We present a comparison between the [Ca,C,N/Fe]-mass relations observed in local spheroids and the results of a chemical evolution model which already successfully reproduces the [Mg/Fe]-mass and the [Fe/H]-mass relations in these systems. We find that the [Ca/Fe]-mass relation is naturally explained by such a model without any additional assumption. In particular, the observed under-abundance of Ca with respect to Mg can be attributed to the different contributions from supernovae Type Ia and supernovae Type II to the nucleosynthesis of these two elements. For C and N, we consider new stellar yields that take into account stellar mass loss and rotation. These yields have been shown to successfully reproduce the C and N abundances in Milky Way metal-poor stars. The use of these new stellar yields produces a good agreement between the chemical evolution model predictions and the integrated stellar population observations for C. In the case of N, the inclusion of fast rotators and stellar mass-loss nucleosynthesis prescriptions improves our predictions for the slope of the [N/Fe] vs. sigma relation, but a zero point discrepancy of 0.3 dex remains. This work demonstrates that current stellar yields are unable to simultaneously reproduce the large mean stellar [<N/Fe>] ratios inferred from integrated spectra of elliptical galaxies and the low N abundance measured in the gas of high redshift spheroids from absorption lines. However, it seems reasonable to suggest that there may be uncertainties in either the inferred stellar or gas-phase N abundances at the level of 0.3 dex. (abriged)
Chemical enrichment in the Ophiuchus cluster core studied by high-resolution XRISM spectroscopy
Institute of Space and Astronautical Science, JAXA（宇宙科学研究所）；Department of Physics, Tokyo Metropolitan University（东京都立大学物理系）；Department of Astrophysics and Atmospheric Sciences, Kyoto Sangyo University（京都产业大学天体物理学与大气科学系）；Department of Physics, Hiroshima University（广岛大学物理系）；Department of Physics, Saitama University（埼玉大学物理系）
利用高分辨率XRISM光谱学研究Ophiuchus团核心的化学富集，发现其X/Fe比值与太阳一致，通过核心坍缩和Ia型超新星模型解释丰度模式，揭示Ca的不足可能由Ca-rich gap transients贡献。
We present a detailed analysis of the elemental abundances distribution of the Virgo cluster using {\it XMM-Newton} observations. We included in the analysis a new EPIC-pn energy scale calibration which allow us to measure velocities with uncertainties down to $Δv \sim 150$ km/s. We investigate the radial distribution of O, Ne, Mg, Si, Ar, S, Ca, Ni and Fe. We found that the best-fit model is close to a single-temperature component for distances $>80$~kpc and the cooler gas is more metal-rich. Discontinuities in temperature are found around $\sim30$~kpc and $\sim90$~kpc, which correspond to th…
We propose a semi-analytic model that is developed to understand the cosmological evolution of the mean metallicity in the Universe. In particular, we study the contributions of Population III (Pop III) and Population II (Pop II) stars to the production of $\mathrm{Fe,~Si,~Zn, ~Ni,~P, ~Mg, ~Al, ~S, ~C, ~N}$, and $\mathrm{~O}$. We aim to quantify the roles of two different models in the chemical enrichment of the Universe. The first model (A) considers both stars with Pop III and Pop II yields. For the second model (B), the yields involved are only for Pop II stars. We start by describing the c…
Galaxies throughout the last 12 Gyr of cosmic time follow a single, universal relation that connects their star-formation rates (SFRs), stellar masses ($M_\star$) and chemical abundances. Deviation from these fundamental scaling relations would imply a drastic change in the processes that regulate galaxy evolution. Observations have hinted at the possibility that this relation may be broken in the very early universe. However, until recently, chemical abundances of galaxies could be only measured reliably as far back as redshift $z=3.3$. With JWST, we can now characterize the SFR, $M_\star$, a…
In this paper, we report the relative SNe contributions on the metal budget of the ICM of Abell 1837 galaxy cluster at redshift z $=$ 0.069. For this purpose, we analysed the hot ICM of the cluster and obtained radial metal distributions by using XMM-Newton archival data with total exposure $\sim$100 ks. These metal measurements consist of Mg, Si, S, Fe and Ni within 0.7 R$_{500}$ radius which is divided into three concentric annuli. In order to explain the observed metal abundance pattern in terms of relative supernova contributions, we used our newly developed code SNeRatio which utilizes th…
Environmental Effects on the Metal Enrichment of Low Mass Galaxies in Nearby Clusters
在本文中，我们研究了低质量恒星形成（SF）星系的化学历史的本地宇宙星系团后发座，A1367，A779和A634。这项工作的目的是寻找环境对这些星系化学演化的影响。星系的化学演化与恒星形成历史（SFH）以及与环境的气体交换有关，众所周知，低质量星系是易受环境过程影响的系统。在我们的研究中，我们使用了SDSS-III DR 8的光谱。我们研究了星系团星系的质量-金属丰度关系，发现了定义明确的序列。这些序列的斜率，在低质量的星系团和星系在大集群中心的距离，遵循最近的流体动力学模型的预测。一个平坦的斜坡已被观察到的星系位于核心的两个更大的集群的样本，主要是在后发座，这表明集群环境的SF星系的化学演化的印记应该是敏感的星系质量和主机集群质量。后发座和A1367星系的HI气体含量表明，低质量SF星系，位于这些星系团的核心，受到严重的影响，冲压压力剥离。根据流体动力学模拟，在致密环境中观察到的低质量星系金属含量的质量依赖性增强似乎是合理的。这种增强的金属富集可以产生的组合效应，如风的再吸积，由于压力coinfinement的集群内介质（ICM），和截断的气体入流，作为一个结果的冲压压力剥离。因此，ICM的性质应该在团簇中低质量星系的化学演化中发挥重要作用。
