标题： 罗塞塔石碑项目。 III. ALMA对高质星形成云碎片的合成观测 显示英文标题

标题： The Rosetta Stone project. III. ALMA synthetic observations of fragmentation in high-mass star-forming clumps

摘要： 物理机制调控大质量秒差距尺度云团的坍缩并使其形成新的恒星群，这是恒星形成中的一个关键方面。为了研究这些机制，我们开发了罗塞塔石项目：一个端到端（模拟-观测）框架，该框架基于系统生成真实的大尺度云团碎片化合成观测数据，并将其与真实数据进行比较。在本工作中，我们将SQUALO调查的ALMA 1.3mm连续尘埃发射观测数据与一组新的24个高质云团碎片化的辐射磁流体动力学模拟进行比较，这些模拟使用CASA软件进行后期处理，以模仿SQUALO的观测策略。模拟初始化结合了典型的云团质量（500,1000太阳质量）和半径（约0.4pc）以及两种湍流水平（马赫数7,10）和三种磁化水平（质量-通量比约3,10,100）。通过沿三个正交方向投影的两个随机种子跟踪云团演化，我们生成了一组732个合成场。在约7000AU处的云团碎片化合成观测中，每个场中发现了2到14个碎片。在模拟的初始条件中，磁场对这些尺度上的碎片多重性影响最大。在云团演化的后期阶段，较少的碎片更倾向于与磁化云团相关。在约7000AU处识别的碎片在约75%的情况下对应于单个或多个吸积粒子，这表明并非所有碎片都在积极形成恒星。吸积粒子和碎片在整个云团演化过程中持续吸积质量，支持碎片与环境不隔离的情景。我们的研究证明了合成观测在解释干涉观测结果中的重要性。 显示英文摘要

摘要： The physical mechanisms that regulate the collapse of high-mass parsec-scale clumps and allow them to form clusters of new stars represent a crucial aspect of star formation. To investigate these mechanisms, we developed the Rosetta Stone project: an end-to-end (simulations-observations) framework that is based on the systematic production of realistic synthetic observations of clump fragmentation and their comparison with real data. In this work, we compare ALMA 1.3mm continuum dust emission observations from the SQUALO survey with a new set of 24 radiative magnetohydrodynamical simulations of high-mass clump fragmentation, post-processed using the CASA software to mimic the observing strategy of SQUALO. The simulations were initialized combining typical values of clump mass (500,1000 solar masses) and radius (~0.4pc) with two levels of turbulence (Mach number of 7,10) and three levels of magnetization (mass-to-flux ratio of ~3,10,100). Following the clump evolution over time with two random seeds projected along three orthogonal directions, we produced a collection of 732 synthetic fields. The synthetic observations of clump fragmentation at ~7000AU revealed between 2 and 14 fragments per field. Among the initial conditions of the simulations, magnetic fields have the largest impact on the fragment multiplicity at these scales. In advanced stages of clump evolution, a lower number of fragments is preferentially associated with magnetized clumps. Fragments identified at ~7000AU correspond to individual or multiple sink particles in ~75% of the cases, suggesting that not all fragments are actively forming stars. Both sinks and fragments accrete mass throughout the whole clump evolution, favoring a scenario in which fragments are not isolated from the environment. Our study demonstrates the importance of synthetic observations in interpreting results from interferometric observations.