Scholarlink

<p>The strongly lensed gravitational wave (SLGW) is a promising transient phenomenon. However, the long-wave nature of gravitational waves poses a considerable challenge in the identification of its host galaxy. Here, to tackle this challenge, we propose a method triggered by the wave optics effect of microlensing. The microlensing interference introduces frequency-dependent fluctuations in the waveform. Our method consists of three steps. First, we reconstruct the waveforms by using template-independent and template-dependent methods. The mismatch of two reconstructions serves as an indicator of SLGWs. This step can identify approximately 10% SLGWs. Second, we pair the multiple images of the SLGWs by using sky localization overlapping. Because we have preidentified at least one image through microlensing, the false-alarm probability for pairing SLGWs is significantly reduced. Third, we search the host galaxy by requiring the consistency of time delays between galaxy–galaxy lensing and SLGW. By combing the stage-IV galaxy survey and the third-generation gravitational wave detectors, we expect to find, on average, one quadruple-image system per 3 years. This method can substantially facilitate the pursuit of time-delay cosmography, discovery of compact objects and multimessenger astronomy.</p>

错误：搜索内容不能为空，请输入英文关键词
错误：关键词超出字数限制，请精简
高级检索

An interference-based method for the detection of strongly lensed gravitational waves

  • 期刊论文

  • 出版模式：

    开放获取

  • 发表日期：

    2025年3月31日

查看全文
  • Xikai Shan,
  • Bin Hu,
  • Xuechun Chen,
  • Rong-Gen Cai

摘要

The strongly lensed gravitational wave (SLGW) is a promising transient phenomenon. However, the long-wave nature of gravitational waves poses a considerable challenge in the identification of its host galaxy. Here, to tackle this challenge, we propose a method triggered by the wave optics effect of microlensing. The microlensing interference introduces frequency-dependent fluctuations in the waveform. Our method consists of three steps. First, we reconstruct the waveforms by using template-independent and template-dependent methods. The mismatch of two reconstructions serves as an indicator of SLGWs. This step can identify approximately 10% SLGWs. Second, we pair the multiple images of the SLGWs by using sky localization overlapping. Because we have preidentified at least one image through microlensing, the false-alarm probability for pairing SLGWs is significantly reduced. Third, we search the host galaxy by requiring the consistency of time delays between galaxy–galaxy lensing and SLGW. By combing the stage-IV galaxy survey and the third-generation gravitational wave detectors, we expect to find, on average, one quadruple-image system per 3 years. This method can substantially facilitate the pursuit of time-delay cosmography, discovery of compact objects and multimessenger astronomy.