| Spectrum ID | 90657290_sp1 |
|---|---|
| Alt name | g1037498-240952 |
| z | 0.0345 |
| RA, Dec | 159.4575, -24.1645 |
| MJD | 60783.42 |
| SNR/Å B/R | 10.7/27.7 |
| Obs Airmass | 1.03 |
| SMSS ID | 90657290 |
| Closest SMSS | 14.26'', 2148589766 |
| SMSS Mean r6"ap | 16.1 ± 0.0 |
| 2MASS Kext | 11.9 ± 0.1 |
| Spectrum Type | Sy 1.5+ |
|---|---|
| Quality Flag | good |
| AGN reference | 6dFGS |
| MW E(B−V) | 0.058 |
| Power law αν | 0.05 ± 0.13 |
| log L5100,AGN | 42.51 ± 0.03 |
| log HβBr/[O III] | <-0.07 |
| log ML5100/M☉ | — |
| log MHα/M☉ | 6.17 ± 0.10 |
| 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 | 39.76 ± 0.25 | 2246 ± 62 | 954 ± 25 | 7.60 ± 2.53 |
| Hβ Narrow | — | — | — | — |
| Hβ Broad | <40.15 | — | — | — |
| [O III] 5007 | 40.22 ± 0.06 | 260 ± 63 | 361 ± 60 | 25.20 ± 2.12 |
| He I Narrow | — | — | — | — |
| He I Broad | — | — | — | — |
| [O I] 6300 | — | — | — | — |
| Hα Narrow | 39.56 ± 0.07 | 243 ± 62 | 102 ± 25 | 9.45 ± 0.70 |
| Hα Broad | 40.23 ± 0.05 | 2362 ± 186 | 917 ± 31 | 43.99 ± 2.35 |
| [N II] 6585 | 39.85 ± 0.03 | 243 ± 62 | 102 ± 25 | 18.78 ± 0.72 |
| [S II] 6718 | 39.46 ± 0.07 | 243 ± 62 | 102 ± 25 | 7.82 ± 0.79 |
| [S II] 6732 | 39.26 ± 0.11 | 243 ± 62 | 102 ± 25 | 5.05 ± 0.71 |
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 | 1.02 |
|---|---|
| Hβ Broad SNR | 0.61 |
| Hγ Broad SNR | 0.00 |
| AGN frac | 0.20 |
| Host frac | 0.80 |
| log L5100,Host | 43.11 |
| Fe II/Hβ | — |
| Fe II/[O III] | 1.55 |
spurious_hab/hbb | 0.0/0 |
|---|---|
l5100 | 1 |
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.