This thesis presents a review of related important concepts in cosmology followed by details of the author's role in a research project on the origin of intracluster light. The author's role in the development of the simulations varied from searching parameters in the literature, through writing and modifying code in IDL, FORTRAN, and UNIX to carrying out hundreds of simulations using the particle-particle algorithm described in this thesis, as well as partaking in joint analysis of the simulation results. Part of this work in the isolated cluster simulations has been submitted for publication (Barai, Brito & Martel 2009). The main results of the simulations described in this thesis are: 1) destruction of dwarf galaxies by mergers dominates destruction by tides, and 2) destruction of galaxies by tides is sufficient to explain the observed intracluster light. These results support the accepted explanation for the origin of the intracluster light. In an ongoing, second stage of the simulation, which extends the isolated cluster results to a cosmologically significant region of the Universe, the author similarly assists in the implementation of a particle-particle/particle-mesh simulation and the joint analysis of the results to-date. The results are as per the Schechter luminosity function, and suggest the approach used is valid and the results obtained robust.
Simulations of the galaxy population constrained by observations from z=3 to the present day: implications for galactic winds and the fate of their ejecta
我们应用蒙特卡罗马尔可夫链（MCMC）方法的大规模模拟的星系形成在LambdaCDM宇宙学，以探讨如何恒星的形成和反馈所观察到的星系的光度和恒星质量函数的约束。我们在Millennium和Millennium-II模拟上联合建立模型，应用快速采样技术，允许在7<log（M*/Msun）<12和z=0至z=3的范围内观测到的星系丰度同时用作MCMC分析中的约束。当仅施加z=0的约束时，我们重现了Guo et al.（2012）先前建模的结果，但没有一组参数可以同时重现所有红移下观测到的星系丰度，这反映了低质量星系形成过早的事实，因此在该模型中，在高红移下过于丰富。这些数据要求星系风喷出物再吸积的效率随红移和晕质量的变化与以前的假设完全不同，但与最近一些星系形成的流体动力学模拟相似。我们提出了一个具体的模型，其中重新纳入时标与晕质量成反比，是独立的红移。这产生了一个不断发展的星系人口，适合观测到的丰度作为恒星质量，B-和K-波段光度的函数，同时在所有的红移。它还在其他两个领域产生了显着的改善，而这些领域是以前的模型所不具备的。它导致了今天的矮星系人口更年轻，更蓝，更强烈的恒星形成和更弱的小规模集群比以前，虽然暗矮星的被动部分仍然太高。
The dark fate of ultra-faint dwarfs: Gravothermal collapse in action
Donostia International Physics Center（多诺斯蒂亚国际物理中心）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学天文台物理学院）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
We present a pilot study on the origin and assembly history of the ICL for four galaxy clusters at 0.44<z<0.57 observed with the Hubble Space Telescope from the Cluster Lensing and Supernova Survey with Hubble (CLASH) sample. Using this sample of clusters we set an empirical limit on the amount of scatter in ICL surface brightness profiles of such clusters at z=0.5 and constrain the progenitor population and formation mechanism of the ICL by measuring the ICL surface brightness profile, the ICL color and color gradient, and the total ICL luminosity within 10<r<110 kpc. The observed scatter is …
Galaxy clusters are known to induce gas loss in infalling galaxies due to the ram pressure exerted by the intracluster medium over their gas content. In this paper, we investigate this process through a set of simulations of Milky Way like galaxies falling inside idealised clusters of 10$^{14}$ M$_\odot$ and 10$^{15}$ M$_\odot$, containing a cool-core or not, using the adaptive mesh refinement code RAMSES. We use these simulations to constrain how much of the initial mass contained in the gaseous disk of the galaxy will be converted into stars and how much of it will be lost, after a single cr…
We present deep Hubble Space Telescope imaging at the locations of four, potentially hostless, long-faded Type Ia supernovae (SNe Ia) in low-redshift, rich galaxy clusters that were identified in the Multi-Epoch Nearby Cluster Survey. Assuming a steep faint-end slope for the galaxy cluster luminosity function ($α_d=-1.5$), our data includes all but $\lesssim0.2\%$ percent of the stellar mass in cluster galaxies ($\lesssim0.005\%$ with $α_d=-1.0$), a factor of 10 better than our ground-based imaging. Two of the four SNe Ia still have no possible host galaxy associated with them ($M_R>-9.2$), co…
Intracluster globular clusters as tracers of the mass assembly of the Hydra I galaxy cluster
European Southern Observatory（欧洲南方天文台）；Universitätssternwarte der Ludwig-Maximilians Universität（路德维希-马克西米利安大学大学天文台）；INAF – Astronomical Observatory of Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；INAF – Astronomical Observatory of Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Gran Sasso Science Institute（格兰萨索科学研究所）
Intracluster Light as a Probe for Dark Matter: Exploring Self-interacting Dark Matter and Cold Dark Matter with C-EAGLE Sims
Korea Astronomy and Space Science Institute (KASI)（韩国天文学与空间科学研究所）；Quantum Universe Center, Korea Institute for Advanced Study（量子宇宙中心，韩国高等研究院）；School of Physics, The University of Sydney（悉尼大学物理学院）；ARC Centre of Excellence for Dark Matter Particle Physics（暗物质粒子物理卓越研究中心）；Departamento de Física Teórica, Facultad de Ciencias M-8, Universidad Autónoma de Madrid（马德里自治大学理学院M-8理论物理系）；Natural Science Research Institute (NSRI), University of Seoul（首尔大学自然科学研究所）；School of Physics, Korea Institute for Advanced Study（韩国高等研究院物理学院）；School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学院）；Center for Advanced Computation, Korea Institute for Advanced Study（韩国高等研究院先进计算中心）；University of Science and Technology (UST)（科学技术院）
