DOCSLIB.ORG

Interactions Between UHE Particles and Protogalaxy Environments

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Interactions Between UHE Particles and Protogalaxy Environments Interactions between UHE Particles and Protogalaxy Environments Ellis Owen Mullard Space Science Laboratory University College London United Kingdom E-mail: [email protected] Kinwah Wu, Idunn Jacobsen, Pooja Surajbali Image Credit: NASA - Adolf Schaller Hubble gallery Artist’s impression of protogalaxies HEPP/APP University of Sussex, Brighton, United Kingdom, March 2016 Outline 1. UHE Particles in Protogalaxies 2. Protogalaxy Environments 3. Interaction Mechanisms & Losses 4. Energy Deposition Lengths & ISM/IGM Heating 2 Ultra High-Energy Particles in Protogalaxies • Cosmic Rays (CRs) accelerated in high energy astrophysical environments – Supernovae explosions / shocks – Accretion • Particle energy distribution follows power law, peaks around ~10 GeV for galactic (stellar) contribution • Expected to be present in young starburst galaxies (protogalaxies) – High star formation rate (SFR) ~1000 times more than cosmic average – Rate of supernovae roughly follows SFR – Cosmic ray flux attributed to stellar sources roughly follows supernova rate 3 102 2 101 10 Protogalaxy Environment 3 − 0 Density Fields 10 101 King radius • King model 102 3 1 − 10− 101 100 ParameterMatter Value Density/cm 3 − rt 2kpc 100 r 1kpc2 K 10− 1 10− 3 Matter Density/cm 1 n0 10 cm− 10− 2 10− Matter Density/cm 3 • Red line at King radius,10− 1kpc 3 10 3 2 1 0 1 − 3 2 1 0 1 10− 1010− − 10− 1010− 10 1010 10 – Approximate radius of a Radius/kpc 2 Radius/kpc protogalaxy (e.g. from high z 10− LAE observations) 4 10 3 − 3 2 1 0 1 10− 10− 10− 10 10 Radius/kpc 102 101 Protogalaxy Environment 3 − 0 r>rgal Radiation Fields 10 7 • Uniform spherical 67 distribution of stars1 within 6 10− 1 5 protogalaxy − 1 s Matter Density/cm 5 − 2 s 2 − • High mass, low metallicity − 44 – O/B type, T~30,000K 2 10− 3 – T Spectrally characterizes 3 radiation field (BB spectrum) Flux/erg cm 2 Flux/erg cm 2 • Field approximately uniform 1 3 within the protogalaxy10− radius, 3 10 2 1 0 1 then simple inverse 10square− 100 − 2 4 10− 6 8 1010 10 Radius/kpc law at r>r Radius/kpc gal 0 0 2 4 6 8 10 Radius/kpc 5 5 10− 7 10− Protogalaxy Environment9 10− 11 10− Efficiency of energy transfer Magnetic Fields 5 10− 13 10− SNe à Turbulence à B field 7 10− 15 • Two scale components:10− 5 9 1010−− 17 -3 7 – Local viscous scale, 10~10− pc 10−11 10− 10 9 19 − 10− 1113 – Turbulent forcing ~1kpc 1010−− 21 10 13 10− − 15 10− • SN driven, B follows density 15 10− 23 17 Forcing Scale, ✏ =0.1 10− 1010 17 profile −− 19 25 10− 19 Viscous Scale, ✏ =0.1 10− 10− -20 21 • Initial B field ~10 G 10− Forcing Scale, ✏ =1 21 27 23 Forcing Scale, ✏ =0.1 10− 1010−− Protogalaxy Magnetic Field Strength/G permeates protogalaxy Viscous Scale, ✏Viscous=0.1 Scale, ✏ =1 25 29 10− 23 Forcing Scale, ✏ =0.1 10− 10− Forcing Scale, ✏ =1 27 10− Forcing Scale, ✏ = 10 Protogalaxy Magnetic Field Strength/G • Stellar processes drive 25 Viscous Scale, ✏ =1 Viscous Scale, ✏ =0.1 31 29 1010−− 10− Forcing Scale, ✏ = 10 Viscous Scale, ✏ = 10 31 Forcing Scale, ✏ =1 turbulence, which drives B 10− 27 Viscous Scale, ✏ = 10 33 10− 10− Protogalaxy Magnetic Field Strength/G 33 4 3 10− 2 1 0 1 2 3 Viscous4 Scale,5✏ =1 4 3 2 1 0 1 2 3 4 5 10− 10− 1029−10− 10− 1010− 10− 10 10 1010 10 1010 1010 10 10 10 field up to µG levels seen in 10− Age of Galaxy/Myr Forcing Scale, ✏ = 10 Age of Galaxy/Myr current epoch 31 10− Viscous Scale, ✏ = 10 10 33 – Exponential growth − 4 3 2 1 0 1 2 3 4 5 10− 10− 10− 10− 10 10 10 10 10 10 – Then linear growth of the forcing scale Age of Galaxy/Myr field after local saturation Model follows J. Schober + 2013 6 5 10− 7 10− Protogalaxy Environment9 10− 11 10− Efficiency of energy transfer Magnetic Fields 5 10− 13 10− SNe à Turbulence à B field 7 10− 15 • Two scale components:10− 5 9 1010−− 17 -3 7 – Local viscous scale, 10~10− pc 10−11 10− 10 9 19 − 10− 1113 – Turbulent forcing ~1kpc 1010−− 21 10 13 10− − 15 10− • SN driven, B follows density 15 10− 23 17 Forcing Scale, ✏ =0.1 10− 1010 17 profile −− 19 25 10− 19 Viscous Scale, ✏ =0.1 10− 10− -20 21 • Initial B field ~10 G 10− Forcing Scale, ✏ =1 21 27 23 Forcing Scale, ✏ =0.1 10− 1010−− Protogalaxy Magnetic Field Strength/G permeates protogalaxy Viscous Scale, ✏Viscous=0.1 Scale, ✏ =1 25 29 10− 23 Forcing Scale, ✏ =0.1 10− 10− Forcing Scale, ✏ =1 27 10− Forcing Scale, ✏ = 10 Protogalaxy Magnetic Field Strength/G • Stellar processes drive 25 Viscous Scale, ✏ =1 Viscous Scale, ✏ =0.1 31 29 1010−− 10− Forcing Scale, ✏ = 10 Viscous Scale, ✏ = 10 31 Forcing Scale, ✏ =1 turbulence, which drives B 10− 27 Viscous Scale, ✏ = 10 33 10− 10− Protogalaxy Magnetic Field Strength/G 33 4 3 10− 2 1 0 1 2 3 Viscous4 Scale,5✏ =1 4 3 2 1 0 1 2 3 4 5 10− 10− 1029−10− 10− 1010− 10− 10 10 1010 10 1010 1010 10 10 10 field up to µG levels seen in 10− Age of Galaxy/Myr Forcing Scale, ✏ = 10 Age of Galaxy/Myr current epoch Exponential31 growth 10− Linear growth Viscous Scale, ✏ = 10 10 33 – Exponential growth − 4 3 2 1 0 1 2 3 4 5 10− 10− Local10 −saturation10− 10 10 10 10 10 10 – Then linear growth of the forcing scale Age of Galaxy/Myr field after local saturation Model follows J. Schober + 2013 6 Interaction Mechanisms & Losses • Low energy particles – Collisions • Direct ionization • Heating • High energy particles – Proton-photon (p�) • Pion production (Photopion) • Pair production (Photopair) – Proton-proton (pp) • Pion production (Hadronuclear) 7 Interaction Mechanisms & Losses Photopion (��) Interaction 0 + p + ⇡ p +2γ + pion multiplicities at p + γ ∆ ! higher energies ! ! n + ⇡+ n + µ+ + ⌫ ( ! µ + Photopair (�e) Interaction n + e + ⌫e +¯⌫µ + ⌫µ + p + γ p + e + e− . ! 8 Interaction Mechanisms & Losses Hadronuclear (pp) Interaction p + p + ⇡0 p + ∆+ p + p + ⇡+ 8 ! 8 p + p > <>p + n + ⇡+ + pion multiplicities ! > at higher energies > + < ++ >n + p + ⇡ n + ∆ : + > ! (n + n + 2(⇡ ) > > :> 9 Interaction Mechanisms & Losses Hadronuclear (pp) Interaction p + p + ⇡0 p + ∆+ p + p + ⇡+ 8 ! 8 p + p > <>p + n + ⇡+ + pion multiplicities ! > at higher energies > + < ++ >n + p + ⇡ n + ∆ : + > ! (n + n + 2(⇡ ) > > :> Interactions of neutrons and photons à pion production n + γ ⇡’s ! 9 Interaction Mechanisms & Losses Hadronuclear (pp) Interaction p + p + ⇡0 p + ∆+ p + p + ⇡+ 8 ! 8 p + p > <>p + n + ⇡+ + pion multiplicities ! > at higher energies > + < ++ >n + p + ⇡ n + ∆ : + ! (n + n + 2(⇡ ) > > > : Pions decay to photons, muons, Interactions of neutrons and neutrinos, electrons, positrons, photons à pion production antineutrinos n + γ ⇡’s ! ⇡ γ,µ,e,⌫ ... ! 9 Cross Section/Mean Free Path � Interactions • Pair production, Bethe-Heitler 7 ✏ σ (✏ ) ↵ σ ln r process γe r ⇡ 6⇡ f T k ✓ γe ◆ – Cross Section by fitting function 10 Cross Section/Mean Free Path � Interactions • Pair production, Bethe-Heitler 7 ✏ σ (✏ ) ↵ σ ln r process γe r ⇡ 6⇡ f T k ✓ γe ◆ – Cross Section by fitting function • Photopion production – Cross section by fitting step function to data (Dermer & Menon 2009/Reimer 2007) 10 Cross Section/Mean Free Path � Interactions • Pair production, Bethe-Heitler 7 ✏ σ (✏ ) ↵ σ ln r process γe r ⇡ 6⇡ f T k ✓ γe ◆ – Cross Section by fitting function • Photopion production – Cross section by fitting step function to data (Dermer & Menon 2009/Reimer 2007) p Interactions • Hadronuclear production – Cross section by fitting to data (Kafexhiu+ 2014) 10 105 105 102 102 10 1 10 1 − UHE− Proton Loss Lengths Energy104 Deposition & IGM/ISM Heating 4 4 10− 10− Mean Free Path of UHE Protons 103 10 7 10 7 − Contributions− Magnetic Field UHE Proton Loss Lengths 104 10 2 10 5 10− 10 10− 10102 103 1010-22 2 13 10 2 13 1 10− 10 1 10− 10− 10 10-8 4 10− 101 16 16 7 10− 10− 10− 100 0 Energy Loss Mean Free Path/Mpc 10 Energy Loss Mean Free Path/Mpc 10 10− 19 Hadronuclear (p⇡) 19 1 20 13 20 10− 10− 10− 10− Seed Magnetic Field,Galactic 10 Radiation− HadronuclearG Photopion (⇡) (p⇡) Seed Magnetic10-22 Field, 10− G 1 Galactic Radiation Photopair (γe) 10 16 102 − 5 − 5 10−-2 − − SaturationEnergy10 Loss Mean Free Path/Mpc Magnetic Field, 10 G Saturation Magnetic Field, 10 G 22 CMB RadiationGalactic Photopion (⇡) Radiation Photopion22 (⇡) Energy Loss Mean Free Path/Mpc 10− 10− 19 10− 20 CMB Radiation Photopair (γe) Seed Magnetic Field, 10− G 3 No Magnetic10− Field Galactic Radiation Photopair (γe) No Magnetic Field 5 CMB Radiation Cosmological Expansion 22 Saturation Magnetic Field, 10− G 2 10− 25 10− Total 25 No Magnetic Field 10− Energy Loss Mean Free Path/Mpc CMB Radiation Photopion10− (⇡) 4 25 9 10 1110− 12 13 14 15 9 16 10 17 1110−18 12 19 13 20 14 15 16 17 18 19 20 10 10 10 109 101010 1011 101012 1013 101014 1015101016 10101710 101810101019 102010 10 109101010 101110 101012 101013 1014 101015 1016 1017 1018 101019 1020 10 10 10 CMBProton RadiationProton Energy/eV Energy/eV Photopair (γe) ProtonProton Energy/eV Energy/eV 3 Owen+(in prep) 10− CMB Radiation Cosmological Expansion • AssumeTotal products decay quickly at interaction point 4 •10− Energy of CR deposited ~at point of interaction 109 1010 1011 1012 1013 1014 1015 1016 1017 1018 1019 1020 11 Proton Energy/eV 23 23 10− 10− 25 25 10− 10− 27 27 10− 10− 29 29 10− 10− 19 1 19 1 31 31 10− − 10− − 10− 10− s s 3 3 − − 33 Energy21 Deposition33 & IGM/ISM21 Heating 10− 10− 10− 10− 23 10− 35 35 Preliminary Estimated23 Heating Impact10− 25 23 10− 10− 10− 10− Local Scales 27 Large Scales 10− 37 37 19 10 23 10 10− − 10− − 25 29 25 1 10− 10− 1 1025− 10− − 21 10− − 1 Heating/erg cm s Heating/erg cm 31 s 39 − 10− 27 0Myr 39 s 10− 3 10 3 10 23 − 3 − 10− − − 27 33 − 10 29 27 1Myr 10 10− − 25− 10− 1 1 10− 31 10 Myr − − 10− s 41 s 41 35 3 3 10 − − 10− − 10−
Load more

Recommended publications
  • A Multimessenger View of Galaxies and Quasars from Now to Mid-Century M
    A multimessenger view of galaxies and quasars from now to mid-century M. D’Onofrio 1;∗, P. Marziani 2;∗ 1 Department of Physics & Astronomy, University of Padova, Padova, Italia 2 National Institute for Astrophysics (INAF), Padua Astronomical Observatory, Italy Correspondence*: Mauro D’Onofrio [email protected] ABSTRACT In the next 30 years, a new generation of space and ground-based telescopes will permit to obtain multi-frequency observations of faint sources and, for the first time in human history, to achieve a deep, almost synoptical monitoring of the whole sky. Gravitational wave observatories will detect a Universe of unseen black holes in the merging process over a broad spectrum of mass. Computing facilities will permit new high-resolution simulations with a deeper physical analysis of the main phenomena occurring at different scales. Given these development lines, we first sketch a panorama of the main instrumental developments expected in the next thirty years, dealing not only with electromagnetic radiation, but also from a multi-messenger perspective that includes gravitational waves, neutrinos, and cosmic rays. We then present how the new instrumentation will make it possible to foster advances in our present understanding of galaxies and quasars. We focus on selected scientific themes that are hotly debated today, in some cases advancing conjectures on the solution of major problems that may become solved in the next 30 years. Keywords: galaxy evolution – quasars – cosmology – supermassive black holes – black hole physics 1 INTRODUCTION: TOWARD MULTIMESSENGER ASTRONOMY The development of astronomy in the second half of the XXth century followed two major lines of improvement: the increase in light gathering power (i.e., the ability to detect fainter objects), and the extension of the frequency domain in the electromagnetic spectrum beyond the traditional optical domain.
    [Show full text]
  • An Overview of New Worlds, New Horizons in Astronomy and Astrophysics About the National Academies
    2020 VISION An Overview of New Worlds, New Horizons in Astronomy and Astrophysics About the National Academies The National Academies—comprising the National Academy of Sciences, the National Academy of Engineering, the Institute of Medicine, and the National Research Council—work together to enlist the nation’s top scientists, engineers, health professionals, and other experts to study specific issues in science, technology, and medicine that underlie many questions of national importance. The results of their deliberations have inspired some of the nation’s most significant and lasting efforts to improve the health, education, and welfare of the United States and have provided independent advice on issues that affect people’s lives worldwide. To learn more about the Academies’ activities, check the website at www.nationalacademies.org. Copyright 2011 by the National Academy of Sciences. All rights reserved. Printed in the United States of America This study was supported by Contract NNX08AN97G between the National Academy of Sciences and the National Aeronautics and Space Administration, Contract AST-0743899 between the National Academy of Sciences and the National Science Foundation, and Contract DE-FG02-08ER41542 between the National Academy of Sciences and the U.S. Department of Energy. Support for this study was also provided by the Vesto Slipher Fund. Any opinions, findings, conclusions, or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of the agencies that provided support for the project. 2020 VISION An Overview of New Worlds, New Horizons in Astronomy and Astrophysics Committee for a Decadal Survey of Astronomy and Astrophysics ROGER D.
    [Show full text]
  • The FIRST STARS in the UNIVERSE WERE TYPICALLY MANY TIMES More Massive and Luminous Than the Sun
    THEFIRST STARS IN THE UNIVERSE Exceptionally massive and bright, the earliest stars changed the course of cosmic history We live in a universe that is full of bright objects. On a clear night one can see thousands of stars with the naked eye. These stars occupy mere- ly a small nearby part of the Milky Way galaxy; tele- scopes reveal a much vaster realm that shines with the light from billions of galaxies. According to our current understanding of cosmology, howev- er, the universe was featureless and dark for a long stretch of its early history. The first stars did not appear until perhaps 100 million years after the big bang, and nearly a billion years passed before galaxies proliferated across the cosmos. Astron- BY RICHARD B. LARSON AND VOLKER BROMM omers have long wondered: How did this dramat- ILLUSTRATIONS BY DON DIXON ic transition from darkness to light come about? 4 SCIENTIFIC AMERICAN Updated from the December 2001 issue COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. EARLIEST COSMIC STRUCTURE mmostost likely took the form of a network of filaments. The first protogalaxies, small-scale systems about 30 to 100 light-years across, coalesced at the nodes of this network. Inside the protogalaxies, the denser regions of gas collapsed to form the first stars (inset). COPYRIGHT 2004 SCIENTIFIC AMERICAN, INC. After decades of study, researchers The Dark Ages to longer wavelengths and the universe have recently made great strides toward THE STUDY of the early universe is grew increasingly cold and dark. As- answering this question. Using sophisti- hampered by a lack of direct observa- tronomers have no observations of this cated computer simulation techniques, tions.
    [Show full text]
  • 15.1 Galaxy Formation: Introduction
    15.1 Galaxy Formation: Introduction Galaxy Formation • The early stages of galaxy evolution - but there is no clear-cut boundary, and it also has two principal aspects: assembly of the mass, and conversion of gas into stars • Must be related to large-scale (hierarchical) structure formation, plus the dissipative processes - it is a very messy process, much more complicated than LSS formation and growth • Probably closely related to the formation of the massive central black holes as well • Generally, we think of massive galaxy formation at high redshifts (z ~ 3 - 10, say); dwarfs may be still forming now • Observations have found populations of what must be young galaxies (ages < 1 Gyr), ostensibly progenitors of large galaxies today, at z ~ 5 - 7 • The frontier is now at z ~ 7 - 20, the so-called Reionization Era 2 A General Outline • The smallest scale density fluctuations keep collapsing, with baryons falling into the potential wells dominated by the dark matter, achieving high densties through cooling – This process starts right after the recombination at z ~ 1100 • Once the gas densities are high enough, star formation ignites – This probably happens around z ~ 20 - 30 – By z ~ 6, UV radiation from young galaxies reionizes the unverse • These protogalactic fragments keep merging, forming larger objects in a hierarchical fashion ever since then • Star formation enriches the gas, and some of it is expelled in the intergalactic medium, while more gas keeps falling in • If a central massive black hole forms, the energy release from accretion
    [Show full text]
  • Second Parameter Globulars and Dwarf Spheroidals Around the Local Group Massive Galaxies: What Can They Evidence?
    A&A 396, 117–123 (2002) Astronomy DOI: 10.1051/0004-6361:20021404 & c ESO 2002 Astrophysics Second parameter globulars and dwarf spheroidals around the Local Group massive galaxies: What can they evidence? V. K ravtsov Sternberg Astronomical Institute, University Avenue 13, 119899 Moscow, Russia Received 29 April 2002 / Accepted 28 August 2002 Abstract. We suggest that the majority of the “young”, so–called “second parameter” globular clusters (SPGCs) have origi- nated in the outer Galactic halo due to a process other than a tidal disruption of the dwarf spheroidal (dSph) galaxies. Basic observational evidence regarding both the dSphs and the SPGCs, coupled with the latest data about a rather large relative num- ber of such clusters among globulars in M 33 and their low portion in M 31, seems to be consistent with the suspected process. It might have taken place within the system of the most massive galaxies of the Local Group (LG) at the earliest stages of their formation and evolution. We argue that the origin and basic characteristics of the SPGCs can naturally be explained as a result of mass outflow from M 31, during and due to formation of its Pop. II stars, and subsequent accretion of gas onto its massive companions, the Galaxy and M 33. An amount of the gas accreted onto the Milky Way is expected to have been quite enough for the formation in the outer Galactic halo not only of the clusters under consideration but also a number of those dSph galaxies which are as young as the SPGCs. A less significant, but notable mass transfer from the starbursting protoGalaxy to the massive members of the LG might have occurred, too.
    [Show full text]
  • The First Galaxies
    First Galaxies 1 The First Galaxies Volker Bromm1 and Naoki Yoshida2 1 Department of Astronomy and Texas Cosmology Center, University of Texas, Austin, Texas 78712; email: [email protected] 2 Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583, Japan; email: [email protected] Key Words cosmology, galaxy formation, intergalactic medium, star formation, Population III Abstract We review our current understanding of how the first galaxies formed at the end of the cosmic dark ages, a few 100 million years after the Big Bang. Modern large telescopes discovered galaxies at redshifts greater than seven, whereas theoretical studies have just reached the degree of sophistication necessary to make meaningful predictions. A crucial ingredient is the feedback exerted by the first generation of stars, through UV radiation, supernova blast waves, and chemical enrichment. The key goal is to derive the signature of the first galaxies to be observed with upcoming or planned next-generation facilities, such as the James Webb Space Telescope or Atacama Large Millimeter Array. ¿From the observational side, ongoing deep-field searches for very high-redshift galaxies begin to provide us with empirical constraints on the nature of the first galaxies. CONTENTS INTRODUCTION .................................... 2 Annu. Rev. Astron. Astrophys. 2011 49 1056-8700/97/0610-00 WHAT IS A FIRST GALAXY? ............................ 6 Theoretical Perspective .................................... 7 Observational
    [Show full text]
  • The Never-Ending Realm of Galaxies
    The Multi-Bang Universe: The Never-Ending Realm of Galaxies Mário Everaldo de Souza Departamento de Física, Universidade Federal de Sergipe, 49.100-000, Brazil Abstract A new cosmological model is proposed for the dynamics of the Universe and the formation and evolution of galaxies. It is shown that the matter of the Universe contracts and expands in cycles, and that galaxies in a particu- lar cycle have imprints from the previous cycle. It is proposed that RHIC’s liquid gets trapped in the cores of galaxies in the beginning of each cycle and is liberated with time and is, thus, the power engine of AGNs. It is also shown that the large-scale structure is a permanent property of the Universe, and thus, it is not created. It is proposed that spiral galaxies and elliptical galaxies are formed by mergers of nucleon vortices (vorteons) at the time of the big squeeze and immediately afterwards and that the merging process, in general, lasts an extremely long time, of many billion years. It is concluded then that the Universe is eternal and that space should be infinite or almost. Keywords Big Bang, RHIC’s liquid, Galaxy Formation, Galaxy Evolution, LCDM Bang Theory: the universal expansion, the Cosmic Micro- 1. Introduction wave Background (CMB) radiation and Primordial or Big The article from 1924 by Alexander Friedmann "Über Bang Nucleosynthesis (BBN). Since then there have been die Möglichkeit einer Welt mit konstanter negativer several improvements in the measurements of the CMB Krümmung des Raumes" ("On the possibility of a world spectrum and its anisotropies by COBE [6], WMAP [7], with constant negative curvature of space") is the theoreti- and Planck 2013 [8].
    [Show full text]
  • Evolution of Proto-Galaxy-Clusters to Their Present Form: Theory and Observations
    Journal of Cosmology, 2010, 6, 1365-1384 Evolution of proto-galaxy-clusters … Gibson & Schild 1365 Evolution of proto-galaxy-clusters to their present form: theory and observations Carl H. Gibson 1,2 1 University of California San Diego, La Jolla, CA 92093-0411, USA [email protected], http://sdcc3.ucsd.edu/~ir118 and Rudolph E. Schild3,4 3 Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4 [email protected] ABSTRACT From hydro-gravitational-dynamics theory HGD, gravitational structure formation begins 30,000 years (1012 s) after the turbulent big bang by viscous-gravitational fragmentation into super-cluster-voids and 1046 kg proto-galaxy-super-clusters. Linear and spiral gas- proto-galaxies GPGs are the smallest fragments to emerge from the plasma epoch at de- 13 1/2 coupling at 10 s with Nomura turbulence morphology and length scale LN ~ (/G) ~1020 m, determined by rate-of-strain , photon viscosity , and density of the plasma fossilized at 1012 s. GPGs fragment into 1036 kg proto-globular-star-cluster PGC clumps of 1024 kg primordial-fog-particle PFP dark matter planets. All stars form from planet mergers, with ~97% unmerged as galaxy baryonic-dark-matter BDM. The non-baryonic- dark-matter NBDM is so weakly collisional it diffuses to form galaxy cluster halos. It does not guide galaxy formation, contrary to conventional cold-dark-matter hierarchical clustering CDMHC theory (=0). NBDM has ~97% of the mass of the universe. It binds rotating clusters of galaxies by gravitational forces. The galaxy rotational spin axis matches that for low wavenumber spherical harmonic components of CMB temperature anomalies and extends to 4.5x1025 m (1.5 Gpc) in quasar polarization vectors, requiring a big bang turbulence origin.
    [Show full text]
  • The Galaxy Environment of Quasars in the Clowes-Campusano Large Quasar Group
    The Galaxy Environment of Quasars in the Clowes-Campusano Large Quasar Group Christopher Paul Haines A thesis submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy. Centre for Astrophysics Department of Physics, Astronomy and Mathematics University of Central Lancashire June 2001 Declaration The work presented in this thesis was carried out in the Department of Physics, Astromony and Mathematics, University of Central Lancashire. Unless otherwise stated it is the original work of the author. While registered for the degree of Doctor of Philosophy, the author has not been a registered candidate for another award of the University. This thesis has not been submitted in whole, or in part, for any other degree. Christopher Haines June 2001 Abstract Quasars have been used as efficient probes of high-redshift galaxy clustering as they are known to favour overdense environments. Quasars may also trace the large- scale structure of the early universe (0.4 1< z 1< 2) in the form of Large Quasar Groups (LQGs), which have comparable sizes (r.J 100-200hMpc) to the largest structures seen at the present epoch. This thesis describes an ultra-deep, wide-field optical study of a region containing three quasars from the largest known LJQG, the Clowes-Campusano LQG of at least 18 quasars at z 1.3, to examine their galaxy environments and to find indications of any associated large-scale structure in the form of galaxies. The optical data were obtained using the Big Throughput Camera (BTC) on the 4-m Blanco telescope at the Cerro Tololo Interamerican Observatory (CTIO) over two nights in April 1998, resulting in ultra-deep V, I imaging of a 40.6 x 34.9 arcmin 2 field centred at l0L47m30s, +05 0 30'00" containing three quasars from the LQG as well as four quasars at higher redshifts.
    [Show full text]
  • Hampton Cove Middle School
    James Webb Space Telescope (JWST) The First Light Machine Who is James Webb? James E Webb was the first administrator of NASA (1961 to 1968) He supported a program balanced between Science and Human Exploration. credit: NASA 1 What is FIRST LIGHT? End of the dark ages: first light and reionization What are the first luminous objects? What are the first galaxies? How did black holes form and interact with their host galaxies? When did re-ionization of the inter-galactic medium occur? What caused the re-ionization? … to identify the first luminous sources to form and to determine the ionization history of the early universe. Hubble Ultra Deep Field A Brief History of Time Planets, Life & Galaxies Intelligence First Galaxies Evolve Form Atoms & Radiation Particle Physics Big Today Bang 3 minutes 300,000 years 100 million years 1 billion COBE years 13.7 Billion years MAP JWST HST Ground Based Observatories 2 First Light Stars 50-to-100 million years after the Big Bang, the first massive stars started to form from clouds of hydrogen. But, because they were so large, they were unstable and either exploded supernova or collapsed into black holes. These first stars helped ionize the universe and created elements such as He. O-class stars are 25X larger than our sun. ‘First’ stars may have been 1000X larger. The (modern) Morgan–Keenan spectral classification system, with the temperature range of each star class shown above it, in kelvin. The overwhelming majority of stars today are M-class stars, with only 1 known O- or B-class star within 25 parsecs.
    [Show full text]
  • Starburst and Post-Starburst High-Redshift Protogalaxies the Feedback Impact of High Energy Cosmic Rays
    A&A 626, A85 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834350 & c ESO 2019 Astrophysics Starburst and post-starburst high-redshift protogalaxies The feedback impact of high energy cosmic rays Ellis R. Owen1,2, Kinwah Wu1,3, Xiangyu Jin4,5, Pooja Surajbali6, and Noriko Kataoka1,7 1 Mullard Space Science Laboratory, University College London, Dorking, Surrey RH5 6NT, UK e-mail: [email protected] 2 Institute of Astronomy, Department of Physics, National Tsing Hua University, Hsinchu, Taiwan (ROC) 3 School of Physics, University of Sydney, Camperdown, NSW 2006, Australia 4 School of Physics, Nanjing University, Nanjing 210023, PR China 5 Department of Physics and McGill Space Institute, McGill University, 3600 University St., Montreal, QC H3A 2T8, Canada 6 Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, Heidelberg 69117, Germany 7 Department of Physics, Faculty of Science, Kyoto Sangyo University, Kyoto 603-8555, Japan Received 1 October 2018 / Accepted 27 April 2019 ABSTRACT Quenching of star-formation has been identified in many starburst and post-starburst galaxies, indicating burst-like star-formation histories (SFH) in the primordial Universe. Galaxies undergoing violent episodes of star-formation are expected to be rich in high energy cosmic rays (CRs). We have investigated the role of these CRs in such environments, particularly how they could contribute to this burst-like SFH via quenching and feedback. These high energy particles interact with the baryon and radiation fields of their host via hadronic processes to produce secondary leptons. The secondary particles then also interact with ambient radiation fields to generate X-rays through inverse-Compton scattering.
    [Show full text]
  • A Scientific Proaram for Infrared, Submillimeter and Radio
    NiNIAL L• A Scientific Proaram for " Infrared, Submillimeter and Radio Astronomy From Space A Report by the Management Operations Working Group June 1989 An IRAS image of a 90 x 90 region of the Chamaeleon molecular cloud shows stars younger than 1 Q5 yr forming out of dense molecular gas. The color coding is such that 12 Am emission is blue, 60 Am emission is green, and 100 /2m emission is red. Hot stars appear blue, while embedded protostars appear orange or white. A Scientific Program for Infrared, Submillimeter and Radio Astronomy From Space A report by the Management Operations Working Group C. Beichman (Caltech and JPL), Chairman L. Allamandola (NASA Ames) F. Gillett (NASA HO and NOAO) E. E. Becklin (U. Hawaii) N. Boggess (Goddard) D.Hollenbach (NASA Ames) D.H. Harper (Yerkes) J. Houck (Cornell) T. Herter (Cornell) H. Moseley (Goddard) K. Kellermann (NRAO) P. Richards (Berkeley) S. Meyer (MIT) R. Wilson (AT&T Bell Labs) P. Thaddeus (Harvard) E.T. Young (U. Arizona) E.L. Wright (UCLA) L. Caroff (NASA HQ and Ames) June 1989 TABLE OF CONTENTS Page Executive Summary 1 Introduction 5 Long Wavelength .Science: The Formation of the Universe, Galaxies, Stars, Solar Systems, and Life 10 Origin of Stars and Planets 11 The Origin and Evolution of Matter and Life 16 Origin and Evolution of Galaxies 21 Evolution of the Universe 27 Serendipity 29 Complementarity with HST, AXAF, and GAO 30 Criteria for a Balanced Program 31 Science 31 Technology 32 Community Support and Development 33 Infrastructure 34 The Program 35 The Highest Priority Missions: SIRTF and SOFIA 35 LDR and Submillimeter Astronomy 37 Smaller Missions 38 International Cooperation 39 Supporting Research Activities 40 Conclusions 44 Acknowledgements 45 EXECUTIVE SUMMARY - Important and fundamental scientific progress can be attained through space observa- tions in the wavelengths longward of 1 j.zm.
    [Show full text]