Table 1.
Overview of the full galaxy sample used in this paper, grouped by C III] and [C II] detection.
| ID | zsp | C III] | [C II] | Ref. |
|---|---|---|---|---|
| HZ10 | 5.657 | ✓ | ✓ | [†, 1] |
| COS-3018 | 6.854 | ✓ | ✓ | [2, 11] |
| A383-5.2 | 6.029 | ✓ | ✓ | [3, 12] |
| z7_GND_42912 | 7.506 | ✓ | ✗ | [7, 13] |
| HZ1 | 5.689 | ✗ | ✓ | [†, 1] |
| RXJ 1347-1216 | 6.766 | ✗ | ✓ | [†, 14] |
| GDS3073 | 5.563 | ✗ | ✓ | [†, 15] |
| UVISTA-Z-002 | 6.634 (a) | ✗ | ✓ | [†, †] |
| Himiko | 6.595 | ✗ | ✓ | [4, 8] |
| CR7 | 6.604 | ✗ | ✓ | [9, 10] |
| CR7a | 6.604 | ✗ | ✓ | [9, 10] |
| CR7b | 6.604 | ✗ | ✓ | [9, 10] |
| CR7c | 6.604 | ✗ | ✓ | [9, 10] |
| COS-13679 | 7.145 | ✗ | ✓ | [2, 16] |
| COS-2987 | 6.816 | ✗ | ✓ | [2, 11] |
| VR7 | 6.532 | ✗ | ✓ | [5, 17] |
| 9347 | 1.851 (b) | ✗ | ✓ | [†, 6] |
| 6515 | 1.844 (b) | ✗ | ✓ | [†, 6] |
| 10076 | 1.946 (b) | ✗ | ✓ | [†, 6] |
| 9834 | 1.764 (b) | ✗ | ✓ | [†, 6] |
| 9681 | 1.885 (c) | ✗ | ✓ | [†, 6] |
| 8490 | 1.906 (c) | ✗ | ✓ | [†, 6] |
Notes. Spectroscopic redshift is based on the Lyα emission or spectroscopic Lyman break except when otherwise noted.
Spectroscopic redshift measured from a Gaussian fit to the integrated spectrum of the [C II] line from this work.
Spectroscopic redshift from the optical spectra. Typical redshift uncertainties are ΔzLyα ∼ 0.0005 − 0.004, Δz[C II] ∼ 0.0002 − 0.0006, and Δzopt ∼ 0.001. The mark ✓ indicates that the emission line has been detected. The mark ✗ indicates that the emission line has not been detected and an upper limit has been placed on the line flux.
References. C III] and [C II] line references: [†] This work, [1] Capak et al. (2015), [2] Laporte et al. (2017), [3] Stark et al. (2015), [4] Carniani et al. (2018b), [5] Matthee et al. (2017b), [6] Zanella et al. (2018), [7] Hutchison et al. (2019), [8] Zabl et al. (2015), [9] Sobral et al. (2018) [10] Matthee et al. (2017a), [11] Smit et al. (2018), [12] Knudsen et al. (2016), [13] Schaerer et al. (2015), [14] Bradač et al. (2017), [15] Béthermin et al. (2020), [16] Pentericci et al. (2016), [17] Matthee et al. (2019).
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