标题： ALMA-ALPAKA巡天I：z = 0.5-3.5星形成星系的高分辨率CO和[CI]动力学特性 显示英文标题

标题： The ALMA-ALPAKA survey I: high-resolution CO and [CI] kinematics of star-forming galaxies at z = 0.5-3.5

摘要： 星系运动学的空间分辨研究提供了对其组装和演化的关键见解，使我们能够推断暗物质晕的属性，推导反馈对星际介质（ISM）的影响，并表征外流运动。 迄今为止，大多数红移 z=0.5-3.5 的运动学研究是通过追踪温暖电离气体的发射线获得的。 然而，这些是否提供了星系动力学和星际介质性质的完整视图，还是仅提供部分视图，仍然存在争议。 因此，需要对冷气体运动学进行互补性洞察。 我们介绍了 ALPAKA 项目，该项目旨在从 ALMA 公共档案馆收集 z=0.5-3.5 星形成星系的 CO 和 [CI] 发射线的高分辨率观测数据。 在总积时 147 小时内，ALPAKA 为 28 个星形成星系提供了 ~0.25'' 观测，这是 z>0.5 星系冷气体运动学（由 CO 或 [CI] 跟踪）的最大样本。 通过结合多波段辅助数据，我们推导了目标的恒星质量（$M_{\star}$）和恒星形成率（SFR），发现值为$M_{\star}\gtrsim 10^{10}$ M$_{\odot}$和 SFR 为 10-3000 M$_{\odot}$/yr。 ALPAKA 星系中有很大一部分（19/28）位于过密区域（星团、星群和原星团）。 我们利用 ALMA 数据推断它们的动力学状态，发现 19/28 ALPAKA 星系是旋转盘状星系，2 个是相互作用系统，而其余 7 个源的分类不确定。 这些盘状星系的速度弥散度值通常在最内部区域比外围更大，整个盘状样本的中位数为 35$^{+11}_{-9}$km/s。 尽管我们的样本偏向于宿主非常活跃机制的星系，但 ALPAKA 盘状星系具有高比例的有序运动与随机运动比值（$V/\sigma$），其中值为 9$^{+7}_{-2}$。 显示英文摘要

摘要： Spatially-resolved studies of the kinematics of galaxies provide crucial insights into their assembly and evolution, enabling to infer the properties of the dark matter halos, derive the impact of feedback on the ISM, characterize the outflow motions. To date, most of the kinematic studies at z=0.5-3.5 were obtained using emission lines tracing the warm, ionized gas. However, whether these provide an exhaustive or only a partial view of the dynamics of galaxies and of the properties of the ISM is still debated. Complementary insights on the cold gas kinematics are therefore needed. We present ALPAKA, a project aimed at gathering high-resolution observations of CO and [CI] emission lines of star-forming galaxies at z=0.5-3.5 from the ALMA public archive. With 147 hours of total integration time, ALPAKA assembles ~0.25'' observations for 28 star-forming galaxies, the largest sample with spatially-resolved cold gas kinematics as traced by either CO or [CI] at z>0.5. By combining multi-wavelength ancillary data, we derive the stellar masses ($M_{\star}$) and star-formation rates (SFR) for our targets, finding values of $M_{\star}\gtrsim 10^{10}$ M$_{\odot}$ and SFR of 10-3000 M$_{\odot}$/yr. A large fraction of ALPAKA galaxies (19/28) lie in overdense regions (clusters, groups, and protoclusters). We exploit the ALMA data to infer their dynamical state and we find that 19/28 ALPAKA galaxies are rotating disks, 2 are interacting systems, while for the remaining 7 sources the classification is uncertain. The disks have velocity dispersion values that are typically larger in the innermost regions than in the outskirts, with a median value for the entire disk sample of 35$^{+11}_{-9}$ km/s. Despite the bias of our sample towards galaxies hosting very energetic mechanisms, the ALPAKA disks have high ratios of ordered-to-random motion ($V/\sigma$) with a median value of 9$^{+7}_{-2}$.