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arXiv 2607.01005astro-ph.CO
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强引力透镜层析成像：双源面和伪多源面强引力透镜约束暗能量

Strong Lensing Tomography: Double and pseudo multi-source plane strong gravitational lensing to constrain dark energy

Stony Brook University（石溪大学）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Universidad Andres Bello（安德斯贝洛大学）；Oxford University（牛津大学）；University of Portsmouth（朴茨茅斯大学）
Paras Sharma, Simon Birrer, Narayan Khadka, Timo Anguita, Adam Bolton, Sydney Erickson, Phil Holloway, Tian Li, Phil Marshall, Dieu D. Nguyen, Graham P. Smith, … 展开作者

Paras Sharma, Simon Birrer, Narayan Khadka, Timo Anguita, Adam Bolton, Sydney Erickson, Phil Holloway, Tian Li, Phil Marshall, Dieu D. Nguyen, Graham P. Smith, Crescenzo Tortora, Bryce Wedig, the Strong Lensing Science Collaboration, the LSST Dark Energy Science Collaboration

备注：
44 pages, 12 figures, submitted to JCAP
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AI总结：

提出伪双源面透镜（PDSPL）方法，利用大量星系-星系透镜对克服质量片简并，结合层次化预测框架，在Flat w0waCDM模型下将暗能量状态方程参数w0约束至σ(w0)~0.29。

摘要：

具有不同透镜和源红移分布的引力透镜层析测量包含宇宙相对膨胀速率的关键信息，从而约束暗能量。虽然该技术在弱透镜中已成熟，其在强透镜中的应用传统上集中于双源面透镜（DSPL）。然而，DSPL极为罕见且根本上受质量片简并（MSD）限制，这一系统不确定性在以往文献中未充分探索。为克服这些挑战，我们引入伪双源面透镜（PDSPL）：具有自相似偏转体的独立单源面透镜对。这将DSPL形式推广到来自即将开展的巡天（如LSST、Euclid和Roman）预期的约10^5个星系-星系透镜。与真实DSPL不同，PDSPL通过构造避免了中间源质量问题，消除了相关的次级MSD和多平面射线追踪需求。我们将偏转星系的MSD纳入层次化预测框架，证明该简并严重降低小DSPL样本的约束能力，从而激励我们的PDSPL统计方法。我们在Flat w0waCDM宇宙学下预测对暗能量状态方程的约束。仅LSST 10年测光样本即可实现σ(w0)~0.45，同时将MSD参数和偏转体幂律斜率约束至约2%。添加Ωm上的先验N(0.3,0.05)——模拟与CMB、BAO或SNe Ia等外部探针结合——可将此收紧至σ(w0)~0.29，与当前Stage III弱透镜分析相竞争。值得注意的是，这一大规模测光样本优于具有精确光谱后续观测（例如来自4MOST）的较小子集，证实统计数量主导每对精度。

英文摘要：

Tomographic measurements of gravitational lensing with different lens and source redshift distributions contain crucial information about the universe's relative expansion rate, and hence dark energy. While this technique is well-established in weak lensing, its application to strong lensing has traditionally focused on Double Source Plane Lenses (DSPLs). However, DSPLs are exceedingly rare and fundamentally limited by the Mass-Sheet Degeneracy (MSD), a systematic uncertainty underexplored in previous literature. To overcome these challenges, we introduce Pseudo Double-Source Plane Lenses (PDSPLs): pairs of independent single-source plane lenses with self-similar deflectors. This generalizes the DSPL formalism to the $\sim 10^5$ galaxy-galaxy lenses expected from LSST, Euclid, and Roman. Unlike true DSPLs, PDSPLs are free from the intermediate source mass problem by construction, eliminating the associated secondary MSD and the need for multi-plane ray tracing. We incorporate the deflector MSD into a hierarchical population model to forecast dark energy constraints in Flat $w_0w_a$CDM, showing that MSD severely degrades constraints from small DSPL samples and motivates our PDSPL statistical approach. Assuming unbiased Gaussian photo-z errors of $σ_z/(1+z)=0.03$, the mock LSST Y10 photometric sample yields $σ(w_0)\sim0.45$, constraining the population-mean MSD parameter and deflector power-law slope to $\sim2\%$. A prior $Ω_m\sim\mathcal{N}(0.3,0.05)$, representing combination with external cosmological probes such as CMB, BAO, or SNe Ia, improves this to $σ(w_0)\sim0.29$, comparable to Stage III weak lensing. The statistical advantage over smaller spectroscopic subsets (e.g., 4MOST) assumes unbiased photo-zs. Real-data use requires spectroscopic photo-z calibration and validation of how paired deflectors' mass-profile differences affect Einstein-radius ratios.

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