高低红移时尘埃积累和星系遮蔽的理论线索
Theoretical clues about dust accumulation and galaxy obscuration at high and low redshift
摘要：
由于宇宙恒星形成的高峰期在$z \sim 2$，大部分在高质量星系中是模糊的，而在低质量星系中，辐射可以畅通无阻地逃逸。在再电离时期，尘埃遮蔽的演化星系的存在对星系形成和演化模型是一个挑战。利用化学动力学演化模型，研究了初始重子质量从$7.5 \times 10^{7}$ ~M $_\odot$到$2.0 \times 10^{12}$ ~M $_\odot$的星系中形成大量尘埃所需的恒星形成和尘埃产生过程.恒星形成效率也被用来代表从不规则矮星系到巨椭圆星系的恒星形成率。我们采用了来自\citep [][案例A]{dwek 1998 evolution}的粉尘凝聚效率以及较低效率的粉尘凝聚效率（案例B），约为案例A的五分之一。计算了这些参数的所有可能组合，总结了40种不同的情况。我们发现，在高恒星形成系统的尘埃吸积在ISM规则恒星生产之前，恒星形成的高峰，使这些系统几乎不敏感的尘埃凝聚效率。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。在我们的观测样本中，从文献中，尘埃与气体的比例往往比尘埃质量更分散，无论是恒星质量还是恒星形成率。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，该模型不同时约束所有这些量。新一代设施（如JWST，ELT，VLT和SPICA）将是不可或缺的，以限制整个宇宙时间的尘埃形成。
英文摘要：
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.
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