| Spectrum ID | 307031075_sp3 |
|---|---|
| Alt name | g1514487-402153 |
| z | 0.0238 |
| RA, Dec | 228.7029, -40.3648 |
| MJD | 59351.54 |
| SNR/Å B/R | 7.5/20.0 |
| Obs Airmass | 1.02 |
| SMSS ID | 307031075 |
| Closest SMSS | 13.77'', 307031145 |
| SMSS Mean r6"ap | 14.9 ± 0.0 |
| 2MASS Kext | 10.8 ± 0.0 |
| Spectrum Type | Sy 1.5+ |
|---|---|
| Quality Flag | good |
| AGN reference | 6dFGS |
| MW E(B−V) | 0.094 |
| Power law αν | 0.49 ± 0.01 |
| log L5100,AGN | 42.76 ± 0.06 |
| log HβBr/[O III] | <0.07 |
| log ML5100/M☉ | — |
| log MHα/M☉ | 7.32 ± 0.03 |
| log MHβ/M☉ | — |
| log M[O III]/M☉ | — |

Spaxel scale: 1 arcsec² — Flux units: erg s⁻¹ cm⁻² Å⁻¹
Apertures: object (solid), background (dashed)
| Line | log L (erg s⁻¹) | FWHM (km s⁻¹) | σ (km s⁻¹) | EW (Å) |
|---|---|---|---|---|
| Hγ Narrow | — | — | — | — |
| Hγ Broad | — | — | — | — |
| [O III] 4364 | — | — | — | — |
| He II Narrow | — | — | — | — |
| He II Broad | — | — | — | — |
| Hβ Narrow | — | — | — | — |
| Hβ Broad | <40.60 | — | — | — |
| [O III] 5007 | 40.53 ± 0.03 | 535 ± 63 | 183 ± 25 | 28.54 ± 1.21 |
| He I Narrow | — | — | — | — |
| He I Broad | 39.88 ± 0.15 | 1360 ± 62 | 577 ± 25 | 9.49 ± 1.74 |
| [O I] 6300 | — | — | — | — |
| Hα Narrow | 39.78 ± 0.08 | 293 ± 62 | 124 ± 25 | 9.95 ± 1.06 |
| Hα Broad | 41.36 ± 0.01 | 4028 ± 89 | 1511 ± 25 | 376.24 ± 4.21 |
| [N II] 6585 | 40.08 ± 0.04 | 293 ± 62 | 124 ± 25 | 20.00 ± 1.07 |
| [S II] 6718 | 39.04 ± 0.37 | 293 ± 62 | 124 ± 25 | 1.93 ± 1.33 |
| [S II] 6732 | 39.44 ± 0.16 | 293 ± 62 | 124 ± 25 | 4.83 ± 1.22 |
All narrow line widths are tied to narrow [O III] 5007Å. [O III] 5007Å and narrow Hβ include a second narrow component not tied to other narrow lines.
| Hα Broad SNR | 3.88 |
|---|---|
| Hβ Broad SNR | 0.97 |
| Hγ Broad SNR | 0.00 |
| AGN frac | 0.24 |
| Host frac | 0.76 |
| log L5100,Host | 43.25 |
| Fe II/Hβ | — |
| Fe II/[O III] | 0.49 |
spurious_hab/hbb | 0.0/0 |
|---|---|
l5100 | 2 |
balmer | 2 |
balmer_snr | 2 |
hb_width | 2 |
balmer_width | 2 |
Hα mass estimates from Cho+2023. Remaining mass estimates from R–L relations in Wang & Woo 2024 and zero-points from Amrutha+2026.