论文标题
使用毫秒瞬变的数据驱动技术来测量银河系光环
A Data-Driven Technique Using Millisecond Transients to Measure the Milky Way Halo
论文作者
论文摘要
我们介绍了一种新技术，以通过分析观察到的pulsars $ \ text {dm} _ \ text {dm} _ \ pulsar} $和快速的无线电爆发{$ \ flud text {pulsar} $，来限制我们银河系halo $ \ text {dm} _ \ text {mw，halo} $限制的视线集成电子密度{dm} _ \ text {mw，halo} $ $ \ text {dm} _ \ text {frb} $。我们对这些分布进行建模，校正银河系插图介质，并具有内核密度估计---非常适合小型数据制度---以找到校正后的$ \ text {dm} _ \ text {pulsar} $/$/$/$ \ text {dm} $ \ text {dm} _ \ text {dm} _ \ frb text {frb} $ {frb} $： $ \ max [\ text {dm} _ \ text {pulsar}] \大约7 \ pm2 \ pm2 \ text {（stat）} \ pm 9 \ pm 9 \ text {（sys）pc cm}^{ - 3} $ and $ \ min and $ \ min [\ min [\ text {dm} _ \ text {dm} _ \ text {dm} _ \ frb}} \ text {（stat）} \ pm 9 \ text {（sys）pc cm}^{ - 3} $。使用Bootstrap重新采样来估计不确定性，我们将保守的限制设置在银河系光散量度$ -2 <\ text {dm} _ \ text {mw，halo} <123 \ 123 \ text {pc cm}^{pc cm}^{-3} $（95 \％c.l.）中。上限特别保守，因为它可能包括FRB宿主星系的不可忽略的贡献以及宇宙网络的非零贡献。它强烈地不散发模型，其中银河系保留了大部分重子，密度曲线跟踪了假定的暗物质密度剖面。最后，我们对较大的FRB样品进行蒙特卡洛模拟，以验证我们的技术并评估正在进行的和将来的调查的敏感性。我们恢复了几个TENS $ \ text {pc cm}^{ - 3} $的界限，这可能足以测试Galaxy是否保留了其大部分的Baryonic质量。我们估计，几千个FRB的样本将大大收紧$ \ text {dm} _ \ text {mw，halo} $的约束，并为其他分析提供了有价值的补充。
We introduce a new technique to constrain the line-of-sight integrated electron density of our Galactic halo $\text{DM}_\text{MW,halo}$ through analysis of the observed dispersion measure distributions of pulsars $\text{DM}_\text{pulsar}$ and fast radio bursts $\text{DM}_\text{FRB}$. We model these distributions, correcting for the Galactic interstellar medium, with kernel density estimation---well-suited to the small data regime---to find lower/upper bounds to the corrected $\text{DM}_\text{pulsar}$/$\text{DM}_\text{FRB}$ distributions: $\max[\text{DM}_\text{pulsar}] \approx 7\pm2 \text{ (stat)} \pm 9 \text{ (sys) pc cm}^{-3}$ and $\min[\text{DM}_\text{FRB}] \approx 63^{+27}_{-21} \text{ (stat)} \pm 9 \text{ (sys) pc cm}^{-3}$. Using bootstrap resampling to estimate uncertainties, we set conservative limits on the Galactic halo dispersion measure $-2 < \text{DM}_\text{MW,halo} < 123 \text{pc cm}^{-3}$ (95\% c.l.). The upper limit is especially conservative because it may include a non-negligible contribution from the FRB host galaxies and a non-zero contribution from the cosmic web. It strongly disfavors models where the Galaxy has retained the majority of its baryons with a density profile tracking the presumed dark matter density profile. Last, we perform Monte Carlo simulations of larger FRB samples to validate our technique and assess the sensitivity of ongoing and future surveys. We recover bounds of several tens $\text{pc cm}^{-3}$ which may be sufficient to test whether the Galaxy has retained a majority of its baryonic mass. We estimate that a sample of several thousand FRBs will significantly tighten constraints on $\text{DM}_\text{MW,halo}$ and offer a valuable complement to other analyses.
