Finding quadruply imaged quasars with machine learning. I. Methods
A. Akhazhanov, A. More, A. Amini, C. Hazlett, T. Treu, S. Birrer, A. Shajib, P. Schechter, C. Lemon, B. Nord, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis… 展开作者
A. Akhazhanov, A. More, A. Amini, C. Hazlett, T. Treu, S. Birrer, A. Shajib, P. Schechter, C. Lemon, B. Nord, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, A. Choi, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, I. Ferrero, D. A. Finley, B. Flaugher, J. Frieman, J. García-Bellido, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, A. G. Kim, K. Kuehn, N. Kuropatkin, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, M. March, F. Menanteau, R. Miquel, R. Morgan, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, E. Sanchez, V. Scarpine, S. Serrano, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, T. N. Varga, J. Weller
Strongly lensed quadruply imaged quasars (quads) are extraordinary objects. They are very rare in the sky -- only a few tens are known to date -- and yet they provide unique information about a wide range of topics, including the expansion history and the composition of the Universe, the distribution of stars and dark matter in galaxies, the host galaxies of quasars, and the stellar initial mass function. Finding them in astronomical images is a classic "needle in a haystack" problem, as they are outnumbered by other (contaminant) sources by many orders of magnitude. To solve this problem, we develop state-of-the-art deep learning methods and train them on realistic simulated quads based on real images of galaxies taken from the Dark Energy Survey, with realistic source and deflector models, including the chromatic effects of microlensing. The performance of the best methods on a mixture of simulated and real objects is excellent, yielding area under the receiver operating curve in the range 0.86 to 0.89. Recall is close to 100% down to total magnitude i~21 indicating high completeness, while precision declines from 85% to 70% in the range i~17-21. The methods are extremely fast: training on 2 million samples takes 20 hours on a GPU machine, and 10^8 multi-band cutouts can be evaluated per GPU-hour. The speed and performance of the method pave the way to apply it to large samples of astronomical sources, bypassing the need for photometric pre-selection that is likely to be a major cause of incompleteness in current samples of known quads.
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。
HST imaging, pipeline modeling, and time-delay predictions of 2 triply-imaged and 15 quadruply-imaged lensed quasars
University of California, Los Angeles（加州大学洛杉矶分校）；STFC Hartree Centre（STFC哈特里中心）；Universidad Andres Bello（安德烈斯贝略大学）；Stony Brook University（石溪大学）；University of Chicago（芝加哥大学）；University of San Francisco（旧金山大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Staples High School（斯塔普尔斯高中）；Universidad de Valparaíso（瓦尔帕莱索大学）
JWST lensed quasar dark matter survey V: Hints of self-interacting dark matter from 29 quadruply imaged quasars
University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙学物理研究所）；University of California, Merced（加州大学默塞德分校）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）；Carnegie Observatories（卡内基观测站）；University of California, Los Angeles（加州大学洛杉矶分校）；University of California, Irvine（加州大学尔湾分校）；Universidad Andres Bello（安德烈斯贝略大学）；Millennium Institute of Astrophysics, Chile（智利天体物理千年研究所）；California Polytechnic State University（加州州立理工大学）
TDCOSMO: XX. WFI2033--4723, the First Quadruply-Imaged Quasar Modeled with JWST Imaging
Department of Physics and Astronomy, UCLA（加州大学洛杉矶分校物理与天文系）；Department of Physics and Astronomy, Stony Brook University（纽约州立大学石溪分校物理与天文系）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh（孟加拉国独立大学天文学、空间科学与天体物理中心）；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）；IPAC, California Institute of Technology（加州理工学院红外处理分析中心）；Space Telescope Science Institute（太空望远镜科学研究所）
Gaia GraL: Gaia DR2 Gravitational Lens Systems. III. A systematic blind search for new lensed systems
目标：在这项工作中，我们的目标是提供一个可靠的引力透镜（GL）候选人的基础上，在整个盖亚数据发布2（盖亚DR2）进行搜索。我们还表明，来自盖亚卫星的唯一天体测量和测光信息为监督学习方法提供了足够的见解，可以自动识别GL候选者，其效率与基于图像处理的方法相当。研究方法：我们模拟了106，623，188个由两个以上图像组成的透镜系统，基于在存在外部剪切的情况下表征非奇异等温椭球透镜模型的规则参数网格。这些模拟被用作训练和测试我们的监督学习模型的输入，该模型由极端随机树组成。后者最终用于为2，129，659个天体集群中的每个集群分配一个判别值，该判别值反映了我们的模拟与每个集群的观测相对位置和通量相匹配的能力。一旦补充了额外的约束条件，这些判别值允许我们从聚类列表中识别GL候选。结果如下：我们报告发现了15个新的四重成像透镜候选者，角间距小于6”，并通过恢复13个已知的四重成像系统中的12个来评估我们方法的性能，这些系统的所有组件都在Gaia DR 2中检测到，偶然的星团作为透镜系统的错误分类率低于1%。类似地，我们的方法关于四重成像系统的识别能力，其中在盖亚DR2中检测到三个图像，通过恢复13个已知的四重成像系统中的10个来评估，其中一个构成图像被丢弃。相关的误分类率在5.8%到20%之间变化，这取决于我们决定删除的图像。
TDCOSMO XXVIII. The Hubble constant from the quadruply lensed quasar J1537$-$3010 with precise time delays
University of Geneva（日内瓦大学）；Technical University of Munich（慕尼黑工业大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Laboratoire Univers et Particules de Montpellier (LUPM), CNRS & Université Montpellier（蒙彼利埃宇宙与粒子实验室（LUPM），法国国家科学研究中心与蒙彼利埃大学）；STAR Institute, University of Liège（列日大学STAR研究所）；Armagh Observatory and Planetarium（阿马天文台和天文馆）；Fermi National Accelerator Laboratory（费米国家加速器实验室）
CLASH: Discovery of a Bright z~6.2 Dwarf Galaxy Quadruply Lensed by MACS J0329.6-0211
We report the discovery of a z_{phot} =6.18^{+0.05}_{-0.07} (95% confidence level) dwarf galaxy, lensed into four images by the galaxy cluster MACS J0329.6-0211 ( z_{l} =0.45). The galaxy is observed as a high-redshift dropout in HST/ACS/WFC3 CLASH and Spitzer/IRAC imaging. Its redshift is securely determined due to a clear detection of the Lyman-break in the 18-band photometry, making this galaxy one of the highest-redshift multiply-lensed objects known to date with an observed magnitude of F125W=24.00 \pm 0.04 AB mag for its highest-magnified image. We also present the first strong-lensing a…
TDCOSMO XXVI: Uniform lens modeling of eight doubly imaged quasars
Stony Brook University（石溪大学）；University of Chicago（芝加哥大学）；Independent University, Bangladesh（孟加拉独立大学）；Stockholm University（斯德哥尔摩大学）；ETH Zurich（苏黎世联邦理工学院）；Université de Genève（日内瓦大学）；Universidad de Valparaíso（瓦尔帕莱索大学）；University of Liège（列日大学）；Universitat de Barcelona（巴塞罗那大学）；Institut Català de Recerca i Estudis Avançats (ICREA)（加泰罗尼亚高级研究所）；Institut dEstudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所）
Time-delay and lens galaxy redshift in the doubly imaged quasar PS J2305+3714
Ulugh Beg Astronomical Institute（乌鲁伯格天文研究所）；Universidad de Cantabria（坎塔布里亚大学）；O.Ya. Usikov Institute for Radiophysics and Electronics, National Academy of Sciences of Ukraine（乌克兰国家科学院 O.Ya. 乌西科夫无线电物理与电子研究所）；Institute of Astronomy, Kharkiv V.N. Karazin National University（哈尔科夫 V.N. 卡拉津国立大学天文学研究所）；Observatoire de la Côte d’Azur（蔚蓝海岸天文台）；Institute of Radio Astronomy, National Academy of Sciences of Ukraine（乌克兰国家科学院无线电物理研究所）；Chirchik State Pedagogical University（奇尔奇克国立师范学院）；National University of Uzbekistan（乌兹别克斯坦国立大学）；ICC-UB Institut de Ciéncies del Cosmos, University of Barcelona（巴塞罗那宇宙科学研究所 (ICCUB)）
TDCOSMO XXX: Spatially resolved kinematics of the deflectors in time-delay lens systems B1608+656 and SDSSJ1206+4332 from JWST-NIRSpec observation
University of California, Los Angeles（加州大学洛杉矶分校）；University of Chicago（芝加哥大学）；Independent University, Bangladesh（孟加拉独立大学）；University of Oxford（牛津大学）；Technical University of Munich（慕尼黑工业大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
