Exploiting the data from the GAs Stripping Phenomena in galaxies with MUSE (GASP) survey, we study the gas-phase metallicity scaling relations of a sample of 29 cluster galaxies undergoing ram-pressure stripping and of a reference sample of (16 cluster and 16 field) galaxies with no significant signs of gas disturbance. We adopt the PYQZ code to infer the mean gas metallicity at the effective radius and achieve a well-defined mass-metallicity relation (MZR) in the stellar mass range $10^{9.25}\le M_\star \le 10^{11.5}\,{\rm M_\odot}$ with a scatter of 0.12 dex. At any given mass, reference cluster and stripping galaxies have similar metallicities, while the field galaxies with $M_\star < 10^{10.25}\,{\rm M_\odot}$ show on average lower gas metallicity than galaxies in clusters. Our results indicate that at the effective radius the chemical properties of the stripping galaxies are independent of the ram-pressure stripping mechanism. Nonetheless, at the lowest masses we detect 4 stripping galaxies well above the common MZR that suggest a more complex scenario. Overall, we find signs of an anti-correlation between the metallicity and both the star formation rate and the galaxy size, in agreement with previous studies. No significant trends are instead found with the halo mass, clustercentric distance and local galaxy density in clusters. In conclusion, we advise a more detailed analysis of the spatially resolved gas metallicity maps of the galaxies, able to highlight effects of gas redistribution inside the disk due to the ram-pressure stripping.

中文翻译：

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GASP XXVII：具有和不具有冲压压力剥离的盘状星系的气相金属度比例关系

利用 MUSE (GASP) 调查星系中 GAs 剥离现象的数据，我们研究了 29 个进行冲压压力剥离的星系团样本和（16 个星系团和 16 个场）的参考样本的气相金属丰度标度关系。 ) 没有明显气体扰动迹象的星系。我们采用 PYQZ 代码来推断有效半径处的平均气体金属丰度，并在恒星质量范围 $10^{9.25}\le M_\star \le 10^{11.5} 内实现明确定义的质量金属丰度关系（MZR） \,{\rm M_\odot}$ 散布为 0.12 dex。在任何给定的质量下，参考星团和剥离星系具有相似的金属丰度，而 $M_\star < 10^{10.25}\,{\rm M_\odot}$ 的场星系平均显示出比星团星系更低的气体金属丰度。我们的结果表明，在有效半径处，剥离星系的化学性质与冲压压力剥离机制无关。尽管如此，在最低质量处，我们检测到 4 个剥离星系，远高于常见的 MZR，这表明了更复杂的情况。总的来说，我们发现金属丰度与恒星形成率和星系大小之间存在反相关的迹象，这与之前的研究一致。相反，在星团中没有发现晕质量、星团中心距离和局地星系密度的显着趋势。总之，我们建议对星系的空间分辨气体金属丰度图进行更详细的分析，能够突出由于冲压压力剥离导致的盘内气体重新分布的影响。