Supernova 2025wny: High-angular resolution Keck/NIRC2 observations and preliminary lens modeling
Institute for Astronomy, University of Hawai’i at Manoa（夏威夷大学马诺阿分校天体物理研究所）；Research Center for the Early Universe, Graduate School of Science, The University of Tokyo（东京大学理学研究科早期宇宙研究中心）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所（CSIC-UC））；INAF – IASF Milano（意大利国家天体物理研究所米兰天文台分部）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Department of Physics & Astronomy, University of San Francisco（旧金山大学物理与天文系）；Physics Division, Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室物理部）；Institute for Astronomy, University of Hawai’i（夏威夷大学天体物理研究所）；Institute of Astronomy and Kavli Institute for（天体物理研究所及卡弗里）
Christopher J. Storfer, Kenneth C. Wong, Ana Acebron, Claudio Grillo, Willem B. Hoogendam, Xiaosheng Huang, David O. Jones, Eugene A. Magnier, Kaisey S. Mandel,… 展开作者
Christopher J. Storfer, Kenneth C. Wong, Ana Acebron, Claudio Grillo, Willem B. Hoogendam, Xiaosheng Huang, David O. Jones, Eugene A. Magnier, Kaisey S. Mandel, Nicolas Ratier-Werbin, David Rubin, Benjamin J. Shappee, Oscar Soler-Perez
Multiply imaged, gravitationally lensed supernovae are rare but powerful tools for providing independent measurements on cosmological parameters. Supernova (SN) 2025wny ("SN Winny") is the first gravitationally-lensed Type I superluminous supernova and the first lensed supernova in a galaxy-scale system that is suitable for time-delay cosmography studies. In this work, we present high-resolution $K_p$-band adaptive optics imaging of SN Winny obtained with the near-infrared camera (NIRC2) on the W. M. Keck II telescope. With exquisite image quality (FWHM$\approx0.^{\prime\prime}065$) we determine and make use of the precise astrometric positions of the five multiple images as constraints for our lens mass models. With lenstronomy and Glee, we parameterize the total mass of the system with a singular isothermal ellipsoid, a singular isothermal sphere, and external shear. The two independent models are in excellent agreement and reproduce the observed image positions with sub-milli-arcsecond residuals. The inferred projected total masses enclosed within the Einstein radii of the primary and secondary lens galaxies are M$_1$ = 4.44$^{+0.06}_{-0.05}\times10^{11} M_\odot$ and M$_2$ = 0.96$^{+0.02}_{-0.02}\times10^{11} M_\odot$, respectively. Likewise, the inferred effective velocity dispersion of the primary lens is $σ_{1} = $ 277.4$^{+0.9}_{-0.7}$ km/s, consistent with the independent spectroscopic measurement made by DESI of $σ_{\star,1} = $ 298$\,\pm\,37$ km/s. Our modeling results are also consistent with previous results for the same system with data from the Large Binocular Telescope (LBT), using the same lens modeling codes. We also corroborate their finding that the SN multiple image A has an anomalous excess of flux by a factor of ~2-3 beyond what our smooth mass models predict.
DESI Strong Lens Foundry III: Keck Spectroscopy for Strong Lenses Discovered Using Residual Neural Networks
University of Chicago（芝加哥大学）；University of California, Berkeley（加州大学伯克利分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of San Francisco（旧金山大学）；University of Hawai’i（夏威夷大学）；University of Pittsburgh（匹兹堡大学）
A Glimpse of the Stellar Populations and Elemental Abundances of Gravitationally Lensed, Quiescent Galaxies at $z\gtrsim 1$ with Keck Deep Spectroscopy
MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Laboratory for Exoplanets and Stellar Astrophysics, NASA/Goddard Space Flight Center（NASA戈达德太空飞行中心行星与恒星天体物理实验室）；Department of Astronomy, University of Maryland（马里兰大学天文学系）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/GSFC空间科学与技术研究探索中心）；School of Natural Sciences, University of Tasmania（塔斯马尼亚大学自然科学学院）；Institute of Natural and Mathematical Sciences, Massey University（梅西大学自然与数学科学研究所）；Department of Earth and Space Science, Graduate School of Science, Osaka University（大阪大学理学研究科地球宇宙学系）
GMP-selected dual and lensed AGNs: selection function and classification based on near-IR colors and resolved spectra from VLT/ERIS, KECK/OSIRIS, and LBT/LUCI
Discovery and first models of the quadruply lensed quasar SDSS J1433+6007
我们报告发现的四倍透镜类星体J1433+6007，在SDSS DR 12光度星表使用一种新的离群选择技术，没有事先光谱或紫外线过量的信息。在北欧光学望远镜（NOT，La Palma）获得的发现数据显示，在$z_s=2.74$上有几乎相同的类星体光谱，还有四张折叠配置的类星体图像，其中一张位于蓝色弧上。偏折器红移为$z_{l}=0.407,$。我们描述的选择程序，发现和后续行动，图像的位置和$BVRi$的大小，并从简单的镜头模型的第一个结果和预测。
The Detection of [O III]$λ$4363 in a Lensed, Dwarf Galaxy at $z$ = 2.59: Testing Metallicity Indicators and Scaling Relations at High Redshift and Low Mass
A Search For Stellar-mass Black Holes Via Astrometric Microlensing II: 2012-2015 Keck Candidates
University of California, Berkeley（加州大学伯克利分校）；Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Weizmann Institute of Science（魏茨曼科学研究所）；University of Chicago（芝加哥大学）
Characterizing Microlensing Planetary System OGLE-2014-BLG-0676L with High-Resolution Image Constrained Light Curve Modeling
The University of Osaka（大阪大学）；NASA/Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；University of Maryland（马里兰大学）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/GSFC空间科学与技术研究卓越中心）；Massey University（梅西大学）；University of Tasmania（塔斯马尼亚大学）；Sorbonne Université（索邦大学）；CNRS, Institut d’Astrophysique de Paris, IAP（法国国家科学研究中心巴黎天文台）
