EMPRESS. II. Highly Fe-Enriched Metal-poor Galaxies with 1.0 (Fe/O) and 0.02 (O/H) : Possible Traces of Super Massive (>300 M) Stars in Early Galaxies

Abstract

We present element abundance ratios and ionizing radiation of local young low-mass (~106 Msun) extremely metal poor galaxies (EMPGs) with a 2% solar oxygen abundance (O/H)sun and a high specific star-formation rate (sSFR~300 Gyr-1), and other (extremely) metal poor galaxies, which are compiled from Extremely Metal-Poor Representatives Explored by the Subaru Survey (EMPRESS) and the literature. Weak emission lines such as [FeIII]4658 and HeII4686 are detected in very deep optical spectra of the EMPGs taken with 8m-class telescopes including Keck and Subaru (Kojima et al. 2019, Izotov et al. 2018), enabling us to derive element abundance ratios with photoionization models. We find that neon- and argon-to-oxygen ratios are comparable to those of known local dwarf galaxies, and that the nitrogen-to-oxygen abundance ratios (N/O) are lower than 20% (N/O)sun consistent with the low oxygen abundance. However, the iron-to-oxygen abundance ratios (Fe/O) of the EMPGs are generally high; the EMPGs with the 2%-solar oxygen abundance show high Fe/O ratios of ~90-140% (Fe/O)sun, which are unlikely explained by suggested scenarios of Type Ia supernova iron productions, iron's dust depletion, and metal-poor gas inflow onto previously metal-riched galaxies with solar abundances. Moreover, these EMPGs have very high HeII4686/Hβ ratios of ~1/40, which are not reproduced by existing models of high-mass X-ray binaries whose progenitor stellar masses are less than 120 Msun. Comparing stellar-nucleosynthesis and photoionization models with a comprehensive sample of EMPGs identified by this and previous EMPG studies, we propose that both the high Fe/O ratios and the high HeII4686/Hβ ratios are explained by the past existence of super massive (>300 Msun) stars, which may evolve into intermediate-mass black holes (100 Msun).

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