[PDF] The Growth Of Supermassive Black Holes And Connections To Star Formation In Galaxies eBook

Author : Chien-Ting Chen
Publisher :
Page : 274 pages
File Size : 29,81 MB
Release : 2015
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ISBN :

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A profound recent discovery in studies of the cosmic evolution of galaxies is that at the center of essentially every large galaxy there is a supermassive black hole (SMBH). This dissertation explores the origin of these massive black holes and their connection to the host galaxies, by studying rapidly growing black holes (the active galactic nuclei or AGNs) and galaxies that are actively forming stars using the wealth of observations in extragalactic surveys. We first report a strong correlation between star formation rate (SFR) and the average SMBH accretion rate in star-forming galaxies. This highlights that even though the growth rates of the SMBHs and the host galaxies in individual galaxies hosting AGNs are not directly correlated, potentially due to the short variability timescale of AGN relative to SF, averaging over the full AGN population still yields a strong linear correlation between AGN and star formation. We next present evidence for a link between AGN obscuration and host galaxy star formation in the most luminous AGNs: quasars. With careful decomposition of galaxy and AGN contributions through analysis of spectral energy distributions, we successfully placed constraints on the SFR in luminous quasars in which AGN radiation outshines the host galaxy at most wavelengths. We find that obscured quasars have a two times larger far-infrared (IR) detection fraction, far-IR flux and SFR than unobscured quasars. The result indicates that large-scale gas and dust in powderful star-forming galaxies contribute to obscuration of the AGN in luminous quasars. Together, these two results support a scenario in which galaxy and SMBH grow from the same gas reservoir that can also obscure the central SMBH during the luminous quasar phase. Finally, we present a study of the correlation between the AGN mid-IR and X-ray luminosities for a large sample of spectroscopically confirmed type 1 quasars. We have determined that more luminous quasars show increasingly weak X-ray emission relative to their mid-IR luminosity, providing insight into the physics of quasar accretion and highlighting an important effect that must be accounted for in studies of SMBH evolution.

Author :
Publisher :
Page : 64 pages
File Size : 40,3 MB
Release : 2013
Category : Black holes (Astronomy)
ISBN : 9780716695899

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"An introduction to quasars and black holes with information about their formation and characteristics. Includes diagrams, fun facts, a glossary, a resource list, and an index"--Provided by publisher.

Author : Daniel Anglés-Alcázar
Publisher :
Page : 207 pages
File Size : 24,43 MB
Release : 2014
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I use cosmological hydrodynamic simulations to investigate different aspects of the evolution of galaxies and massive black holes across cosmic time. First, I present high resolution "zoom-in" simulations including various prescriptions for galactic outflows designed to explore the impact of star-formation driven winds on the morphological, dynamical, and structural properties of individual galaxies from early times down to z = 2. Simulations without winds produce massive, compact galaxies with low gas fractions, super-solar metallicities, high bulge fractions, and much of the star formation concentrated within the inner kpc. I show that strong winds are required to suppress early star formation, maintain high gas fractions, redistribute star-forming gas and metals over larger scales, and increase the velocity dispersion of simulated galaxies, more in agreement with the large, extended, turbulent disks typical of high-redshift star-forming galaxies. Next, I combine cosmological simulations with analytic models of black hole growth to investigate the physical mechanisms driving the observed connection between massive black holes and their host galaxies. I describe a plausible model consistent with available observations in which black hole growth is limited by galaxy-scale torques. In this torque-limited growth scenario, black holes and host galaxies evolve on average toward the observed scaling relations, regardless of the initial conditions, and with no need for mass averaging through mergers or additional self-regulation processes. Outflows from the accretion disk play a key role by providing significant mass loss, but there is no need for strong interaction with the inflowing gas in order to regulate black holes in a non-linear feedback loop. I discuss some of the main implications of this scenario in the context of current observations, including the distribution and evolution of Eddington ratios, the connection between major galaxy mergers, star formation, and nuclear activity, and the rapid growth of the first black holes in the early universe. Finally, I present preliminary results from simulations including a fully consistent treatment of black hole accretion and feedback indicating that the effects of powerful accretion-driven outflows on black hole growth itself may have a more limited impact than previously thought.

Author : Luis C. Ho
Publisher : Cambridge University Press
Page : 502 pages
File Size : 50,40 MB
Release : 2004-09-09
Category : Science
ISBN : 9780521824491

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This book was originally published in 2004. Black holes are among the most mysterious objects in the Universe. Weighing up to several billion Suns, massive black holes have long been suspected to be the central powerhouses of energetic phenomena such as quasars. Advances in astronomy have not only provided spectacular proof of this long-standing paradigm, but have revealed the unexpected result that far from being rare, exotic beasts, they inhabit the center of virtually all large galaxies. Candidate black holes have been identified in increasingly large numbers of galaxies, both inactive and active, to the point where statistical studies are possible. Fresh work has highlighted the close connection between the formation, growth, and evolution of supermassive black holes and their host galaxies. This volume contains the invited lectures from an international symposium that was held to explore this exciting theme, and is a valuable review for professional astronomers and graduate students.

Author : Chi-hun Kim
Publisher : Stanford University
Page : 189 pages
File Size : 36,3 MB
Release : 2011
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While mounting observational evidence suggests the coevolution of galaxies and their embedded massive black holes (MBHs), a comprehensive astrophysical understanding which incorporates both galaxies and MBHs has been missing. To tackle the nonlinear processes of galaxy formation, we develop a state-of-the-art numerical framework which self-consistently models the interplay between galactic components: dark matter, gas, stars, and MBHs. Utilizing this physically motivated tool, we present an investigation of a massive star-forming galaxy hosting a slowly growing MBH in a cosmological LCDM simulation. The MBH feedback heats the surrounding gas and locally suppresses star formation in the galactic inner core. In simulations of merging galaxies, the high-resolution adaptive mesh allows us to observe widespread starbursts via shock-induced star formation, and the interplay between the galaxies and their embedding medium. Fast growing MBHs in merging galaxies drive more frequent and powerful jets creating sizable bubbles at the galactic centers. We conclude that the interaction between the interstellar gas, stars and MBHs is critical in understanding the star formation history, black hole accretion history, and cosmological evolution of galaxies. Expanding upon our extensive experience in galactic simulations, we are well poised to apply this tool to other challenging, yet highly rewarding tasks in contemporary astrophysics, such as high-redshift quasar formation.

Author : Tiziana Di Matteo
Publisher : Springer Nature
Page : 212 pages
File Size : 15,52 MB
Release : 2019-10-31
Category : Science
ISBN : 3662597993

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The ultimate proofs that black holes exist have been obtained very recently thanks to the detection of gravitational waves from their coalescence and due to material orbiting at a distance of some gravitational radii imaged by optical interferometry or X-ray reverberation mapping. This book provides three comprehensive and up-to-date reviews covering the gravitational wave breakthrough, our understanding of accretion and feedback in supermassive black holes and the relevance of black holes for the Universe since the Big Bang. Neil J. Cornish presents gravitational wave emission from black hole mergers and the physics of detection. Andrew King reviews the physics of accretion on to supermassive black holes and their feedback on host galaxies. Tiziana Di Matteo addresses our understanding of black hole formation at cosmic dawn, the emergence of the first quasars, black hole merging and structure formation. The topics covered by the 48th Saas-Fee Course provide a broad overview of the importance of black holes in modern astrophysics.

Author : Celestial Angell
Publisher : Dedona Publishing
Page : 43 pages
File Size : 26,53 MB
Release :
Category : Science
ISBN :

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A black hole is a region in space where the gravitational pull is so strong that nothing, not even light, can escape from it. This occurs when a massive amount of matter is compressed into a very small area, creating a powerful gravitational field. Black holes form through various processes that involve the collapse of massive astronomical objects and the merging of smaller black holes. One primary method is the stellar collapse. Stars, during their lifecycle, fuse hydrogen into helium in their cores. When the hydrogen is depleted, they begin fusing heavier elements until iron is produced. For stars more than 20 times the mass of the Sun, the end of this fusion process leads to a supernova explosion. The core of the star collapses rapidly due to gravity, and if the core's mass is sufficiently large (typically more than about three times the mass of the Sun), it will continue collapsing into a singularity, forming a stellar-mass black hole. Another way black holes can form is through accretion and growth. A compact object like a neutron star or a white dwarf can accumulate matter from a companion star or its surroundings. As this matter accumulates, the mass of the compact object increases, and it may eventually reach a critical mass where it collapses into a black hole.

Author : Nathaniel Robert Ross
Publisher :
Page : 131 pages
File Size : 27,88 MB
Release : 2016
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ISBN :

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Massive galaxies in the nearby universe all show evidence of a central Supermassive Black Hole. The black holes are seen to grow over time by accretion of gas from their host galaxy, a phenomenon referred to as an Active Galactic Nucleus. This process is believed to be fundamental to the observed correlations between black hole mass and properties of the host galaxies. We have a more limited and biased understanding of the growth of supermassive black holes in more 'typical' galaxies at z 1 2. In this work, we search for Active Galactic Nuclei in a population of star-forming galaxies spanning a mass range of M 10^7 10^12 M at 0.62 z

Author : Andrea Merloni
Publisher : Springer Science & Business Media
Page : 524 pages
File Size : 45,84 MB
Release : 2005-04-25
Category : Science
ISBN : 9783540252757

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Supermassive black holes are now believed to play an important role in the evolution of the Universe. Every respectable galaxy hosts in its center a black hole that appears to regulate the growth of the galaxy itself. In this book, leading experts in the field review the most recent theoretical and observational results on the following topics: - formation and growth of the first black holes in the Universe and their role in the formation and evolution of galaxies - the physics of black-hole accretion and the production of relativistic jets - binary black-hole mergers and gravitational radiation. Theoretical work is supplemented by the most recent exciting results from space and ground based observatories. This volume is useful research and reference tool for the entire astrophysical community.