Table 2.
Fits of the emission lines identified in the March 2024 spectrum at the position of SN 2020qxz.
| Central wavelength (Å) | σ (Å) | σ (km s−1) | significance | Element | Rest wavelength (Å) | Velocity offset (km s−1) |
|---|---|---|---|---|---|---|
| 4766.0 ± 1.1 | 12.7 ± 1.4 | 800 ± 88 ± 196inst | 62 | Hβ | 4861.00 | 5920 ± 70 |
| 8395.8 ± 0.6 | 9.3 ± 0.7 | 332 ± 25 ± 124inst | 76 | Ca II(1) | 8542.00 | 5180 ± 20 |
| 8423.6 ± 1.4 | 5.6 ± 1.5 | 199 ± 53 ± 124inst | 14 | N I | 8567.74 | 5090 ± 50 |
| 8615.8 ± 1.3 | 5.8 ± 1.5 | 202 ± 52 ± 122inst | 17 | K I(2) | 8763.96, 8767.05 | 5170 ± 50 |
Notes. The first three columns give the central wavelength and width (in Å and km s−1) of the fitted lines, we also give the instrumental velocity uncertainty at the emission line in the third column. The fourth column gives the significance of the detection. The last three columns give the most likely matched elements and emission lines, assuming some amount of blueshift velocity offset (given in the last column). The redshift uncertainty contribution to the velocity offset (120 km s−1) has not been included. All fits are done in the SN rest-frame.
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