arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2304.01320astro-ph.GA
收藏

利用引力透镜类星体中的微透镜信号探测致密暗物质天体

Probing compact dark matter objects with microlensing in gravitationally lensed quasars

Petra Awad, James H. H. Chan, Martin Millon, Frederic Courbin, Eric Paic

阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

AI总结：

本研究基于COSMOGRAIL六个透镜类星体的微透镜光变曲线，提出Kolmogorov-Smirnov检验方法验证暗物质组成，发现现有数据不排斥恒星透镜标准模型，并预计Rubin天文台的900条曲线可区分恒星与原始黑洞致密暗物质情景。

摘要：

引力透镜类星体光变曲线中的微透镜信号可以揭示其透镜星系中暗物质（DM）的组成。在此，我们研究了来自最新且最佳的 COSMOGRAIL 观测的六个透镜类星体样本：HE 1104-1805、HE 0435-1223、RX J1131-1231、WFI 2033-4723、PG 1115+080 和 J1206+4332，结合独立的图像对，总共产生了八条微透镜光变曲线，通常跨越十年时间。我们探索微透镜信号，以确定对恒星族的标准假设是否足以解释测量信号的振幅。我们使用来自 H0LiCOW/TDCOSMO 合作项目迄今最详细的透镜模型来生成模拟微透镜光变曲线。最后，我们提出了一种基于 Kolmogorov-Smirnov 检验的方法，以验证我们数据中观测到的微透镜振幅是否与最标准情景相符，即星系由作为致密天体的恒星和平滑分布的 DM 组成。鉴于我们目前的样本，我们表明标准情景不能被拒绝，这与 Hawkins (2020a) 的先前结果形成对比，后者声称需要一群恒星质量的原始黑洞（PBHs）来解释透镜类星体光变曲线中微透镜信号的振幅。我们进一步估计了区分恒星微透镜的标准情景与描述星系中所有 DM 以致密天体（如 PBHs）形式存在（平均质量为 0.2M⊙）的情景所需的微透镜光变曲线数量。我们发现，来自 Rubin 天文台的约 900 条微透镜曲线将足以在 95% 置信水平上区分这两种极端情景。

英文摘要：

The microlensing signal in the light curves of gravitationally lensed quasars can shed light on the dark matter (DM) composition in their lensing galaxies. Here, we investigate a sample of six lensed quasars from the most recent and best COSMOGRAIL observations: HE~1104$-$1805, HE~0435$-$1223, RX~J1131$-$1231, WFI~2033$-$4723, PG~1115$+$080, and J1206$+$4332, yielding a total of eight microlensing light curves, when combining independent image pairs and typically spanning ten years. We explore the microlensing signals to determine whether the standard assumptions on the stellar populations are sufficient to account for the amplitudes of the measured signals. We use the most detailed lens models to date from the H0LiCOW/TDCOSMO collaboration to generate simulated microlensing light curves. Finally, we propose a methodology based on the Kolmogorov-Smirnov test to verify whether the observed microlensing amplitudes in our data are compatible with the most standard scenario, whereby galaxies are composed of stars as compact bodies and smoothly distributed DM. Given our current sample, we show that the standard scenario cannot be rejected, in contrast with previous results by Hawkins (2020a), claiming that a population of stellar mass primordial black holes (PBHs) is necessary to explain the amplitude of the microlensing signals in lensed quasar light curves. We further estimate the number of microlensing light curves needed to distinguish between the standard scenario with stellar microlensing and a scenario that describes all the DM contained in galaxies in the form of compact objects such as PBHs, with a mean mass of $0.2M_{\odot}$. We find that about 900 microlensing curves from the Rubin Observatory will be sufficient to discriminate between the two extreme scenarios at a 95\% confidence level.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑