We present a simulation probing the formation of water in the remnant of low-mass Population III supernovae in a cosmological minihalo, and provide a tentative lower mass limit on host minihaloes that can recollapse on a short enough timescale and efficiently mix metals at high densities. We start from cosmological initial conditions and end the simulation when the central density undergoes catastrophic recollapse, whereby the water abundance is reported. During the Population III stars lifetime, the minihalo (M$ = 5 \times 10^5$ M$_{\odot}$) becomes blown out, and consequently the faint supernova explosion (E$_{\mathrm{SN}} = 5\times 10^{50}$ ergs) is completely unconfined to the virial radius of the minihalo. At the end of the simulation there is no significant water formation anywhere throughout the remnant, and the central recollapsing region is inefficient at incorporating the first metals into itself, remaining at low metallicity. The majority of metals are ejected from the core via bipolar outflow into the void and reach a peak metallicity of $\mathrm{Z} \sim 10^{-6}\ \mathrm{Z}_{\odot}$ at very low densities. The mass of the minihalo is low enough such that the recollapse timescale is unreasonable for this configuration to be the primary avenue of water formation in the early universe. We also provide a comparison with a regular CCSN (E$_{\mathrm{SN}} = 10^{51}$ ergs) and find the same effect, but amplified. As such, we can suggest that the minimum minihalo mass required for a confined explosion, and therefore the possibility of water formation is at least $10^{6}$ M$_{\odot}$ and the chemo-thermal evolution of a supernova remnant is more sensitive to the mass of the host minihalo than the mass of the Population III star residing within it.
Constraining early-time dust formation in core-collapse supernovae
核心坍缩超新星（CCSNe）尘埃形成的理论模型预测在$\sim 1000$天内形成的喷出物尘埃的$\gtrsim 0.01$ M $_\odot$，与这些时期的观测结果之间存在严重的差异，这推断出更低的质量。我们证明，在光学薄的情况下，这些低尘埃质量是强大的，尽管显着的观测和模型的不确定性。对于11个观测良好的CCSNe样本，没有合理的模型达到$10^{-4}$ M $_\odot$以上的碳尘质量，或$\sim 10^{-3}$ M $_\odot$以上的硅酸盐质量。光学厚的模型可以容纳更大的尘埃质量，但尘埃必须聚集在一起，并有一个低（$<0.1$）覆盖分数，以避免与光学波长的数据冲突。这些值是不足以重现所观察到的红外通量，所需的覆盖率不仅不同SNe之间，但时代之间的同一对象。在协调大型尘埃质量与早期的CCSNe观测的困难，结合完善的检测超新星遗迹中的巨大尘埃质量，表明后期尘埃形成的机制是必要的。
Constraining the Sub-Galactic Relationship Between Star Formation and the Hot Interstellar Medium in NGC 4254
Middle Tennessee State University（中田纳西州立大学）；Pennsylvania State University（宾夕法尼亚州立大学）；University of Arkansas（阿肯色大学）；The Ohio State University（俄亥俄州立大学）；European Southern Observatory（欧洲南方天文台）
The Nearby Star Formation and Supernova Histories Reconstructed from Young Star Clusters
Center for Astrophysics — Harvard & Smithsonian（天体物理中心——哈佛与史密森尼学会）；Department of Astrophysics, University of Vienna（维也纳大学天体物理学系）；Department of Physics, University of Wisconsin–Whitewater（威斯康星大学惠特沃分校物理系）
Warm Ionized Gas Revealed in the Magellanic Bridge Tidal Remnant: Constraining the Baryon Content and the Escaping Ionizing Photons around Dwarf Galaxies
Constraining the Galactic Center Dark Cluster with ELT/MICADO Observations
Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学理论天体物理研究所）；Max Planck Institute for Radioastronomy（马克斯·普朗克射电天文研究所）；Department of Theoretical Physics and Astrophysics, Masaryk University（马萨里克大学理论与天体物理学系）
Constraining Lens Masses in Moderately to Highly Magnified Microlensing Events from Gaia
University of Warsaw（华沙大学）；National Centre for Nuclear Research（国家核研究中心）；University of Wrocław（弗罗茨瓦夫大学）；Nicolaus Copernicus University in Toruń（托伦哥白尼大学）
