Since the epoch of cosmic star formation peak at $z \sim 2$, most of it is obscured in high mass galaxies, while in low mass galaxies the radiation escapes unobstructed. During the reionization epoch, the presence of evolved, dust obscured galaxies are a challenge to galaxy formation and evolution models. By means of a chemodynamical evolution model, we investigate the star formation and dust production required to build up the bulk of dust in galaxies with initial baryonic mass ranging from $7.5 \times 10^{7}$~M$_\odot$ to $2.0 \times 10^{12}$~M$_\odot$. The star formation efficiency was also chosen to represent the star formation rate from irregular dwarf to giant elliptical galaxies. We adopted a dust coagulation efficiency from \citep[][Case A]{dwek1998evolution} as well as a lower efficiency one (Case B), about five times smaller than Case A. All possible combination of these parameters was computed, summing forty different scenarios. We find that in high stellar formation systems the dust accretion in ISM rules over stellar production before the star formation peak, making these systems almost insensible to dust coagulation efficiency. In low star formation systems, the difference between Case A and B lasts longer, mainly in small galaxies. Thus, small irregular galaxies should be the best place to discriminate different dust sources. In our observational sample, taken from the literature, dust-to-gas ratio tends to be more spread only than dust mass, for both stellar mass and star formation rate. Dust-to-gas vs. dust-to-star diagram is a good tracer for both galaxy and dust evolution, due to the link between gas, star, dust and star formation rate. However, the model do not constrain simultaneously all this quantities. The new generation facilities (such as JWST, ELT, VLT and SPICA) will be indispensable to constrain dust formation across the cosmic time.

中文翻译：

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高低红移下尘埃聚集和星系遮蔽的理论线索

由于宇宙恒星形成的时代在 $z \sim 2$ 达到峰值，因此大部分在高质量星系中被遮蔽，而在低质量星系中，辐射不受阻碍地逃逸。在再电离时代，进化的、被尘埃遮挡的星系的存在对星系形成和演化模型是一个挑战。通过化学动力学演化模型，我们研究了星系中形成大量尘埃所需的恒星形成和尘埃产生，初始重子质量范围从 $7.5 \times 10^{7}$~M$_\odot$ 到 $2.0 \times 10^{12}$~M$_\odot$。恒星形成效率也被选择来代表从不规则矮星到巨椭圆星系的恒星形成率。我们采用了 \citep[][Case A]{dwek1998evolution} 中的粉尘凝结效率以及效率较低的一种（Case B），大约比 Case A 小五倍。计算了这些参数的所有可能组合，总结了四十种不同的场景。我们发现在高恒星形成系统中，ISM 中的尘埃吸积在恒星形成高峰之前支配了恒星的产生，使得这些系统对尘埃凝结效率几乎不敏感。在低恒星形成系统中，情况 A 和 B 之间的差异持续时间更长，主要是在小星系中。因此，小的不规则星系应该是区分不同尘埃源的最佳场所。在我们从文献中获取的观测样本中，对于恒星质量和恒星形成率而言，尘埃与气体的比率往往仅比尘埃质量更分散。由于气体、恒星、尘埃和恒星形成率之间的联系，尘埃-气体与尘埃-恒星图是星系和尘埃演化的良好示踪剂。然而，该模型不会同时约束所有这些量。新一代设施（如 JWST、ELT、VLT 和 SPICA）对于限制整个宇宙时间的尘埃形成是必不可少的。