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The Universe, on extra-galactic scales, is composed of a vast network of structures dubbed the "cosmic web". One of the most fundamental discoveries about the evolution of galaxies is that their properties have a dependence on their location relative to this cosmic web (i.e., their environment). However, detailed studies of the environmental dependence on galaxy evolution have been extremely challenging due to the inherent complexity of the structures on the largest scales, a plethora of techniques being used to try to map the cosmic web, and other confounding factors, such as the masses of galaxies, that also affect their evolution. In this work, we will present a technique for characterizing the environments of galaxies in the cosmic web, which is comprised of two separate, but complementary, methods that together provide a more complete measure of environment. After some introductory background in Chapter 1, we will demonstrate these mapping techniques on the Coma Supercluster, and present an analysis of the star-formation activity of about 4,000 galaxies in the supercluster environment in Chapter 2. Next, in Chapter 3 we present a greatly expanded application of our mapping techniques encompassing about 60,000 galaxies within 200 Mpc that addresses several outstanding questions from the Coma Supercluster study, and also leads to new intriguing insights into the evolution of galaxies as a function of environment. Then, in Chapter 4 we present a pilot study focusing on galaxy evolution as traced by the gas content around two galaxy clusters. We also expand upon this pilot study in Chapter 5, whereupon we examine more closely the resiliency of molecular gas content, compared to the atomic gas, to the effects of the cluster environment. And finally, in Chapter 6 we present some concluding remarks and explore some promising avenues for future study.
We study the effects of environment on the evolution of galaxies, with an emphasis on two different approaches towards the definition of environment: (1) environment defined based on the local surface density of galaxies and (2) environment defined based on the major components of the cosmic web; i.e., filaments, clusters and the field. In the first approach, surface density field is estimated using a variety of estimators and tested with simulations. Using the estimated surface densities assigned to galaxies, we observe a strong environmental dependence on the properties of galaxies (e.g., SFR, sSFR and the quiescent fraction) at z ≤ 1. We explore the fractional role of stellar mass and environment in quenching the star-formation. In the second approach, we use the Multi-scale Morphology Filter algorithm to disentangle the density field into its component. We apply this method to a sample of star-forming galaxies for a large-scale structure at z ∼0.84 in the HiZELS-COSMOS field. We show that the observed median SFR, stellar mass, sSFR, the mean SFR$-$mass relation and its scatter for star-forming galaxies do not strongly depend on the cosmic web. However, the fraction of H[Alpha] star-forming galaxies varies with environment and is enhanced in filaments. Furthermore, we study the physical properties of a spectroscopic sample of star-forming galaxies in a large filament in the COSMOS field at z ∼0.53, with spectroscopic data taken with the Keck/DEIMOS spectrograph, and compare them with a control sample of field galaxies. We spectroscopically confirm the presence of a large galaxy filament (∼ 8 Mpc). We show that within the uncertainties, the ionization parameter, EW, EW versus sSFR relation, EW versus stellar mass relation, line-of-sight velocity dispersion, dynamical mass, and stellar-to-dynamical mass ratio are similar for filament and field star-forming galaxies. However, we show that on average, filament star-forming galaxies are more metal-enriched (∼ 0.1-0.15 dex) and the electron densities are significantly lower (a factor of ∼17) in filament star-forming systems compared to those in the field. Our results highlight the potential role of galaxy filaments and intermediate-density environments on the evolution of galaxies, which has been poorly investigated.
Chaisson addresses some of the most basic issues we can contemplate: the origin of matter and the origin of life, and the ways matter, life, and radiation interact and change with time. He designs for us an expansive yet intricate model depicting the origin and evolution of all material structures.
A coherent introduction for researchers in astronomy, particle physics, and cosmology on the formation and evolution of galaxies.
As the most massive bound structures in the universe, galaxy clusters are a powerful probe of the impact of environment on galaxy evolution. In this work, I present AMASCFI, a new cluster finder algorithm using photometric redshifts I developed during the PhD and use the cluster catalogue obtained on the Canada France Hawaii Telescope Legacy Survey (CFHTLS) to investigate the role played by clusters and their environment on galaxy evolution. We show the good performances of AMASCFI on Euclid and the CFHTLS using mock data. In particular AMASCFI is 90% pure and 70% complete to z
My intention in this book is to describe in simple language, using a minimum of mathematics but a maximum of numerical values, the most important developments of science dealing with matter and energy on cosmic and global scales. In the conventional literature all of these findings are distributed among books and journals on physics, astronomy, chemistry, geology, biology, energy, engineering, and the environmental sciences. The main purpose here is to attempt to give a unified description of Nature from the elementary particles to the Universe as a whole. This is used as a basis for analysing the future development of mankind. The future evolution of the Universe, galaxies, stars, and planets gives some hope for the destiny of mankind. The problem of matter and energy flow on the Earth appears soluble even for the distant future. There seems to be no reason why a long period of human development on this planet should not be possible. The book has been prepared based on my lectures at the Warsaw University from 1959 to 1968 and during the 15 years 1969-1983 at the Swiss Federal Institute of Technology (Eidgenossische Technische Hochschule) in Zurich and at the University of Zurich. I wish to give my sincere thanks to the Swiss Federal Institute for Reactor Research at Wurenlingen for their constant support. I am especially grateful to Mrs. Christine Stratton for setting up the English text and to Mr. R.W. Stratton and LG. McKinley for their helpful criticisms and remarks.
The work presented in this dissertation provides the groundwork for understanding key unresolved questions in the study of galaxy evolution: the circumgalactic medium (CGM) and the role of environment. I present a new survey that has the power to drastically improve our understanding of the CGM and use it to estimate the size of the CGM as a function of galactic mass. In addition, a novel method to reconstruct the cosmic web using Physarum polycephalum slime mold is presented and applied to the SDSS surveys. This cosmic web reconstruction was released publicly with SDSS DR17 and will allow exciting connections between galaxies and their environments to be illuminated, to distances greater than other previous catalogs.
Galaxies, along with their underlying dark matter halos, constitute the building blocks of structure in the Universe. Of all fundamental forces, gravity is the dominant one that drives the evolution of structures from small density seeds at early times to the galaxies we see today. The interactions among myriads of stars, or dark matter particles, in a gravitating structure produce a system with fascinating connotations to thermodynamics, with some analogies and some fundamental differences. Ignacio Ferreras presents a concise introduction to extragalactic astrophysics, with emphasis on stellar dynamics, and the growth of density fluctuations in an expanding Universe. Additional chapters are devoted to smaller systems (stellar clusters) and larger ones (galaxy clusters). Fundamentals of Galaxy Dynamics, Formation and Evolution is written for advanced undergraduates and beginning postgraduate students, providing a useful tool to get up to speed in a starting research career. Some of the derivations for the most important results are presented in detail to enable students appreciate the beauty of maths as a tool to understand the workings of galaxies. Each chapter includes a set of problems to help the student advance with the material.
This book follows the evolutionary trail all the way from the Big Bang 13.7 billion years ago to conscious life today. It is an accessible introductory book written for the interested layperson – anyone interested in the ‘big picture’ coming from modern science. It covers a wide range of topics including the origin and evolution of our universe, the nature and origin of life, the evolution of life including questions of birth and death, the evolution of cognition, the nature of consciousness, the possibility of extraterrestrial life and the future of the universe. The book is written in a narrative style, as these topics are all parts of a single story. It concludes with a discussion on the nature and future of science.