论文标题
搜索主机属性与$ {\ rm dm_ {host}} $的$ {\ rm dm_ {host}} $：baryon质量分数的约束
Search for the correlations between host properties and ${\rm DM_{host}}$ of fast radio bursts: constraints on the baryon mass fraction in IGM
论文作者
论文摘要
快速无线电突发（FRB）作为探针进行研究，以研究天体物理学和宇宙学，需要对银河系的分散度（$ {\ rm dm_ {mw}} $）进行适当的建模（$ {\ rm dm_ {mw}} $）和宿主galaxy（$ {$ {\ rm dm_ dm_ {host}} $）。 $ {\ rm dm_ {mw}} $可以使用银河系电子模型（例如NE2001型号和YMW16模型）估算。但是，由于FRB的本地环境的信息有限，因此很难建模$ {\ rm dm_ {host}} $。在本文中，使用17个稳定的FRB，我们搜索$ {\ rm dm_ {host}} $之间的可能相关性与主机星系的属性，例如红移，恒星质量，星形形成率，星系时代，银河系的时代，FRB现场的偏移，是FRB现场的偏移，是FRB的偏移，从Galactic Center和Heft Lift the Halfight and and the Halfipt and and off the Halfipt lift and the Halfipt and of。我们发现$ {\ rm dm_ {host}} $与任何主机属性之间没有强大的相关性。假设$ {\ rm dm_ {host}} $是所有主机星系的常数，我们将今天的baryon质量限制为$ f _ {\ rm Igm，0} = 0.78 _ { - 0.19}}^{-0.19}^{+0.15} $。但是，如果我们将$ {\ rm dm_ {host}} $作为对数正态分布的建模，但是，我们获得了更大的值，$ f _ {\ rm Igm，0} = 0.83 _ { - 0.17}^{+0.12} $。基于有限数量的FRB，找不到$ f _ {\ rm igm} $的红移演变的有力证据。
The application of fast radio bursts (FRBs) as probes to investigate astrophysics and cosmology requires the proper modelling of the dispersion measures of Milky Way (${\rm DM_{MW}}$) and host galaxy (${\rm DM_{host}}$). ${\rm DM_{MW}}$ can be estimated using the Milky Way electron models, such as NE2001 model and YMW16 model. However, ${\rm DM_{host}}$ is hard to model due to limited information on the local environment of FRBs. In this paper, using 17 well-localized FRBs, we search for the possible correlations between ${\rm DM_{host}}$ and the properties of host galaxies, such as the redshift, the stellar mass, the star-formation rate, the age of galaxy, the offset of FRB site from galactic center, and the half-light radius. We find no strong correlation between ${\rm DM_{host}}$ and any of the host property. Assuming that ${\rm DM_{host}}$ is a constant for all host galaxies, we constrain the fraction of baryon mass in the intergalactic medium today to be $f_{\rm IGM,0}=0.78_{-0.19}^{+0.15}$. If we model ${\rm DM_{host}}$ as a log-normal distribution, however, we obtain a larger value, $f_{\rm IGM,0}=0.83_{-0.17}^{+0.12}$. Based on the limited number of FRBs, no strong evidence for the redshift evolution of $f_{\rm IGM}$ is found.
