Hawaii Supernova Flows

30年前，对宇宙微波背景辐射的观测发现，一个方向的温度比相反方向的温度略高。公认的解释是，辐射是由我们的银河系及其同伴的630公里/秒的运动多普勒频移。30年来，天文学家一直在寻找导致这种极端运动的引力源。在十亿光年的尺度上一定有吸引子。唯一已知的研究如此大尺度运动的方法是基于一类超新星的明确定义的光度。在三年的时间里，我们的计划将监测数千颗这样的超新星，确定它们的距离，并首次绘制星系运动对十亿光年距离的物质分布的响应。这项研究是探索暗物质本质的一部分，暗物质是物质的神秘主要成分。如果不了解暗物质，我们就无法理解宇宙的发展。这个问题是当前物理学和宇宙学研究工作的核心，最终也是理解宇宙和我们起源的社会兴趣的核心。 通过视频、交互式模型和虚拟现实，公众可以获得这些知识。 所描述的工作实现了一个特定的共鸣与外行观众和这个计划是致力于公共宣传。在夏威夷大学，存在的手段，以确定一个大样本的超新星在z= 0. 1，并获得必要的补充信息，以确定准确的距离。在探测附近超新星和记录其光变曲线方面，ATLAS和ASSAS-SN是两个节奏最好的设施。每晚都会发现六个新的SNIa事件。这些事件必须在大量其他瞬变中识别出来。夏威夷大学的2.24米望远镜将被用来获得光谱，以证明超新星的类型并给出红移。位于Maunakea的3.8米UKIRT用于获取近红外的光曲线信息，其中SNIa的标准烛光性质得到了最好的定义。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

Thirty years ago, observations of the cosmic microwave background was found to be slightly hotter in one direction than in the opposite direction. The accepted explanation was that the radiation is doppler shifted by the motion of our Milky Way Galaxy and its companions of 630 km/s. For 30 years, astronomers have sought the sources of attraction that would cause this extreme motion. There must be attractors on scales of a billion light years. The only known methodology to study motions on such large scales is based on the well-defined luminosities of a class of supernovae. Over three years, our program will monitor thousands of such supernovae, determine their distances and, for the first time, map the motions of galaxies in response to the distribution of matter to a distance of a billion light years. This research is part of a quest to understand the nature of dark matter, the mysterious dominant constituent of matter. We cannot comprehend the development of the universe without an understanding of dark matter. This problem is central to current research efforts in physics and cosmology and, ultimately, to societal interest in understanding the universe and our origins. Through videos, interactive models, and virtual reality this knowledge can be made accessible to the public. The work that is described achieves a particular resonance with lay audiences and this program is committed to public outreach.At the University of Hawaii, the means exist to identify a large sample of supernovae within z=0.1 and obtain the requisite supplementary information to determine accurate distances. The two facilities with the best cadences for detecting nearby supernovae and documenting their light curves are ATLAS and ASSAS-SN. A half dozen new SNIa events will be discovered every night. These events must be identified among the large number of other transients. The University of Hawaii 2.24m telescope will be employed to obtain spectra to certify the supernova type and to give a redshift. The 3.8m UKIRT on Maunakea is used to acquire light curve information in the near infrared where the standard candle nature of SNIa is best defined.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.