Yu Feng, Rupert A. C. Croft, Tiziana Di Matteo, Nishikanta Khandai, Randy Sargent, Illah Nourbakhsh, Paul Dille, Chris Bartley, Volker Springel, Anirban Jana, Jeffrey Gardner
The increasing size of cosmological simulations has led to the need for new visualization techniques. We focus on Smoothed Particle Hydrodynamical (SPH) simulations run with the GADGET code and describe methods for visually accessing the entire simulation at full resolution. The simulation snapshots are rastered and processed on supercomputers into images that are ready to be accessed through a web interface (GigaPan). This allows any scientist with a web-browser to interactively explore simulation datasets in both in spatial and temporal dimensions, datasets which in their native format can be hundreds of terabytes in size or more. We present two examples, the first a static terapixel image of the MassiveBlack simulation, a P-GADGET SPH simulation with 65 billion particles, and the second an interactively zoomable animation of a different simulation with more than one thousand frames, each a gigapixel in size. Both are available for public access through the GigaPan web interface. We also make our imaging software publicly available.
A million-solar-mass object detected at cosmological distance using gravitational imaging
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡佩滕天文研究所）；South African Radio Astronomy Observatory（南非射电天文观测台）；Department of Physics, University of Pretoria（比勒陀利亚大学物理系）；Istituto di Radioastronomia, INAF（意大利国家天体物理研究所射电天文研究所）；Department of Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）
OpenUniverse2024: A shared, simulated view of the sky for the next generation of cosmological surveys
Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Duke University（杜克大学）；Argonne National Laboratory（阿贡国家实验室）；University of Texas, Dallas（德克萨斯大学达拉斯分校）；Northeastern University（东北大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；ETH Zurich（苏黎世联邦理工学院）；Ohio State University（俄亥俄州立大学）；Institute for Theoretical Physics, Utrecht University（乌得勒支大学理论物理研究所）；IPAC, California Institute of Technology（加州理工学院IPAC）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所）；University of Maryland, Baltimore County（马里兰大学巴尔的摩县分校）；NASA Goddard Space Flight Center（NASA戈达德太空飞行中心）；University of Pennsylvania（宾夕法尼亚大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理研究所）；NASA Jet Propulsion Laboratory（NASA喷气推进实验室）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；Carnegie Mellon University（卡内基梅隆大学）；Stanford University（斯坦福大学）；University of Pittsburgh（匹兹堡大学）；Department of Physics and Astronomy, Baylor University（贝勒大学物理与天文系）；Centro Brasileiro de Pesquisas Físicas（巴西物理研究中心）；Newcastle University（纽卡斯尔大学）；Caltech Optical Observatories, California Institute of Technology（加州理工学院卡尔光学观测站）
High resolution imaging and spectroscopy of the gravitational lens SDSSJ1206+4332: a natural coronagraph at $z=1.789$ and a standard ruler at $z=0.745$
我们目前的光谱和激光导星自适应光学（LGSAO）的双重成像透镜类星体SDSS J1206+4332的图像。我们将以前提出的偏导红移修正为$z_{d}=0.745,$，并首次测量了它的速度色散$σ=(290\pm30)$ km/s。LGSAO的数据显示，透镜类星体宿主星系在星状焦散面上伸展，从而形成了一对额外的合并图像，这在以前被认为是一个不相关的星系，因为数据有限。由于这种特殊的几何形状，透镜在类星体的宽线区起着天然日冕的作用，因此在折叠弧中只发现窄的[O III]发射。我们使用的数据来重建源结构和偏转潜力，包括附近的扰动。我们重建的点扩散函数（PSF）从类星体图像本身，因为没有额外的点源是目前在该领域的看法。从引力透镜和恒星动力学，我们发现的总质量密度剖面的斜率是$γ^{\prime}=-\logρ/\log r =1.93\pm0.09.$我们讨论的潜力SDSS J1206+4332测量时间延迟距离（从而H $_0$和其他宇宙学参数），或作为一个标准的统治者，结合时间延迟由COSMOGRAIL合作出版。我们的结论是，该系统是非常有前途的宇宙学。然而，为了实现有竞争力的精度和准确度，需要PSF的独立表征。偏转器的空间解析运动学将进一步减少不确定性。两者都在现有观测设施的范围之内。
Signatures of Massive Black Hole Merger Host Galaxies from Cosmological Simulations II: Unique Stellar Kinematics in Integral Field Unit Spectroscopy
Bishop's University（主教大学）；California Institute of Technology（加州理工学院）；McGill Space Institute（麦吉尔空间研究所）；McGill University（麦吉尔大学）；University College Cork（科克大学学院）
