Euclid: The Early Release Observations Lens Search Experiment
J. A. Acevedo Barroso, C. M. O'Riordan, B. Clément, C. Tortora, T. E. Collett, F. Courbin, R. Gavazzi, R. B. Metcalf, V. Busillo, I. T. Andika, R. Cabanac, H. M… 展开作者
J. A. Acevedo Barroso, C. M. O'Riordan, B. Clément, C. Tortora, T. E. Collett, F. Courbin, R. Gavazzi, R. B. Metcalf, V. Busillo, I. T. Andika, R. Cabanac, H. M. Courtois, J. Crook-Mansour, L. Delchambre, G. Despali, L. R. Ecker, A. Franco, P. Holloway, N. Jackson, K. Jahnke, G. Mahler, L. Marchetti, P. Matavulj, A. Melo, M. Meneghetti, L. A. Moustakas, O. Müller, A. A. Nucita, A. Paulino-Afonso, J. Pearson, K. Rojas, C. Scarlata, S. Schuldt, S. Serjeant, D. Sluse, S. H. Suyu, M. Vaccari, A. Verma, G. Vernardos, M. Walmsley, H. Bouy, G. L. Walth, D. M. Powell, M. Bolzonella, J. -C. Cuillandre, M. Kluge, T. Saifollahi, M. Schirmer, C. Stone, A. Acebron, L. Bazzanini, A. Díaz-Sánchez, N. B. Hogg, L. V. E. Koopmans, S. Kruk, L. Leuzzi, A. Manjón-García, F. Mannucci, B. C. Nagam, R. Pearce-Casey, L. Scharré, J. Wilde, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, A. Basset, P. Battaglia, R. Bender, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, A. Caillat, S. Camera, G. P. Candini, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, L. Corcione, M. Cropper, A. Da Silva, H. Degaudenzi, G. De Lucia, J. Dinis, F. Dubath, X. Dupac, S. Dusini, M. Farina, S. Farrens, S. Ferriol, M. Frailis, E. Franceschi, S. Galeotta, B. Garilli, K. George, W. Gillard, B. Gillis, C. Giocoli, P. Gómez-Alvarez, A. Grazian, F. Grupp, L. Guzzo, S. V. H. Haugan, H. Hoekstra, W. Holmes, I. Hook, F. Hormuth, A. Hornstrup, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kunz, H. Kurki-Suonio, D. Le Mignant, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, E. Maiorano, O. Mansutti, S. Marcin, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R. Massey, E. Medinaceli, M. Melchior, Y. Mellier, E. Merlin, G. Meylan, M. Moresco, L. Moscardini, E. Munari, R. Nakajima, C. Neissner, R. C. Nichol, S. -M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, R. Saglia, Z. Sakr, A. G. Sánchez, D. Sapone, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, J. Skottfelt, L. Stanco, J. Steinwagner, P. Tallada-Crespí, D. Tavagnacco, A. N. Taylor, I. Tereno, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. A. Valentijn, L. Valenziano, T. Vassallo, Y. Wang, J. Weller, E. Zucca, C. Burigana, V. Scottez, M. Viel, D. Scott, S. Vegetti
We investigated the ability of the Euclid telescope to detect galaxy-scale gravitational lenses. To do so, we performed a systematic visual inspection of the $0.7\,\rm{deg}^2$ Euclid Early Release Observations data towards the Perseus cluster using both the high-resolution $I_{\scriptscriptstyle\rm E}$ band and the lower-resolution $Y_{\scriptscriptstyle\rm E}$, $J_{\scriptscriptstyle\rm E}$, $H_{\scriptscriptstyle\rm E}$ bands. Each extended source brighter than magnitude 23 in $I_{\scriptscriptstyle\rm E}$ was inspected by 41 expert human classifiers. This amounts to $12\,086$ stamps of $10^{\prime\prime}\,\times\,10^{\prime\prime}$. We found $3$ grade A and $13$ grade B candidates. We assessed the validity of these $16$ candidates by modelling them and checking that they are consistent with a single source lensed by a plausible mass distribution. Five of the candidates pass this check, five others are rejected by the modelling, and six are inconclusive. Extrapolating from the five successfully modelled candidates, we infer that the full $14\,000\,{\rm deg}^2$ of the Euclid Wide Survey should contain $100\,000^{+70\,000}_{-30\,000}$ galaxy-galaxy lenses that are both discoverable through visual inspection and have valid lens models. This is consistent with theoretical forecasts of $170\,000$ discoverable galaxy-galaxy lenses in Euclid. Our five modelled lenses have Einstein radii in the range $0.\!\!^{\prime\prime}68\,<\,θ_\mathrm{E}\,<1.\!\!^{\prime\prime}24$, but their Einstein radius distribution is on the higher side when compared to theoretical forecasts. This suggests that our methodology is likely missing small-Einstein-radius systems. Whilst it is implausible to visually inspect the full Euclid dataset, our results corroborate the promise that Euclid will ultimately deliver a sample of around $10^5$ galaxy-scale lenses.
Synergies between SALT and Herschel, Euclid & the SKA: strong gravitational lensing & galaxy evolution
引力透镜在过去的几年里引起了人们极大的兴趣。由于创新的多波长选择，2000年已知的少数几个强透镜系统现在已经被数百个所取代，并且来自Herschel和其他亚毫米测量的数千个透镜的前景迫在眉睫。欧几里德和平方公里阵列承诺数万甚至数十万。引力透镜是极少数能够绘制暗物质晕分布的探测器之一。透镜还提供了独立的宇宙学参数估计，并使研究星系人口，否则太微弱的详细研究。SALT处于非常有利的位置，可以对Herschel、南极望远镜、Atacama宇宙学望远镜、Euclid和Square Kilometer Array等的前景透镜和背景源的后续观测产生巨大影响。本文回顾了高影响SALT科学的前景和星系演化的许多限制，可能导致。
Euclid: Quick Data Release (Q1) -- LensMC shear measurement catalogue for cluster lensing science
University of Edinburgh（爱丁堡大学）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚天文物理与空间科学研究所）；INFN-Sezione di Bologna（博洛尼亚意大利国家核物理研究所分部）；Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University（名古屋大学小林-益川粒子宇宙起源研究所）；Institute for Advanced Research, Nagoya University（名古屋大学高等研究院）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学嘉利弗宇宙物理学与数学研究所）；Université Paris Cité（巴黎西岱大学）；Université Paris-Saclay（巴黎萨克雷大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理学、信息学与物质研究所）；INAF-Osservatorio Astronomico di Padova（帕多瓦天文台）；Universität Innsbruck（因斯布鲁克大学）
Euclid Quick Data Release (Q1) The Strong Lensing Discovery Engine B -- Early strong lens candidates from visual inspection of high velocity dispersion galaxies
Gravitational Lenses in UNIONS and Euclid (GLUE) I: A Search for Strong Gravitational Lenses in UNIONS with Subaru, CFHT, and Pan-STARRS Data
University of Hawai‘i（夏威夷大学）；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 at Mānoa（夏威夷大学马诺阿分校）；University of California, Berkeley（加州大学伯克利分校）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理与宇宙微波背景研究所）；Laboratoire d’Astrophysique de Marseille（马赛天体物理学实验室）；Aix-Marseille Université（艾克斯-马赛大学）；CNES（法国国家空间研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理学研究所）；Sorbonne Université（索邦大学）；National Research Council Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究所）；University of Waterloo（滑铁卢大学）；Waterloo Centre for Astrophysics（滑铁卢天体物理学中心）；Perimeter Institute for Theoretical Physics（理论物理珀IMETER研究所）；University of Hawaii（夏威夷大学）；University of British Columbia（不列颠哥伦比亚大学）
Measuring the Stellar-to-Halo Mass Relation at $\sim10^{10}$ Solar masses, using forthcoming space-based imaging of galaxy-galaxy strong lenses
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）；Institute for Astrophysics, School of Physics, Zhengzhou University（郑州大学物理学院天体物理研究所）；School of Mathematics, Statistics and Physics, Newcastle University（纽卡斯尔大学数学、统计与物理学院）；Institute for Computational Cosmology, Department of Physics, Durham University（杜伦大学物理学院计算宇宙学研究所）
Galaxy Ellipticity Measurements in the Near-Infrared for Weak Lensing
我们调查的价值，近红外成像从即将到来的调查约束星系的椭圆。我们选择的星系之间的0.5 < z < 3比预期的欧几里德灵敏度限制从GOODS-S和N领域在CANDELS。共同添加的CANDELS/HST V+I和J+H图像的分辨率和灵敏度降低，以模拟欧几里得质量的光学和近红外（NIR）图像。然后我们对这些模拟图像运行GALFIT，发现光学和近红外在测量星系椭圆率方面提供了类似的性能，在红移0.5 < z < 3. At z >1.0时，近红外选择的源密度高出1.4倍，因此近红外推导的椭圆率的标准误差小了约30%，这意味着更精确的椭圆率测量。近红外光谱的良好性能主要是因为星系在近红外波段的光分布比光学波段的光分布更平滑，后者追踪的是星团的恒星形成区域。此外，NIR波段的每像素表面亮度比光学图像高，同时受灰尘衰减的影响较小。尽管欧几里德近红外光谱的空间采样和分辨率比光学差，但近红外光谱的方法可以产生等效或更精确的星系椭圆率测量。如果影响形状的系统学，如抖动策略和点扩散函数欠采样可以减轻，包括近红外光谱可以改善星系椭圆率测量所有的红移。这对于即将到来的弱透镜调查特别重要，例如Euclid和WFIRST。
The GLASS James Webb Space Telescope Early Release Science Program. I. Survey Design and Release Plans
GLASS James Webb空间望远镜早期释放科学（以下简称GLASS-JWST-ERS）计划将获得并公开提供ERS活动的最深河外数据。它主要是为了解决两个关键的科学问题，即“什么来源电离宇宙和什么时候？重子如何在星系中循环？“，同时也使各种各样的第一眼科学调查成为可能。在主模式下，它将获得由前景哈勃前沿场星系团Abell 2744透镜的星系的NIRISS和NIRSpec光谱。与此同时，它将使用NIRCam来观察两个偏离星团中心的视场，其中透镜放大率可以忽略不计，因此可以有效地将其视为空白视场。为了让社区做好准备，以获得这一前所未有的数据，我们描述了科学原理，调查设计（包括目标选择和观测设置），并提出了预期灵敏度的预调试估计。此外，我们还介绍了计划公开发布的高级别数据产品，供更广泛的天文学界使用。
Euclid: Quick Data Release (Q1) -- Watching ICM-selected galaxy clusters with Euclid eyes -- prospects of Euclid data in the context of large SZ and X-ray based surveys
