标题： 罗塞塔石碑项目。 一。 高质量恒星形成团块的辐射磁流体动力学模拟套件 显示英文标题

标题： The Rosetta Stone Project. I. A suite of radiative magnetohydrodynamics simulations of high-mass star-forming clumps

摘要： 上下文。 恒星形成，特别是大质量恒星形成，是天体物理过程中关键的环节，但目前仍远未被完全理解。 不幸的是，这些领域的进展缓慢，因为观测结果难以解释，无法直接与数值模拟进行比较。 因此，合成观测是必要的，以更好地约束模型。 目标。 通过罗塞塔石项目，我们的目标是开发一个端到端的流程，尽可能准确地将恒星形成模拟与观测进行比较，以研究从云团尺度到恒星的演化过程。 方法。 使用自适应网格细化代码RAMSES，我们计算了一个初始的模型网格，用于开发我们的流程并探索云团初始条件对其演化的影响力。 这一组模拟的主要目的是转化为合成观测，以便与赫歇尔和ALMA观测到的真实恒星形成云团进行直接比较。 结果。 这里介绍的罗塞塔石模拟提供了一个可供完整后期处理并随后与观测进行比较的目录（RS1）。 在所有在此探讨的参数中，磁场强度对云团演化（碎片化、恒星形成、整体坍缩）在大尺度和小尺度上影响最大。 数值参数如每Jeans长度的分辨率或吸积到汇粒子的阈值会影响低质量汇的形成。 最后，广泛使用的L/M比被发现是一个很好的指示器，可以反映云团的演化状态，无论其初始条件如何，但当包含更多反馈过程（喷流、HII区）时，这可能会发生变化。 结论。 我们现在有一套新的恒星形成云团模拟，可供完整后期处理并随后与观测进行比较。 显示英文摘要

摘要： Context. Star formation and, in particular, high-mass star formation are key astrophysical processes that are far from being fully understood. Unfortunately, progress in these fields is slow because observations are hard to interpret as they cannot be directly compared to numerical simulations. Synthetic observations are therefore necessary to better constrain the models. Aims. With the Rosetta Stone project, we aim to develop an end-to-end pipeline to compare star formation simulations with observations as accurately as possible in order to study the evolution from clumps scales to stars. Methods. Using the adaptive mesh-refinement code RAMSES, we computed a first grid of model of star-forming clumps to develop our pipeline and explore the impact of the clump initial conditions on their evolution. The main purpose of this set of simulations is to be converted into synthetic observations to enable a direct comparison with real star-forming clumps observed with Herschel and ALMA. Results. The Rosetta Stone simulations presented here provide a catalog available for full post-processing and subsequent comparison with observations (RS1). Among all the parameters explored here, the strength of the magnetic field has the strongest influence on the clump evolution (fragmentation, star formation, global collapse) at both large and small scales. Numerical parameters such as the resolution per Jeans length or the threshold for accretion onto sink particles affects the formation of low-mass sinks. Finally, the widely used L/M ratio is found to be a good indicator of the clump evolutionary state regardless of its initial condition, but this could change when more feedback processes (jets, HII regions) are included. Conclusions. We now have a new suite of simulations of star-forming clumps that is available for full post-processing and subsequent comparison with the observations,