Table 3.
Best-fit FWHM and integrated fluxes of observed spectral lines.
| Hγ | Hβ | [OIII]λ4959 | [OIII]λ5007 | [NII]λ6548 | Hα | [NII]λ6584 | [SII]λ6716 | [SII]λ6731 | [SIII]λ9532 | HeIλ10829 | ||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| G1 | FWHM | − | − | − | − | 282 ± 85 | 333 ± 53 | 282 ± 85 | 194 ± 70 | 194 ± 70 | 352 ± 18 | 432 ± 39 |
| I | − | − | − | − | 63 ± 13 | 1035 ± 65 | 184 ± 39 | 64 ± 14 | 71 ± 19 | 286 ± 11 | 402 ± 34 | |
| C | FWHM | (500) | 679 ± 43 | 476 ± 53 | 476 ± 53 | 571 ± 101 | 679 ± 43 | 571 ± 101 | 679 ± 43 | 679 ± 43 | − | − |
| I | < 172 | 310 ± 37 | 165 ± 14 | 492 ± 42 | 144 ± 28 | 1747 ± 190 | 423 ± 82 | 290 ± 70 | 265 ± 68 | − | − | |
| S1 | FWHM | 116 ± 15 | 116 ± 15 | 119 ± 5 | 119 ± 5 | 98 ± 58 | 116 ± 15 | 98 ± 58 | (150) | (150) | − | − |
| I | 95 ± 14 | 216 ± 10 | 498 ± 9 | 1484 ± 26 | 22 ± 6 | 802 ± 29 | 64 ± 16 | < 61 | < 64 | − | − | |
| S2 | FWHM | 125 ± 14 | 125 ± 14 | 65 ± 5 | 65 ± 5 | (150) | 125 ± 14 | (150) | (150) | (150) | − | − |
| I | 75 ± 18 | 130 ± 10 | 235 ± 7 | 701 ± 20 | < 53 | 458 ± 30 | < 44 | < 55 | < 64 | − | − | |
| W1 | FWHM | 332 ± 27 | 332 ± 27 | 324 ± 14 | 324 ± 14 | (300) | 332 ± 27 | (300) | (300) | (300) | − | − |
| I | 92 ± 29 | 310 ± 40 | 452 ± 24 | 1348 ± 73 | < 205 | 1223 ± 158 | < 227 | < 236 | < 199 | − | − | |
| W2 | FWHM | 172 ± 16 | 172 ± 16 | 135 ± 8 | 135 ± 8 | (200) | 172 ± 16 | (200) | (200) | (200) | − | − |
| I | 59 ± 19 | 169 ± 26 | 555 ± 21 | 1655 ± 64 | < 136 | 891 ± 120 | < 151 | < 157 | < 133 | − | − | |
| X1 | FWHM | (150) | 270 ± 69 | 131 ± 28 | 131 ± 28 | (150) | 270 ± 69 | (150) | (150) | (150) | − | − |
| I | < 27 | 39 ± 12 | 30 ± 3 | 88 ± 9 | 54 | 324 ± 53 | < 51 | < 59 | < 55 | − | − | |
Notes. FWHM and integrated fluxes given in units of [km s−1] and [10−20 erg s−1 cm−2], respectively. Values found using simultaneous fit of a power law continuum and 1D Gaussian for each line. For undetected lines, we list the 3σ upper limit on the integrated flux based on the error spectrum and an assumed FWHM (see the value in parentheses). No correction for dust reddening or gravitational magnification has been applied. We include the best-fit line fluxes for a weaker candidate galaxy (X1; see Appendix B).
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