Quasar Sightline and Galaxy Evolution (QSAGE) - III. The mass-metallicity and fundamental metallicity relation of z ˜ 2.2 galaxies
Quasar Sightline and Galaxy Evolution (QSAGE) - III. The mass-metallicity and fundamental metallicity relation of z ˜ 2.2 galaxies
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类星体视线和星系演化 (QSAGE) - III。
DOI：
10.1093/mnras/stad3721
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发表时间：
2024
影响因子：
4.8
通讯作者：
Stephenson H
中科院分区：
文献类型：
--
作者：
Stephenson H
我们利用哈勃空间望远镜宽视场相机3棱镜光谱分析了类星体视线和星系演化巡天中67个红移范围为z = 1.99−2.32（zmed= 2.16）的恒星形成（SF）星系的质量-金属丰度关系（MZR）。根据强发射线[Oii]3727、3729、[Oiii]4959、5007和Hβ，使用经验气相金属度校准确定金属度。SF星系被确定，并从活动星系核，通过质量激发图区分。使用z = 0的金属丰度校准，我们观察到一个负的偏移量在thez= 2.2 MZR的金属丰度的δ-0.51 dex相比，本地推导的关系，与以前的文献分析。当使用适用于2005年的经验金属丰度校准时，发现金属丰度的类似偏移量为2.46 dex，尽管在这种情况下，ourz= 2.2 MZR具有较浅的斜率。我们发现我们的MZR和那些从各种星系演化模型和模拟预测之间的协议。此外，我们探讨了扩展的基本金属丰度关系（FMR），其中包括一个额外的依赖于星星形成率。我们的结果一致支持FMR的存在，并揭示了与本地导出的关系相比，金属丰度的偏移量为0.28 ± 0.04 dex，与以前在类似红移下的研究一致。我们解释的负相关性与SFR在固定的质量，从我们的样品中存在的FMR推断，作为在宇宙中午的金属贫气体燃料SFR的有效吸积所造成的。
We present analysis of the mass–metallicity relation (MZR) for a sample of 67 [Oiii]-selected star-forming (SF) galaxies at a redshift range ofz= 1.99−2.32 (zmed= 2.16) usingHubble Space TelescopeWide Field Camera 3 grism spectroscopy from the Quasar Sightline and Galaxy Evolution survey. Metallicities were determined using empirical gas-phase metallicity calibrations based on the strong emission lines [Oii]3727, 3729, [Oiii]4959, 5007 and Hβ. SF galaxies were identified, and distinguished from active-galactic nuclei, via Mass–Excitation diagrams. Usingz∼ 0 metallicity calibrations, we observe a negative offset in thez= 2.2 MZR of ≈−0.51 dex in metallicity when compared to locally derived relationships, in agreement with previous literature analysis. A similar offset of ≈−0.46 dex in metallicity is found when using empirical metallicity calibrations that are suitable out toz∼ 5, though ourz= 2.2 MZR, in this case, has a shallower slope. We find agreement between our MZR and those predicted from various galaxy evolution models and simulations. Additionally, we explore the extended fundamental metallicity relation (FMR) which includes an additional dependence on star formation rate. Our results consistently support the existence of the FMR, as well as revealing an offset of 0.28 ± 0.04 dex in metallicity compared to locally derived relationships, consistent with previous studies at similar redshifts. We interpret the negative correlation with SFR at fixed mass, inferred from an FMR existing for our sample, as being caused by the efficient accretion of metal-poor gas fuelling SFR at cosmic noon.