Table 2.
Properties of the sources detected in the MUSE datacube and compatible with z ≃ 5.3.
| ID | RA | Dec | λLyα | F(Lyα) | S/N | zLyα–z[C II] (c) | M* | MCO | Mdyn([C II]) | Mdust | SFR (d) | AV(d) | IAU name |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (Å) | (10−18 erg s−1 cm−2) | (km s−1) | (109 M⊙) | (109 M⊙) | (109 M⊙) | (108 M⊙) | (M⊙ yr−1) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) |
| Main | |||||||||||||
| mosaic_1513 (a) | 150.0864 | 2.5891 | 7663.2 | 16.92 ± 0.37 | 46 | 380 ± 5 | 20, 0.95 | 57 ± 5, – | 97 ± 16, – | 2.66 ± 0.76, – | 1100 (e), 18 | 0.8, 0.0 | LAE J100020.74+023520.8 |
| mosaic_1496 (b) | 150.0897 | 2.5865 | 7662.7 | 5.63 ± 0.26 | 22 | 540 ± 10 | 14.8 ± 2.0 (f) | 19.0 ± 5.0 | < 0.9 | < 54 (e) | 0.2 (f) | LAE J100021.53+023511.4 | |
| mosaic_1548 (g) | 150.0909 | 2.5770 | 7666.5 | 5.42 ± 0.34 | 16 | 12.2 ± 2.2 | 15 | 0.0 | LAE J100021.82+023437.2 | ||||
| mosaic_1520 (h) | 150.0874 | 2.5938 | 7657.9 | 1.89 ± 0.17 | 11 | 2.8 ± 3.8 | 130 | 0.7 | LAE J100020.98+023537.7 | ||||
| mosaic_770 | 150.1012 | 2.5915 | 7634.5 | 2.60 ± 0.24 | 11 | LAE J100024.29+023529.4 | |||||||
| mosaic_1035 | 150.0823 | 2.5959 | 7640.7 | 2.53 ± 0.23 | 11 | LAE J100019.75+023545.2 | |||||||
| P3_547 | 150.0895 | 2.5842 | 7643.9 | 1.60 ± 0.14 | 11 | LAE J100021.48+023503.1 | |||||||
| Supplemental | |||||||||||||
| P2_446 | 150.0852 | 2.5877 | 7643.7 | 1.68 ± 0.19 | 9 | LAE J100020.45+023515.7 | |||||||
| mosaic_414 | 150.0924 | 2.5752 | 7667.8 | 0.96 ± 0.10 | 10 | LAE J100022.18+023430.7 | |||||||
| mosaic_199 (i) | 150.0860 | 2.5881 | 7662.7 | 5.14 ± 1.15 | 5 | 0.5 ± 0.4 | 23 | 0.2 | LAE J100020.64+023517.2 | ||||
Notes. Lyα and physical properties of the galaxies detected in the MUSE datacube. In the first part of the table, we list the sources in the ‘Main’ sample, in the second part the “Supplemental” sample. The columns correspond to (1) ID of the sources, (2) their RA and (3) declination, (4) wavelength of the detected emission line which is interpreted as Lyα, (5) isophotal integrated flux of the detected Lyα emission line, (6) signal-to-noise ratio of the detected emission line, (7) velocity difference between the redshift implied by the detected Lyα central wavelength and the systemic redshift inferred by the [C II] emission line, (8) stellar, (9) molecular-gas, (10) dynamical, and (11) dust mass, (12) star-formation rate, (13) dust extinction in magnitude, (14) name of the sources according to the IAU standard. The mass estimates are reported only for the sources with CO and/or [C II] detections (Capak et al. 2011; Riechers et al. 2010, 2014), and for the sources with a counterpart in the COSMOS2015 catalog (Laigle et al. 2016). Star-formation rate and dust extinction are reported for the sources with a counterpart in the COSMOS2015 catalog.
System composed by AzTEC-3 and LBG-3. LBG-3 is named 1447526 in Capak et al. (2011), COLDz.COS.0 in Riechers et al. (2020), and COSMOS2015_849732 in the COSMOS2015 catalog. The physical parameters corresponding to AzTEC-3 (first number) and LBG-3 (second number) are taken from Riechers et al. (2014, 2020).
LBG-1 as defined in Riechers et al. (2014), 1447524 in Capak et al. (2011), HZ6 in Capak et al. (2015), and COSMOS2015_848185 in the COSMOS2015 catalog. The parameter values are taken from Riechers et al. (2014), Pavesi et al. (2019), Faisst et al. (2020) (see also Barisic et al. 2017, for HST and ALMA measurements).
SFR and AV from the best fit SED fitting that provides the photometric redshift in the COSMOS2015 catalog, except for AzTEC-3 and LBG-1.
Capak et al. (2011) reported M* = 3.2 × 109 M⊙ and AV = 0.5.
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