2019MNRAS.483.5491I

We have obtained optical spectroscopy of one of the most metal-poor dwarf star-forming galaxies (SFG) in the local Universe, J1234+3901, with the Large Binocular Telescope (LBT)/Multi-Object Dual Spectrograph (MODS). This blue compact dwarf (BCD) galaxy with a redshift z = 0.133 was selected from the Data Release 14 (DR14) of the Sloan Digital Sky Survey (SDSS). Its properties are extreme in many ways. Its oxygen abundance 12 + log O/H = 7.035 ± 0.026 is among the lowest ever observed for a SFG. Its absolute magnitude M_g = -17.35 mag makes it the brightest galaxy among the known BCDs with 12 + log O/H ≲7.3. With its low metallicity, low stellar mass M_* = 10^7.13 M_☉ and very low mass-to-light ratio M_*/L_g ∼ 0.01 (in solar units), it deviates strongly from the mass–metallicity and luminosity–metallicity relations defined by the bulk of the SFGs in SDSS DR14. J1234 + 3901 has a very high specific star-formation rate sSFR ∼ 100 Gyr^–1, indicating very active ongoing star formation. Its spectrum shows a strong He II λ4686 emission line, with a flux ∼2.4 per cent that of the Hβ emission line. The most probable source of ionizing radiation for producing such a strong line is fast radiative shocks. J1234+3901 has a ratio O₃₂ = [O III] λ5007/[O II] λ3727 ∼ 15, the highest among the lowest-metallicity SFGs, and is thus likely leaking Lyman continuum radiation. It is a good candidate for being a young dwarf galaxy, with a large fraction of its stars formed recently. As such, it is probably one of the best local counterparts of dwarf primeval galaxies responsible for the reionization of the early Universe.