all fields, MUSE-Wide, UDF mosaic and UDF10) include three numbers corresponding to the number of lines detected, the number of objects available in the effective redshift range, and the percentage of spectra with a detection this corresponds to. The MUSE-Wide includes ≈91 arcmin2 at 1 h depth, the UDF mosaic ≈9 arcmin2 at 10 h depth, and the UDF10 ≈1 arcmin2 at 31 h depth. Each 1D spectrum was searched for UV emission via template matching with the FELIS software (Appendix A) using the template sets listed in Table 2.
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