标题： 使用SIMBA追踪高红移宁静星系中的尘埃和冷气体的演化路径 显示英文标题

标题： Tracing the evolutionary pathways of dust and cold gas in high-z quiescent galaxies with SIMBA

摘要： 高红移（$z\gtrsim 1-2$）宁静星系（QGs）中发现大量尘埃，这挑战了传统观点，即这些天体的星际介质（ISM）与其恒星质量成比例地较少。 我们使用SIMBA宇宙学模拟来探索宁静星系中尘埃和冷气体含量随星系淬火过程的变化。 我们追踪了在场环境和星团环境中于$0 \lesssim z \lesssim2$处识别出的QGs的星际介质尘埃丰度变化。 QGs通过多样化的方式淬灭，既有快速的也有缓慢的，并且在淬灭事件与冷气体去除之间的时间跨度范围很广（从$\sim650$百万年到$\sim8$十亿年）。 我们发现，由活动星系核（AGN）反馈引起的淬灭模式不会在同一时间尺度内影响尘埃和冷气体。 值得注意的是，QGs可能主要由于内部过程而在淬灭阶段补充其尘埃含量，外部因素如小规模合并也起到次要作用。 重新形成尘埃的关键机制是气相金属的持续颗粒生长，该过程在淬灭事件后$\sim100$百万年内有效，并迅速将QGs中的尘埃-气体质量比提高到标准值以上（$\delta_{\rm DGR}\gtrsim1/100$）。 因此，尽管冷气体储库严重耗尽，大约一半的QGs在其恒星年龄在淬灭后的前2Gyr内，其星际介质中的尘埃几乎没有演化。 总体而言，我们预测相对尘埃较多的星系群（$M_{\rm dust}/M_{\star}\gtrsim10^{-3}-10^{-4}$）起源于快速和缓慢的淬灭机制，并且在中间质量和低恒星质量的系统中普遍存在（$9<\log(M_{\star}/M_{\odot})<10.5$）。 这一预测立即引发了例如詹姆斯韦伯太空望远镜（JWST）和阿塔卡马大型毫米波阵列（ALMA）之间的观测协同作用的问题。 显示英文摘要

摘要： Recent discoveries of copious amounts of dust in quiescent galaxies (QGs) at high redshifts ($z\gtrsim 1-2$) challenge the conventional view that these objects have poor interstellar medium (ISM) in proportion to their stellar mass. We use the SIMBA cosmological simulation to explore the evolution of dust and cold gas content in QGs in relation to the quenching processes affecting them. We track the changes in the ISM dust abundance across the evolutionary history of QGs identified at $0 \lesssim z \lesssim2$ in the field and cluster environments. The QGs quench via diverse pathways, both rapid and slow, and exhibit a wide range of times elapsed between the quenching event and cold gas removal (from $\sim650$ Myr to $\sim8$ Gyr). We find that quenching modes attributed to the feedback from active galactic nuclei (AGN) do not affect dust and cold gas within the same timescales. Remarkably, QGs may replenish their dust content in the quenched phase primarily due to internal processes and marginally by external factors such as minor mergers. The key mechanism for re-formation of dust is prolonged grain growth on gas-phase metals, it is effective within $\sim100$ Myr after the quenching event, and rapidly increases the dust-to-gas mass ratio in QGs above the standard values ($\delta_{\rm DGR}\gtrsim1/100$). As a result, despite heavily depleted cold gas reservoirs, roughly half of QGs maintain little evolution in their ISM dust with stellar age within the first 2 Gyr following the quenching. Overall, we predict that relatively dusty QGs ($M_{\rm dust}/M_{\star}\gtrsim10^{-3}-10^{-4}$) arise from both fast and slow quenchers, and are prevalent in systems of intermediate and low stellar masses ($9<\log(M_{\star}/M_{\odot})<10.5$). This prediction poses an immediate quest for observational synergy between e.g., James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA).