AI 中文总结
本研究对红移z=2.015的强引力透镜超亮超新星SN 2025wny进行透镜建模，结合空间成像、时间延迟等数据约束哈勃常数，为宇宙学研究提供了重要观测依据。
AI 中文摘要
我们对红移z=2.015的I型强引力透镜超亮超新星SN 2025wny开展了透镜与宇宙学分析，该超新星被两个红移z=0.376的前景星系多重成像。利用哈勃空间望远镜与詹姆斯·韦布空间望远镜获取的成像数据，我们采用两个椭圆幂律质量分布与一个外部剪切分量对该透镜系统进行建模。除超新星的像位置外，建模还纳入了被透镜的宿主星系的面亮度分布。所有滤镜下推导得到的爱因斯坦半径大致一致，θ_E,1≈1.6角秒，θ_E,2≈0.7-0.8角秒。在考虑透镜星系中恒星的微引力透镜效应后，后验分布给出总放大率约为μ_tot~5-50，多重像的流量比与观测结果一致。将透镜模型与通过光谱和测光测量得到的时间延迟相结合，对于采用等温质量剖面的基准模型，我们得到滤镜边缘化约束下的哈勃常数H₀=66.7⁺⁷.⁶₋₆.₃ km·s⁻¹·Mpc⁻¹；若允许透镜星系的密度斜率在宽范围内变化，则H₀=70.8⁺⁸.²₋₆.₁ km·s⁻¹·Mpc⁻¹。这些值依赖于所采用的透镜质量分布参数化、密度斜率的先验假设以及周围大尺度环境可能带来的额外透镜贡献。我们发现，纳入当前可用的恒星运动学测量对H₀的推导值仅产生微弱影响。未来对透镜星系运动学的测量以及透镜环境的详细表征，将进一步提升SN 2025wny作为宇宙学探针的效用。
英文摘要
We present a lensing and cosmographic analysis of the strongly lensed Type I superluminous supernova SN 2025wny at redshift $z=2.015$, multiply imaged by two foreground galaxies at $z=0.376$. Using imaging obtained with the Hubble Space Telescope and the James Webb Space Telescope, we model the lens system with two elliptical power-law mass distributions and an external shear component. In addition to the supernova image positions, the modelling incorporates the surface-brightness distribution of the lensed host galaxy. The inferred Einstein radii are $θ_{\rm E,1}\simeq 1.6$" and $θ_{\rm E,2}\simeq 0.7$ - $0.8$", with broadly consistent results across all filters. After accounting for microlensing by stars in the lens galaxies, the posterior distribution spans total magnifications of approximately $μ_{\rm tot}\sim 5$--$50$, with flux ratios of the multiple images consistent with observations. Combining the lens models with spectroscopically and photomerically measured time delays yields a filter-marginalized constraint of \[ H_0 = 66.7^{+7.6}_{-6.3}\; {\rm km\,s^{-1}\,Mpc^{-1}}, \] for a fiducial model with isothermal mass profiles. Allowing the density slopes of the lens galaxies to vary over a broad range results in \[ H_0 = 70.8^{+8.2}_{-6.1}\; {\rm km\,s^{-1}\,Mpc^{-1}}. \] These values are conditional on the adopted parameterization of the lens mass distribution, the assumed priors on the density slopes, and possible additional lensing contributions from the surrounding large-scale environment. We find that incorporating the currently available stellar kinematic measurements has only a modest effect on the inferred value of $H_0$. Future measurements of the lens-galaxy kinematics and a detailed characterization of the lens environment will further strengthen the utility of SN 2025wny as a cosmological probe.
CommentsSubmitted to the ApJ Focus Issue on SN 2025wny (Paper V)
