标题： 快速射电暴的宇宙演化和恒星形成率 显示英文标题

标题： Cosmological Evolution of Fast Radio Bursts and The Star Formation Rate

摘要： 我们研究快速射电暴（FRBs）的光度和红移的宇宙学演化。 如同所有河外源一样，我们处理的数据受到观测选择效应的截断，其中最重要的是流量极限，这引入了所谓的爱丁顿-马尔姆奎斯特偏差。 此外，对于FRBs而言，从观测到的色散量（DMs）获得的红移存在显著的不确定性。 为了校正截断，我们使用非参数、非分箱的Efron-Petrosian和Lynden-Bell方法，这些方法能给出光度和红移及其宇宙学演化的无偏分布。 为了量化红移的不确定性，我们使用一个数据集，该数据集考虑了宿主星系对DM的贡献不确定性和由于星际介质波动引起的DM不确定性。 这个数据集除了平均红移外，还给出了1σ误差。 我们构建了三个样本，分别具有较低、平均和较高的红移，并将上述方法应用于每个样本。 对于这三个样本，我们发现类似的（1）$\sim 3\sigma$证据表明光度演化，（2）光度函数可以用简单的分段幂律拟合，以及（3）共动密度形成率随红移迅速下降，与宇宙恒星形成率（SFR）不同。 这一速率类似于短伽马射线暴，它们被认为是由紧凑星体合并产生的，其形成率相对于SFR有所延迟。 这可能进一步支持磁星是FRBs前身天体的假说。 显示英文摘要

摘要： We investigate the cosmological evolution of the luminosity and redshift of FRBs. As is the case for all extragalactic sources, we are dealing with data that are truncated by observational selection effects, the most important being the flux limit, which introduces the so-called Eddington-Malmquist bias. In addition, for FRBs, there is a significant uncertainty in the redshifts obtained from the observed dispersion measures (DMs). To correct for the truncation we use the non-parametric, non-binning Efron-Petrosian and Lynden-Bell methods, which give unbiased distributions of luminosities and redshifts and their cosmological evolution. To quantify the redshift uncertainty, we use a data set which accounts for uncertainties of contribution to the DM of the host galaxy, and DM uncertainties due to fluctuation in the intergalactic medium. This data, in addition to a mean redshift, gives the one-sigma errors. We construct three samples with lower, mean, and upper redshifts and apply the above methods to each. For the three samples, we find similar (1) $\sim 3\sigma$ evidence for luminosity evolution, (2) a luminosity function that can be fit by a simple broken power law, and (3) a comoving density formation rate that decreases rapidly with redshift unlike the cosmic star formation rate (SFR). This rate is similar to that of short gamma-ray bursts, which are believed to result from compact star mergers with a formation rate delayed relative to the SFR. This may further support the hypothesis that magnetars are the progenitors of FRBs.