Table 1.
LFBOTs, their host metallicities, and references.
| LFBOT | Z/Z⊙ | Reference |
|---|---|---|
| AT 2018cow | 0.47 ± 0.01 | Lyman et al. (2020)a |
| ZTF18abvkwla | ∼0.37 | Ho et al. (2020) |
| CSS161010 | ∼0.15 | Gutiérrez et al. (2024) |
| ZTF20acigmel | 0.15 |
Perley et al. (2021)b |
| AT2020mrf | 0.27 |
Yao et al. (2022) |
| AT2023fhn | 0.08 ± 0.02 | Chrimes et al. (2024a) |
| AT2024wpp | 0.53 |
Pursiainen et al. (2025)b |
Notes. Other LFBOT candidates exist, but have insufficient follow up to confirm their nature or to characterise the host galaxy (e.g. we have no Z estimate for AT2022tsd). In cases where the metallicities are reported in 12+log(O/H), we converted to mass fractions following a linear interpolation of the values in Table 2 of Xiao et al. (2018). For CSS161010, we adopted the gas-phase metallicity determined with emission lines (Gutiérrez et al. 2024), as this is likely more representative of recently formed stars in the galaxy. (a)IFU metallicity measurement, resolving the host giving a local (few hundred parsec scale) value. (b)Metallicity derived from the host’s total stellar mass using Equation 3 of Tremonti et al. (2004). Uncertainties are solely propagated from uncertainties on the galaxy stellar mass and do not include scatter in the M − Z relation.
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