The Dynamical Echoes Of Dark Matter Sub-Structure: In Simulations & In Spirals Out To z ~ 0.1

暗物质子结构的动态回声：模拟

• 批准号: 1517488
• 负责人: Sukanya Chakrabarti
• 金额: $ 32.51万
• 依托单位: Rochester Institute of Tech
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2015
• 资助国家: 美国
• 起止时间: 2015-08-01 至 2019-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1517488&HistoricalAwards=false
• 关键词: Dynamical; Echoes; Dark; Matter; Sub

The current cosmological paradigm includes two significant and unknown physical entities called "dark matter" and "dark energy," which are used to model the Universe as we know it. Understanding the distribution of dark matter remains one of the most fundamental problems in astronomy and is the focus of this project. There are many discrepancies between dark matter sub-structure in the existing computer simulations and in observations. There are too few massive satellites relative to simulations, and at low Galactic latitudes there are hardly any Milky Way satellites. This project aims to extract essential information on the dark matter distribution in spiral galaxies by building on the investigator's ongoing work in characterizing galactic satellites from analysis of disturbances in extended disks of hydrogen gas.Communicating scientific results to a broad audience and promoting diversity benefits the astronomy community and our society at large. This project will be carried out at Rochester Institute of Technology (RIT), which has historically been primarily an undergraduate institution:(1) Women in Science: The PI will organize regular meetings with visiting women colloquium speakers, with the goal of gathering advice on professional development. Dr. Chakrabarti will also continue participating in the Expanding Your Horizons program, which is geared towards engaging middle school girls in science.(2) Computational Bootcamp: Every summer, the PI will provide a two-week, intensive computational bootcamp geared towards entering graduate students. The goal of this bootcamp is to serve as a bridge---providing an introduction to computational astrophysics, with hands-on lectures that illustrate the basics of computing and applications to astronomy. The PI will work through simple examples in IDL and Python, and she will encourage women and minority students to attend the bootcamp, and assign mentors for entering students.(3) Visualization Laboratory: The PI will continue producing 3-D animations of galaxy collisions, which will be showcased in the Viz-Lab at RIT. Three-D movies are becoming an increasingly popular tool to engage the public and are effective in widely disseminating research on galaxy evolution.The PI will carry out the following technical tasks:(1) The Milky Way: By matching simulated orbits of the Milky Way satellites with HST proper motions and tidal debris, the PI will derive constraints on the orbital parameters, as well as the initial stellar (and dark matter) distribution of the Milky Way satellites. The PI will produce models that are consistent with both the HI and stellar data of our galaxy, which displays large ripples in the outskirts, a prominent warp, and vertical waves in the galactic disk.(2) Probing The Dark Matter Halo: Dark matter halos evolve as a function of time, and they may have complex shapes. The PI will determine if the inference of the halo potential from stellar streams is viable for time-varying potentials. By deconstructing the hydrodynamical cosmological simulation ERIS, the PI will study if the distribution of satellites and the morphology of the gas and stellar disk is representative of the Milky Way or local spirals.(3) Shaking and Rattling The Local Spirals: By simulating a wide range of encounters with sub-halos from cosmological simulations, and mapping to multiple observational constraints in a statistically robust manner using a Monte Carlo Markov Chain analysis, the PI will produce realistic mock catalogs and evolutionary histories of HI disks and their satellite populations.(4) Strong Spiral Lenses in HI: As the SWELLS sample is a sufficiently low redshift sample of strong spiral lenses (z_avg ~ 0.1) showing visible signs of interaction, the PI will compare and contrast the team's HI analysis and gravitational lensing to derive two independent constraints on the dark matter distribution.

当前的宇宙学范式包括两个称为“暗物质”和“暗能量”的重要和未知的物理实体，这些实体用于对我们所知的宇宙进行建模。 了解暗物质的分布仍然是天文学中最根本的问题之一，并且是该项目的重点。 现有计算机模拟中的暗物质子结构和观察结果之间存在许多差异。 相对于模拟而言，大型卫星的数量太少，在低银河纬度下，几乎没有任何银河系卫星。 该项目旨在通过基于研究者正在进行的工作来提取螺旋星系中暗物质分布的基本信息，以通过分析氢气扩展磁盘的分析来表征银河卫星。向广泛的受众群体进行科学成果，并促进多样性有益于天文学社区和我们社会。 该项目将在罗切斯特理工学院（RIT）进行，该研究所历史上主要是一家本科机构：（1）科学妇女：PI将与访问的女性座谈会演讲者定期开会，目的是收集有关专业发展的建议。 Chakrabarti博士还将继续参加扩大的视野计划，该计划旨在吸引中学女生参与科学。（2）计算训练营：每年夏天，PI将为两周，密集的计算训练营提供，旨在用于入学研究生。该训练营的目的是用作桥梁 - 提供计算天体物理学的介绍，并进行动手讲座，以说明计算和应用天文学的基础知识。 PI将通过IDL和Python的简单示例进行工作，她将鼓励妇女和少数族裔学生参加训练营，并为入学学生分配导师。（3）可视化实验室：PI将继续制作3D动画的银河碰撞动画，这将在RIT的Viz-Lab中展示。三维电影正在成为越来越受欢迎的公众参与的工具，并有效地广泛传播了有关银河系进化的研究。PI将执行以下技术任务：（1）银河系：通过匹配银河系卫星的模拟轨道，与HST适当的动作和Tidal Debris相匹配，PI将构成限制，并限制了限制的启发。卫星。 PI将产生与我们银河系的HI和恒星数据一致的模型，该模型显示出郊区的大涟漪，突出的扭曲和银河磁盘中的垂直波。（2）探索暗物质光环：暗物质晕作为时间的功能，它们可能具有复杂的形状。 PI将确定从恒星流的晕球电位的推断对于随时间变化的电位可行。 通过解构流体动力学宇宙学模拟ERIS，PI将研究卫星的分布以及气体和恒星磁盘的形态是否代表银河系或当地螺旋形。（3）摇动当地螺旋螺旋出现：通过与统计的统计型号相吻合，通过统计型号进行统一的范围，并通过统计量进行统计，并使用统计量的型号，并使用统计量的型号，并在统计上进行单独的途径。 Carlo Markov链分析，PI将产生逼真的模拟目录和HI磁盘及其卫星种群的进化历史。（4）HI：HI：HI：的强螺旋镜头的强螺旋镜头是一个足够低的红移样本的强烈的螺旋透镜（Z_AVG〜0.1），与PI的互动相结合，并将其分析，与次数的分析相结合，并将其分析，并将其分析。暗物质分布。