Galaxy Formation Near the Epoch of Reionization
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Report from the Dark Energy Task Force (DETF)
Fermi National Accelerator Laboratory Fermilab Particle Astrophysics Center P.O.Box 500 - MS209 Batavia, Il l i noi s • 60510 June 6, 2006 Dr. Garth Illingworth Chair, Astronomy and Astrophysics Advisory Committee Dr. Mel Shochet Chair, High Energy Physics Advisory Panel Dear Garth, Dear Mel, I am pleased to transmit to you the report of the Dark Energy Task Force. The report is a comprehensive study of the dark energy issue, perhaps the most compelling of all outstanding problems in physical science. In the Report, we outline the crucial need for a vigorous program to explore dark energy as fully as possible since it challenges our understanding of fundamental physical laws and the nature of the cosmos. We recommend that program elements include 1. Prompt critical evaluation of the benefits, costs, and risks of proposed long-term projects. 2. Commitment to a program combining observational techniques from one or more of these projects that will lead to a dramatic improvement in our understanding of dark energy. (A quantitative measure for that improvement is presented in the report.) 3. Immediately expanded support for long-term projects judged to be the most promising components of the long-term program. 4. Expanded support for ancillary measurements required for the long-term program and for projects that will improve our understanding and reduction of the dominant systematic measurement errors. 5. An immediate start for nearer term projects designed to advance our knowledge of dark energy and to develop the observational and analytical techniques that will be needed for the long-term program. Sincerely yours, on behalf of the Dark Energy Task Force, Edward Kolb Director, Particle Astrophysics Center Fermi National Accelerator Laboratory Professor of Astronomy and Astrophysics The University of Chicago REPORT OF THE DARK ENERGY TASK FORCE Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude. -
Last and First Men
LAST AND FIRST MEN A STORY OF THE NEAR AND FAR FUTURE by W. Olaf Stapledon Project Gutenburg PREFACE THIS is a work of fiction. I have tried to invent a story which may seem a possible, or at least not wholly impossible, account of the future of man; and I have tried to make that story relevant to the change that is taking place today in man's outlook. To romance of the future may seem to be indulgence in ungoverned speculation for the sake of the marvellous. Yet controlled imagination in this sphere can be a very valuable exercise for minds bewildered about the present and its potentialities. Today we should welcome, and even study, every serious attempt to envisage the future of our race; not merely in order to grasp the very diverse and often tragic possibilities that confront us, but also that we may familiarize ourselves with the certainty that many of our most cherished ideals would seem puerile to more developed minds. To romance of the far future, then, is to attempt to see the human race in its cosmic setting, and to mould our hearts to entertain new values. But if such imaginative construction of possible futures is to be at all potent, our imagination must be strictly disciplined. We must endeavour not to go beyond the bounds of possibility set by the particular state of culture within which we live. The merely fantastic has only minor power. Not that we should seek actually to prophesy what will as a matter of fact occur; for in our present state such prophecy is certainly futile, save in the simplest matters. -
Fine-Tuning, Complexity, and Life in the Multiverse*
Fine-Tuning, Complexity, and Life in the Multiverse* Mario Livio Dept. of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA E-mail: [email protected] and Martin J. Rees Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK E-mail: [email protected] Abstract The physical processes that determine the properties of our everyday world, and of the wider cosmos, are determined by some key numbers: the ‘constants’ of micro-physics and the parameters that describe the expanding universe in which we have emerged. We identify various steps in the emergence of stars, planets and life that are dependent on these fundamental numbers, and explore how these steps might have been changed — or completely prevented — if the numbers were different. We then outline some cosmological models where physical reality is vastly more extensive than the ‘universe’ that astronomers observe (perhaps even involving many ‘big bangs’) — which could perhaps encompass domains governed by different physics. Although the concept of a multiverse is still speculative, we argue that attempts to determine whether it exists constitute a genuinely scientific endeavor. If we indeed inhabit a multiverse, then we may have to accept that there can be no explanation other than anthropic reasoning for some features our world. _______________________ *Chapter for the book Consolidation of Fine Tuning 1 Introduction At their fundamental level, phenomena in our universe can be described by certain laws—the so-called “laws of nature” — and by the values of some three dozen parameters (e.g., [1]). Those parameters specify such physical quantities as the coupling constants of the weak and strong interactions in the Standard Model of particle physics, and the dark energy density, the baryon mass per photon, and the spatial curvature in cosmology. -
Icons of Survival: Metahumanism As Planetary Defense." Nerd Ecology: Defending the Earth with Unpopular Culture
Lioi, Anthony. "Icons of Survival: Metahumanism as Planetary Defense." Nerd Ecology: Defending the Earth with Unpopular Culture. London: Bloomsbury Academic, 2016. 169–196. Environmental Cultures. Bloomsbury Collections. Web. 25 Sep. 2021. <http:// dx.doi.org/10.5040/9781474219730.ch-007>. Downloaded from Bloomsbury Collections, www.bloomsburycollections.com, 25 September 2021, 20:32 UTC. Copyright © Anthony Lioi 2016. You may share this work for non-commercial purposes only, provided you give attribution to the copyright holder and the publisher, and provide a link to the Creative Commons licence. 6 Icons of Survival: Metahumanism as Planetary Defense In which I argue that superhero comics, the most maligned of nerd genres, theorize the transformation of ethics and politics necessary to the project of planetary defense. The figure of the “metahuman,” the human with superpowers and purpose, embodies the transfigured nerd whose defects—intellect, swarm-behavior, abnormality, flux, and love of machines—become virtues of survival in the twenty-first century. The conflict among capitalism, fascism, and communism, which drove the Cold War and its immediate aftermath, also drove the Golden and Silver Ages of Comics. In the era of planetary emergency, these forces reconfigure themselves as different versions of world-destruction. The metahuman also signifies going “beyond” these economic and political systems into orders that preserve democracy without destroying the biosphere. Therefore, the styles of metahuman figuration represent an appeal to tradition and a technique of transformation. I call these strategies the iconic style and metamorphic style. The iconic style, more typical of DC Comics, makes the hero an icon of virtue, and metahuman powers manifest as visible signs: the “S” of Superman, the tiara and golden lasso of Wonder Woman. -
Cosmology Slides
Inhomogeneous cosmologies George Ellis, University of Cape Town 27th Texas Symposium on Relativistic Astrophyiscs Dallas, Texas Thursday 12th December 9h00-9h45 • The universe is inhomogeneous on all scales except the largest • This conclusion has often been resisted by theorists who have said it could not be so (e.g. walls and large scale motions) • Most of the universe is almost empty space, punctuated by very small very high density objects (e.g. solar system) • Very non-linear: / = 1030 in this room. Models in cosmology • Static: Einstein (1917), de Sitter (1917) • Spatially homogeneous and isotropic, evolving: - Friedmann (1922), Lemaitre (1927), Robertson-Walker, Tolman, Guth • Spatially homogeneous anisotropic (Bianchi/ Kantowski-Sachs) models: - Gödel, Schücking, Thorne, Misner, Collins and Hawking,Wainwright, … • Perturbed FLRW: Lifschitz, Hawking, Sachs and Wolfe, Peebles, Bardeen, Ellis and Bruni: structure formation (linear), CMB anisotropies, lensing Spherically symmetric inhomogeneous: • LTB: Lemaître, Tolman, Bondi, Silk, Krasinski, Celerier , Bolejko,…, • Szekeres (no symmetries): Sussman, Hellaby, Ishak, … • Swiss cheese: Einstein and Strauss, Schücking, Kantowski, Dyer,… • Lindquist and Wheeler: Perreira, Clifton, … • Black holes: Schwarzschild, Kerr The key observational point is that we can only observe on the past light cone (Hoyle, Schücking, Sachs) See the diagrams of our past light cone by Mark Whittle (Virginia) 5 Expand the spatial distances to see the causal structure: light cones at ±45o. Observable Geo Data Start of universe Particle Horizon (Rindler) Spacelike singularity (Penrose). 6 The cosmological principle The CP is the foundational assumption that the Universe obeys a cosmological law: It is necessarily spatially homogeneous and isotropic (Milne 1935, Bondi 1960) Thus a priori: geometry is Robertson-Walker Weaker form: the Copernican Principle: We do not live in a special place (Weinberg 1973). -
Arxiv:1707.01004V1 [Astro-Ph.CO] 4 Jul 2017
July 5, 2017 0:15 WSPC/INSTRUCTION FILE coc2ijmpe International Journal of Modern Physics E c World Scientific Publishing Company Primordial Nucleosynthesis Alain Coc Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, Univ. Paris-Sud, Universit´eParis–Saclay, Bˆatiment 104, F–91405 Orsay Campus, France [email protected] Elisabeth Vangioni Institut d’Astrophysique de Paris, UMR-7095 du CNRS, Universit´ePierre et Marie Curie, 98 bis bd Arago, 75014 Paris (France), Sorbonne Universit´es, Institut Lagrange de Paris, 98 bis bd Arago, 75014 Paris (France) [email protected] Received July 5, 2017 Revised Day Month Year Primordial nucleosynthesis, or big bang nucleosynthesis (BBN), is one of the three evi- dences for the big bang model, together with the expansion of the universe and the Cos- mic Microwave Background. There is a good global agreement over a range of nine orders of magnitude between abundances of 4He, D, 3He and 7Li deduced from observations, and calculated in primordial nucleosynthesis. However, there remains a yet–unexplained discrepancy of a factor ≈3, between the calculated and observed lithium primordial abundances, that has not been reduced, neither by recent nuclear physics experiments, nor by new observations. The precision in deuterium observations in cosmological clouds has recently improved dramatically, so that nuclear cross sections involved in deuterium BBN need to be known with similar precision. We will shortly discuss nuclear aspects re- lated to BBN of Li and D, BBN with non-standard neutron sources, and finally, improved sensitivity studies using Monte Carlo that can be used in other sites of nucleosynthesis. -
The Reionization of Cosmic Hydrogen by the First Galaxies Abstract 1
David Goodstein’s Cosmology Book The Reionization of Cosmic Hydrogen by the First Galaxies Abraham Loeb Department of Astronomy, Harvard University, 60 Garden St., Cambridge MA, 02138 Abstract Cosmology is by now a mature experimental science. We are privileged to live at a time when the story of genesis (how the Universe started and developed) can be critically explored by direct observations. Looking deep into the Universe through powerful telescopes, we can see images of the Universe when it was younger because of the finite time it takes light to travel to us from distant sources. Existing data sets include an image of the Universe when it was 0.4 million years old (in the form of the cosmic microwave background), as well as images of individual galaxies when the Universe was older than a billion years. But there is a serious challenge: in between these two epochs was a period when the Universe was dark, stars had not yet formed, and the cosmic microwave background no longer traced the distribution of matter. And this is precisely the most interesting period, when the primordial soup evolved into the rich zoo of objects we now see. The observers are moving ahead along several fronts. The first involves the construction of large infrared telescopes on the ground and in space, that will provide us with new photos of the first galaxies. Current plans include ground-based telescopes which are 24-42 meter in diameter, and NASA’s successor to the Hubble Space Telescope, called the James Webb Space Telescope. In addition, several observational groups around the globe are constructing radio arrays that will be capable of mapping the three-dimensional distribution of cosmic hydrogen in the infant Universe. -
DARK AGES of the Universe the DARK AGES of the Universe Astronomers Are Trying to fill in the Blank Pages in Our Photo Album of the Infant Universe by Abraham Loeb
THE DARK AGES of the Universe THE DARK AGES of the Universe Astronomers are trying to fill in the blank pages in our photo album of the infant universe By Abraham Loeb W hen I look up into the sky at night, I often wonder whether we humans are too preoccupied with ourselves. There is much more to the universe than meets the eye on earth. As an astrophysicist I have the privilege of being paid to think about it, and it puts things in perspective for me. There are things that I would otherwise be bothered by—my own death, for example. Everyone will die sometime, but when I see the universe as a whole, it gives me a sense of longevity. I do not care so much about myself as I would otherwise, because of the big picture. Cosmologists are addressing some of the fundamental questions that people attempted to resolve over the centuries through philosophical thinking, but we are doing so based on systematic observation and a quantitative methodology. Perhaps the greatest triumph of the past century has been a model of the uni- verse that is supported by a large body of data. The value of such a model to our society is sometimes underappreciated. When I open the daily newspaper as part of my morning routine, I often see lengthy de- scriptions of conflicts between people about borders, possessions or liberties. Today’s news is often forgotten a few days later. But when one opens ancient texts that have appealed to a broad audience over a longer period of time, such as the Bible, what does one often find in the opening chap- ter? A discussion of how the constituents of the universe—light, stars, life—were created. -
Dermining the Photon Budget of Galaxies During Reionization with Numerical Simulations, and Studying the Impact of Dust Joseph Lewis
Who reionized the Universe ? : dermining the photon budget of galaxies during reionization with numerical simulations, and studying the impact of dust Joseph Lewis To cite this version: Joseph Lewis. Who reionized the Universe ? : dermining the photon budget of galaxies during reioniza- tion with numerical simulations, and studying the impact of dust. Astrophysics [astro-ph]. Université de Strasbourg, 2020. English. NNT : 2020STRAE041. tel-03199136 HAL Id: tel-03199136 https://tel.archives-ouvertes.fr/tel-03199136 Submitted on 15 Apr 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. UNIVERSITÉ DE STRASBOURG ÉCOLE DOCTORALE 182 UMR 7550, Observatoire astronomique de Strasbourg THÈSE présentée par : Joseph Lewis soutenue le : 25 septembre 2020 pour obtenir le grade de : Docteur de l’université de Strasbourg Discipline/ Spécialité : Astrophysique Qui a réionisé l’Univers ? Détermination par la simulation numérique du budget de photons des galaxies pendant l’époque de la Réionisation, et étude de l’impact des poussières THÈSE dirigée par : M. AUBERT Dominique Professeur des universités, Université de Strasbourg RAPPORTEURS : M. GONZALES Mathias Maître de conférences, Université de Paris M. LANGER Mathieu Professeur des universités, Université Paris-Saclay AUTRES MEMBRES DU JURY : M. -
Determining the Redshift of Reionization from the Spectra Of
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Determining the Redshift of Reionization From the Sp ectra of High{Redshift Sources 1;2 1 Zoltan Haiman and Abraham Lo eb ABSTRACT The redshift at which the universe was reionized is currently unknown. We examine the optimal strategy for extracting this redshift, z , from the sp ectra of reion early sources. For a source lo cated at a redshift z beyond but close to reionization, s 32 (1 + z ) < (1 + z ) < (1 + z ), the Gunn{Peterson trough splits into disjoint reion s reion 27 Lyman , , and p ossibly higher Lyman series troughs, with some transmitted ux in b etween these troughs. We show that although the transmitted ux is suppressed considerably by the dense Ly forest after reionization, it is still detectable for suciently bright sources and can b e used to infer the reionization redshift. The Next Generation Space Telescop e will reach the sp ectroscopic sensitivity required for the detection of such sources. Subject headings: cosmology: theory { quasars: absorption lines { galaxies: formation {intergalactic medium { radiative transfer Submitted to The Astrophysical Journal, July 1998 1. Intro duction The standard Big Bang mo del predicts that the primeval plasma recombined and b ecame predominantly neutral as the universe co oled b elow a temp erature of several thousand degrees at 3 a redshift z 10 (Peebles 1968). Indeed, the recent detection of Cosmic Microwave Background (CMB) anisotropies rules out a fully ionized intergalactic medium (IGM) beyond z 300 (Scott, Silk & White 1995). However, the lack of a Gunn{Peterson trough (GP, Gunn & Peterson 1965) in the sp ectra of high{redshift quasars (Schneider, Schmidt & Gunn 1991) and galaxies (Franx et < al. -
Structure Formation in a CDM Universe
Structure formation in a CDM Universe Thomas Quinn, University of Washington Greg Stinson, Charlotte Christensen, Alyson Brooks Ferah Munshi Fabio Governato, Andrew Pontzen, Chris Brook, James Wadsley Microwave Background Fluctuations Image courtesy NASA/WMAP Large Scale Clustering A well constrained cosmology ` Contents of the Universe Can it make one of these? Structure formation issues ● The substructure problem ● The angular momentum problem ● The cusp problem Light vs CDM structure Stars Gas Dark Matter The CDM Substructure Problem Moore et al 1998 Substructure down to 100 pc Stadel et al, 2009 Consequences for direct detection Afshordi etal 2010 Warm Dark Matter cold warm hot Constant Core Mass Strigari et al 2008 Light vs Mass Number density log(halo or galaxy mass) Simulations of Galaxy formation Guo e tal, 2010 Origin of Galaxy Spins ● Torques on the collapsing galaxy (Peebles, 1969; Ryden, 1988) λ ≡ L E1/2/GM5/2 ≈ 0.09 for galaxies Distribution of Halo Spins f(λ) Λ = LE1/2/GM5/2 Gardner, 2001 Angular momentum Problem Too few low-J baryons Van den Bosch 01 Bullock 01 Core/Cusps in Dwarfs Moore 1994 Warm DM doesn't help Moore et al 1999 Dwarf simulated to z=0 Stellar mass = 5e8 M sun` M = -16.8 i g - r = 0.53 V = 55 km/s rot R = 1 kpc d M /M = 2.5 HI * f = .3 f cosmic b b i band image Dwarf Light Profile Rotation Curve Resolution effects Low resolution: bad Low resolution star formation: worse Inner Profile Slopes vs Mass Governato, Zolotov etal 2012 Constant Core Masses Angular Momentum Outflows preferential remove low J baryons Simulation Results: Resolution and H2 Munshi, in prep. -
The Optical Depth to Reionization As a Probe of Cosmological and Astrophysical Parameters Aparna Venkatesan University of San Francisco, [email protected]
The University of San Francisco USF Scholarship: a digital repository @ Gleeson Library | Geschke Center Physics and Astronomy College of Arts and Sciences 2000 The Optical Depth to Reionization as a Probe of Cosmological and Astrophysical Parameters Aparna Venkatesan University of San Francisco, [email protected] Follow this and additional works at: http://repository.usfca.edu/phys Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation Aparna Venkatesan. The Optical Depth to Reionization as a Probe of Cosmological and Astrophysical Parameters. The Astrophysical Journal, 537:55-64, 2000 July 1. http://dx.doi.org/10.1086/309033 This Article is brought to you for free and open access by the College of Arts and Sciences at USF Scholarship: a digital repository @ Gleeson Library | Geschke Center. It has been accepted for inclusion in Physics and Astronomy by an authorized administrator of USF Scholarship: a digital repository @ Gleeson Library | Geschke Center. For more information, please contact [email protected]. THE ASTROPHYSICAL JOURNAL, 537:55È64, 2000 July 1 ( 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE OPTICAL DEPTH TO REIONIZATION AS A PROBE OF COSMOLOGICAL AND ASTROPHYSICAL PARAMETERS APARNA VENKATESAN Department of Astronomy and Astrophysics, 5640 South Ellis Avenue, University of Chicago, Chicago, IL 60637; aparna=oddjob.uchicago.edu Received 1999 December 17; accepted 2000 February 8 ABSTRACT Current data of high-redshift absorption-line systems imply that hydrogen reionization occurred before redshifts of about 5. Previous works on reionization by the Ðrst stars or quasars have shown that such scenarios are described by a large number of cosmological and astrophysical parameters.