论文标题
快速无线电爆发宿主星系的分散度度量：宇宙模拟的估计
The dispersion measure of Fast Radio Bursts host galaxies: estimation from cosmological simulations
论文作者
论文摘要
快速无线电爆发的色散度量（DM）编码重要信息，例如其距离，中间介质的性质。基于Illustris和Illustristng项目中的模拟，我们分析了主机中星际介质和圆形培养基贡献的FRB的DM，$ \ rm {dm_ {host}} $。我们探讨了两个种群模型 - 追踪恒星形成率（SFR）和恒星质量，即年轻和老年祖细胞。 $ \ rm {dm_ {host}} $的分布在两个种群之间显示出$ z = 0 $的显着差异：恒星质量模型相对于SFR模型在低DM端表现出多余的差异。 SFR（恒星质量）模型的中值为$ \ rm {dm_ {host}} $ = 179（63）$ \ rm {pc \，cm^{ - 3}} $，用于$ m _*= 10^= 10^{8-13} {8-13} \，m _ = 10^{8-13} \，M _ { Illustris-1中的星系具有较小的$ \ rm {dm_ {host}} $。 $ \ rm {dm_ {host}} $的分布与两个模型的log-normal函数相关。此外，在主机的恒星质量功能中，空间偏移与主机中心的空间偏移中有两个群体相差。 $ \ rm {dm_ {host}} $随着$ m _*<10^{10.5} \，m _ {\ odot} $而增加主机的出色质量，并以较高的质量波动。在$ 0 <z <2 $，$ \ rm {dm_ {host}} $随着红移而增加。 $ \ rm {dm_ {host}} $之间两个种群之间的差异随着红移的增加而下降。随着将来更多的本地化事件，诸如$ \ rm {dm_ {host}} $之类的统计信息，Galaxy Center的偏移量和主机的出色质量功能将对确定FRB的起源非常有帮助。同时，本地化FRB事件的$ \ rm {dm_ {host}} $的统计信息可以帮助限制银河系进化中的baryon物理模型。
The dispersion measure(DM) of fast radio burst encodes important information such as its distance, properties of intervening medium. Based on simulations in the Illustris and IllustrisTNG projects, we analyze the DM of FRBs contributed by the interstellar medium and circumgalactic medium in the hosts, $\rm{DM_{host}}$. We explore two population models - tracing the star formation rate (SFR), and the stellar mass, i.e. young and old progenitors respectively. The distribution of $\rm{DM_{host}}$ shows significant differences at $z=0$ between two populations: the stellar mass model exhibits an excess at the low DM end with respect to the SFR model. The SFR (stellar mass) model has a median value of $\rm{DM_{host}}$=179 (63) $\rm{pc\, cm^{-3}}$ for galaxies with $M_*=10^{8-13}\,M_{\odot}$ in the TNG100-1. Galaxies in the Illustris-1 have a much smaller $\rm{DM_{host}}$. The distributions of $\rm{DM_{host}}$ deviate from log-normal function for both models. Furthermore, two populations differ moderately in the spatial offset from host galaxy's center, in the stellar mass function of hosts. $\rm{DM_{host}}$ increases with the stellar mass of hosts when $M_*<10^{10.5}\,M_{\odot}$, and fluctuate at higher mass. At $0<z<2$, $\rm{DM_{host}}$ increases with redshift. The differences in $\rm{DM_{host}}$ between two populations declines with increasing redshift. With more localized events available in the future, statistics such as $\rm{DM_{host}}$, the offset from galaxy center and the stellar mass function of hosts will be of great helpful to ascertain the origin of FRB. Meanwhile, statistics of $\rm{DM_{host}}$ of localized FRB events could help to constrain the baryon physics models in galaxy evolution.
