Table 1.
Rest-frame UV properties of the galaxy sample.
| Target | znebular(a) | MUV | βUV | LUV | SFRUV(b) | Mstars(c) | sSFR (d) |
|---|---|---|---|---|---|---|---|
| (1011 L⊙) | (M⊙ yr−1) | (109 M⊙) | (Gyr−1) | ||||
| J1322+0423 | 2.0800 | −23.49 | −2.06 ± 0.12 | 5.64 ± 0.12 | 154 ± 7 | 3.42 ± 0.40 | 52 ± 7 |
| J0146–0220 | 2.1595 | −23.68 | −1.98 ± 0.12 | 6.76 ± 0.06 | 127 ± 6 | 3.41 ± 0.43 | 61 ± 23 |
| J1415+2036 | 2.2435 | −23.53 | −3.49 ± 0.11 ( † ) | 5.87 ± 0.12 | 188 ± 11 | 1.88 ± 0.20 | 118 ± 14 |
| J1249+1550 | 2.2928 | −23.41 | −1.84 ± 0.12 | 5.24 ± 0.11 | 118 ± 5 | 4.25 ± 0.53 | 48 ± 18 |
| J0006+2452 | 2.3796 | −24.17 | −2.30 ± 0.10 | 10.6 ± 0.2 | 232 ± 7 | 3.16 ± 0.31 | 163 ± 59 |
| J0850+1549 | 2.4235 | −23.76 | −2.62 ± 0.14 | 7.21 ± 0.17 | 189 ± 8 | 1.89 ± 0.26 | 131 ± 49 |
| J1220–0051 | 2.4269 | −23.50 | −2.43 ± 0.11 | 5.68 ± 0.12 | 144 ± 5 | 1.47 ± 0.16 | 163 ± 59 |
| J0950+0523 | 2.4548 | −23.69 | −2.41 ± 0.15 | 6.80 ± 0.18 | 179 ± 9 | 1.91 ± 0.29 | 191 ± 73 |
| J1220+0842 | 2.4698 | −24.36 | −2.36 ± 0.09 | 12.6 ± 0.2 | 302 ± 7 | 3.60 ± 0.32 | 100 ± 9 |
| J1157+0113 | 2.5450 | −23.40 | −2.15 ± 0.34 | 5.19 ± 0.16 | 104 ± 8 | 1.94 ± 0.68 | 126 ± 62 |
| J0121+0025 | 3.2445 | −24.11 | −2.19 ± 0.20 | 10.0 ± 0.1 | 269 ± 18 | 4.59 ± 0.92 | 74 ± 27 |
| J1316+2614 | 3.6122 | −24.65 | −2.59 ± 0.05 | 16.4 ± 0.2 | 415 ± 16 | 4.15 ± 1.15 | 118 ± 47 |
Notes.
Unobscured SFRs (uncorrected for dust attenuation) obtained from the UV luminosities by applying the specific LUV–SFRUV conversion factor κUV = 1.3 × 10−8 M⊙ yr−1/(erg s−1 Hz−1), derived using the BPASS models that assume the Chabrier (2003) IMF, a metallicity of 0.5 Z⊙, and a continuous star formation over 10 Myr (Sect. 2).
Stellar masses of the dominant young stellar population derived by assuming a continuous star formation over 10 Myr, that is, Mstars = SFRUV × 10 Myr, where SFRUV are corrected for the dust attenuation using the observed βUV and assuming the Calzetti et al. (2000) attenuation law (Sect. 2).
Specific star-formation rates derived using the total SFRUV+IR, with SFRIR given in Table 4.
( † )The UV spectral slope of J1415+2036 is uncertain and likely unrealistic, so far measured using the low S/N SDSS spectrum. However, if confirmed, it would indicate a rest-frame UV spectrum of the galaxy dominated by stellar radiation (without nebular emission).
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