The Large Scale Universe As a Quasi Quantum White Hole
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A Revised View of the Canis Major Stellar Overdensity with Decam And
MNRAS 501, 1690–1700 (2021) doi:10.1093/mnras/staa2655 Advance Access publication 2020 October 14 A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars Downloaded from https://academic.oup.com/mnras/article/501/2/1690/5923573 by Consejo Superior de Investigaciones Cientificas (CSIC) user on 15 March 2021 Julio A. Carballo-Bello ,1‹ David Mart´ınez-Delgado,2 Jesus´ M. Corral-Santana ,3 Emilio J. Alfaro,2 Camila Navarrete,3,4 A. Katherina Vivas 5 and Marcio´ Catelan 4,6 1Instituto de Alta Investigacion,´ Universidad de Tarapaca,´ Casilla 7D, Arica, Chile 2Instituto de Astrof´ısica de Andaluc´ıa, CSIC, E-18080 Granada, Spain 3European Southern Observatory, Alonso de Cordova´ 3107, Casilla 19001, Santiago, Chile 4Millennium Institute of Astrophysics, Santiago, Chile 5Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, Chile 6Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 782-0436 Macul, Santiago, Chile Accepted 2020 August 27. Received 2020 July 16; in original form 2020 February 24 ABSTRACT We present the Dark Energy Camera (DECam) imaging combined with Gaia Data Release 2 (DR2) data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the colour–magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and in the range 230◦ <<255◦. -
Complex Stellar Populations in Massive Clusters: Trapping Stars of a Dwarf Disc Galaxy in a Newborn Stellar Supercluster
Mon. Not. R. Astron. Soc. 372, 338–342 (2006) doi:10.1111/j.1365-2966.2006.10867.x Complex stellar populations in massive clusters: trapping stars of a dwarf disc galaxy in a newborn stellar supercluster M. Fellhauer,1,3⋆ P. Kroupa2,3⋆ and N. W. Evans1⋆ 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA 2Argelander Institute for Astronomy, University of Bonn, Auf dem Hug¨ el 71, D-53121 Bonn, Germany 3The Rhine Stellar-Dynamical Network Accepted 2006 July 24. Received 2006 July 21; in original form 2006 April 27 ABSTRACT Some of the most-massive globular clusters of our Milky Way, such as, for example, ω Centauri, show a mixture of stellar populations spanning a few Gyr in age and 1.5 dex in metallicities. In contrast, standard formation scenarios predict that globular and open clusters form in one single starburst event of duration 10 Myr and therefore should exhibit only one age and one metallicity in its stars. Here, we investigate the possibility that a massive stellar supercluster may trap older galactic field stars during its formation process that are later detectable in the cluster as an apparent population of stars with a very different age and metallicity. With a set of numerical N-body simulations, we are able to show that, if the mass of the stellar supercluster is high enough and the stellar velocity dispersion in the cluster is comparable to the dispersion of the surrounding disc stars in the host galaxy, then up to about 40 per cent of its initial mass can be additionally gained from trapped disc stars. -
The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia
MNRAS 000,1{20 (2019) Preprint 14 November 2019 Compiled using MNRAS LATEX style file v3.0 The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia DR2 Marcel S. Pawlowski,1? and Pavel Kroupa2;3 1Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany 2Helmholtz-Institut fur¨ Strahlen- und Kernphysik, University of Bonn, Nussallee 14-16, D- 53115 Bonn, Germany 3Charles University in Prague, Faculty of Mathematics and Physics, Astronomical Institute, V Holeˇsoviˇck´ach 2, CZ-180 00 Praha 8, Czech Republic Accepted 2019 November 7. Received 2019 November 7; in original form 2019 August 26 ABSTRACT We study the correlation of orbital poles of the 11 classical satellite galaxies of the Milky Way, comparing results from previous proper motions with the independent data by Gaia DR2. Previous results on the degree of correlation and its significance are confirmed by the new data. A majority of the satellites co-orbit along the Vast Polar Structure, the plane (or disk) of satellite galaxies defined by their positions. The orbital planes of eight satellites align to < 20◦ with a common direction, seven even orbit in the same sense. Most also share similar specific angular momenta, though their wide distribution on the sky does not support a recent group infall or satellites- of-satellites origin. The orbital pole concentration has continuously increased as more precise proper motions were measured, as expected if the underlying distribution shows true correlation that is washed out by observational uncertainties. The orbital poles of the up to seven most correlated satellites are in fact almost as concentrated as expected for the best-possible orbital alignment achievable given the satellite posi- tions. -
VI. Star-Forming Companions of Nearby Field Galaxies
A&A 486, 131–142 (2008) Astronomy DOI: 10.1051/0004-6361:20079297 & c ESO 2008 Astrophysics The Hα Galaxy Survey VI. Star-forming companions of nearby field galaxies P. A. James1, J. O’Neill2, and N. S. Shane1,3 1 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK e-mail: [email protected] 2 Wirral Grammar School for Girls, Heath Road, Bebington, Wirral CH63 3AF, UK 3 Planetary Science Group, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK Received 20 December 2007 / Accepted 5 May 2008 ABSTRACT Aims. We searched for star-forming satellite galaxies that are close enough to their parent galaxies to be considered analogues of the Magellanic Clouds. Methods. Our search technique relied on the detection of the satellites in continuum-subtracted narrow-band Hα imaging of the central galaxies, which removes most of the background and foreground line-of-sight companions, thus giving a high probability that we are detecting true satellites. The search was performed for 119 central galaxies at distances between 20 and 40 Mpc, although spatial incompleteness means that we have effectively searched 53 full satellite-containing volumes. Results. We find only 9 “probable” star-forming satellites, around 9 different central galaxies, and 2 more “possible” satellites. After incompleteness correction, this is equivalent to 0.17/0.21 satellites per central galaxy. This frequency is unchanged whether we consider all central galaxy types or just those of Hubble types S0a–Sc, i.e. only the more luminous and massive spiral types. -
Introduction to Astronomy from Darkness to Blazing Glory
Introduction to Astronomy From Darkness to Blazing Glory Published by JAS Educational Publications Copyright Pending 2010 JAS Educational Publications All rights reserved. Including the right of reproduction in whole or in part in any form. Second Edition Author: Jeffrey Wright Scott Photographs and Diagrams: Credit NASA, Jet Propulsion Laboratory, USGS, NOAA, Aames Research Center JAS Educational Publications 2601 Oakdale Road, H2 P.O. Box 197 Modesto California 95355 1-888-586-6252 Website: http://.Introastro.com Printing by Minuteman Press, Berkley, California ISBN 978-0-9827200-0-4 1 Introduction to Astronomy From Darkness to Blazing Glory The moon Titan is in the forefront with the moon Tethys behind it. These are two of many of Saturn’s moons Credit: Cassini Imaging Team, ISS, JPL, ESA, NASA 2 Introduction to Astronomy Contents in Brief Chapter 1: Astronomy Basics: Pages 1 – 6 Workbook Pages 1 - 2 Chapter 2: Time: Pages 7 - 10 Workbook Pages 3 - 4 Chapter 3: Solar System Overview: Pages 11 - 14 Workbook Pages 5 - 8 Chapter 4: Our Sun: Pages 15 - 20 Workbook Pages 9 - 16 Chapter 5: The Terrestrial Planets: Page 21 - 39 Workbook Pages 17 - 36 Mercury: Pages 22 - 23 Venus: Pages 24 - 25 Earth: Pages 25 - 34 Mars: Pages 34 - 39 Chapter 6: Outer, Dwarf and Exoplanets Pages: 41-54 Workbook Pages 37 - 48 Jupiter: Pages 41 - 42 Saturn: Pages 42 - 44 Uranus: Pages 44 - 45 Neptune: Pages 45 - 46 Dwarf Planets, Plutoids and Exoplanets: Pages 47 -54 3 Chapter 7: The Moons: Pages: 55 - 66 Workbook Pages 49 - 56 Chapter 8: Rocks and Ice: -
Midwife of the Galactic Zoo
FOCUS 30 A miniature milky way: approximately 40 million light-years away, UGC 5340 is classified as a dwarf galaxy. Dwarf galaxies exist in a variety of forms – elliptical, spheroidal, spiral, or irregular – and originate in small halos of dark matter. Dwarf galaxies contain the oldest known stars. Max Planck Research · 4 | 2020 FOCUS MIDWIFE OF THE GALACTIC ZOO TEXT: THOMAS BÜHRKE 31 IMAGE: NASA, TEAM ESA & LEGUS Stars cluster in galaxies of dramatically different shapes and sizes: elliptical galaxies, spheroidal galaxies, lenticular galaxies, spiral galaxies, and occasionally even irregular galaxies. Nadine Neumayer at the Max Planck Institute for Astronomy in Heidelberg and Ralf Bender at the Max Planck Institute for Extraterrestrial Physics in Garching investigate the reasons for this diversity. They have already identified one crucial factor: dark matter. Max Planck Research · 4 | 2020 FOCUS Nature has bestowed an overwhelming diversity upon our planet. The sheer resourcefulness of the plant and animal world is seemingly inexhaustible. When scien- tists first started to explore this diversity, their first step was always to systematize it. Hence, the Swedish naturalist Carl von Linné established the principles of modern botany and zoology in the 18th century by clas- sifying organisms. In the last century, astronomers have likewise discovered that galaxies can come in an array of shapes and sizes. In this case, it was Edwin Hubble in the mid-1920s who systematized them. The “Hubble tuning fork dia- gram” classified elliptical galaxies according to their ellipticity. The series of elliptical galaxies along the di- PHOTO: PETER FRIEDRICH agram branches off into two arms: spiral galaxies with a compact bulge along the upper branch and galaxies with a central bar on the lower branch. -
Habitability on Local, Galactic and Cosmological Scales
Habitability on local, Galactic and cosmological scales Luigi Secco1 • Marco Fecchio1 • Francesco Marzari1 Abstract The aim of this paper is to underline con- detectable studying our site. The Climatic Astronom- ditions necessary for the emergence and development ical Theory is introduced in sect.5 in order to define of life. They are placed at local planetary scale, at the circumsolar habitable zone (HZ) (sect.6) while the Galactic scale and within the cosmological evolution, translation from Solar to extra-Solar systems leads to a as pointed out by the Anthropic Cosmological Princi- generalized circumstellar habitable zone (CHZ) defined ple. We will consider the circumstellar habitable zone in sect.7 with some exemplifications to the Gliese-667C (CHZ) for planetary systems and a Galactic Habitable and the TRAPPIST-1 systems; some general remarks Zone (GHZ) including also a set of strong cosmologi- follow (sect.8). A first conclusion related to CHZ is cal constraints to allow life (cosmological habitability done moving toward GHZ and COSH (sect.9). The (COSH)). Some requirements are specific of a single conditions for the development of life are indeed only scale and its related physical phenomena, while others partially connected to the local scale in which a planet are due to the conspired effects occurring at more than is located. A strong interplay between different scales one scale. The scenario emerging from this analysis is exists and each single contribution to life from individ- that all the habitability conditions here detailed must ual scales is difficult to be isolated. However we will at least be met. -
Modeling and Interpretation of the Ultraviolet Spectral Energy Distributions of Primeval Galaxies
Ecole´ Doctorale d'Astronomie et Astrophysique d'^Ile-de-France UNIVERSITE´ PARIS VI - PIERRE & MARIE CURIE DOCTORATE THESIS to obtain the title of Doctor of the University of Pierre & Marie Curie in Astrophysics Presented by Alba Vidal Garc´ıa Modeling and interpretation of the ultraviolet spectral energy distributions of primeval galaxies Thesis Advisor: St´ephane Charlot prepared at Institut d'Astrophysique de Paris, CNRS (UMR 7095), Universit´ePierre & Marie Curie (Paris VI) with financial support from the European Research Council grant `ERC NEOGAL' Composition of the jury Reviewers: Alessandro Bressan - SISSA, Trieste, Italy Rosa Gonzalez´ Delgado - IAA (CSIC), Granada, Spain Advisor: St´ephane Charlot - IAP, Paris, France President: Patrick Boisse´ - IAP, Paris, France Examinators: Jeremy Blaizot - CRAL, Observatoire de Lyon, France Vianney Lebouteiller - CEA, Saclay, France Dedicatoria v Contents Abstract vii R´esum´e ix 1 Introduction 3 1.1 Historical context . .4 1.2 Early epochs of the Universe . .5 1.3 Galaxytypes ......................................6 1.4 Components of a Galaxy . .8 1.4.1 Classification of stars . .9 1.4.2 The ISM: components and phases . .9 1.4.3 Physical processes in the ISM . 12 1.5 Chemical content of a galaxy . 17 1.6 Galaxy spectral energy distributions . 17 1.7 Future observing facilities . 19 1.8 Outline ......................................... 20 2 Modeling spectral energy distributions of galaxies 23 2.1 Stellar emission . 24 2.1.1 Stellar population synthesis codes . 24 2.1.2 Evolutionary tracks . 25 2.1.3 IMF . 29 2.1.4 Stellar spectral libraries . 30 2.2 Absorption and emission in the ISM . 31 2.2.1 Photoionization code: CLOUDY ....................... -
Basic Interactions in Black Hole Cosmology
American Journal of Astronomy and Astrophysics 2014; 2(1): 6-17 Published online February 20, 2014 (http://www.sciencepublishinggroup.com/j/ajaa) doi: 10.11648/j.ajaa.20140201.12 Basic interactions in black hole cosmology U. V. S. Seshavatharam 1, S. Lakshminarayana 2 1Honorary faculty, I-SERVE, Alakapuri, Hyderabad-35, AP, India 2Dept. of Nuclear Physics, Andhra University, Visakhapatnam-03, AP, India Email address: [email protected] (U. V. S. Seshavatharam), [email protected] (S. Lakshminarayana) To cite this article: U. V. S. Seshavatharam, S. Lakshminarayana. Basic Interactions in Black Hole Cosmology. American Journal of Astronomy and Astrophysics. Vol. 2, No. 1, 2013, pp. 6-17. doi: 10.11648/j.ajaa.20140201.12 Abstract: By highlighting the 12 major shortcomings of modern big bang cosmology and reinterpreting the cosmic redshift as a galactic atomic emission phenomenon, the authors made an attempt to develop a possible model of Black hole cosmology in a constructive way. Its validity can be well confirmed from a combined study of cosmological and microscopic physical phenomena. It can be suggested that, there exists one variable physical quantity in the presently believed atomic and nuclear physical constants and “rate of change” in its magnitude can be considered as a “standard measure” of the present “cosmic rate of expansion”. The characteristic nuclear charge radius, inverse of the Fine structure ratio, the characteristic reduced Planck’s constant seem to increase with cosmic time and there will be no change in the magnitude of Planck's constant. At any cosmic time, ’Hubble length’ can be considered as the gravitational or electromagnetic interaction range. -
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Online ISSN: 2249-4626 Print ISSN: 0975-5896 Strong Absorption Model Pulsejet Engine Exhaust Gravitational Field Deducing Scope of General Theory VOLUME 14 ISSUE 4 VERSION 1.0 Global Journal of Science Frontier Research: A Physics & Space Science Global Journal of Science Frontier Research: A Physics & Space Science Volume 14 Issue 4 (Ver. 1.0) Open Association of Research Society © Global Journal of Science Global Journals Inc. Frontier Research. 2014 . (A Delaware USA Incorporation with “Good Standing”; Reg. Number: 0423089) Sponsors: Open Association of Research Society All rights reserved. Open Scientific Standards This is a special issue published in version 1.0 of “Global Journal of Science Frontier Publisher’s Headquarters office Research.” By Global Journals Inc. All articles are open access articles distributed Global Journals Headquarters under “Global Journal of Science Frontier 301st Edgewater Place Suite, 100 Edgewater Dr.-Pl, Research” Wakefield MASSACHUSETTS, Pin: 01880, Reading License, which permits restricted use. United States of America Entire contents are copyright by of “Global Journal of Science Frontier Research” unless USA Toll Free: +001-888-839-7392 otherwise noted on specific articles. USA Toll Free Fax: +001-888-839-7392 No part of this publication may be reproduced Offset Typesetting or transmitted in any form or by any means, electronic or mechanical, including photocopy, recording, or any information Global Journals Incorporated storage and retrieval system, without written 2nd, Lansdowne, Lansdowne Rd., Croydon-Surrey, permission. Pin: CR9 2ER, United Kingdom The opinions and statements made in this book are those of the authors concerned. Packaging & Continental Dispatching Ultraculture has not verified and neither confirms nor denies any of the foregoing and no warranty or fitness is implied. -
An Introduction to Our Universe
An Introduction to Our Universe Lyman Page Princeton, NJ [email protected] Draft, August 31, 2018 The full-sky heat map of the temperature differences in the remnant light from the birth of the universe. From the bluest to the reddest corresponds to a temperature difference of 400 millionths of a degree Celsius. The goal of this essay is to explain this image and what it tells us about the universe. 1 Contents 1 Preface 2 2 Introduction to Cosmology 3 3 How Big is the Universe? 4 4 The Universe is Expanding 10 5 The Age of the Universe is Finite 15 6 The Observable Universe 17 7 The Universe is Infinite ?! 17 8 Telescopes are Like Time Machines 18 9 The CMB 20 10 Dark Matter 23 11 The Accelerating Universe 25 12 Structure Formation and the Cosmic Timeline 26 13 The CMB Anisotropy 29 14 How Do We Measure the CMB? 36 15 The Geometry of the Universe 40 16 Quantum Mechanics and the Seeds of Cosmic Structure Formation. 43 17 Pulling it all Together with the Standard Model of Cosmology 45 18 Frontiers 48 19 Endnote 49 A Appendix A: The Electromagnetic Spectrum 51 B Appendix B: Expanding Space 52 C Appendix C: Significant Events in the Cosmic Timeline 53 D Appendix D: Size and Age of the Observable Universe 54 1 1 Preface These pages are a brief introduction to modern cosmology. They were written for family and friends who at various times have asked what I work on. The goal is to convey a geometrical picture of how to think about the universe on the grandest scales. -
Three Strongly Lensed Images of a Candidate Z 11 Galaxy
Accepted for publication in the Astrophysical Journal, Monday 29th October, 2012 Preprint typeset using LATEX style emulateapj v. 5/2/11 CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY Dan Coe1, Adi Zitrin2, Mauricio Carrasco2,3, Xinwen Shu4, Wei Zheng5, Marc Postman1, Larry Bradley1, Anton Koekemoer1, Rychard Bouwens6, Tom Broadhurst7,8, Anna Monna9, Ole Host10,11, Leonidas A. Moustakas12, Holland Ford5, John Moustakas13, Arjen van der Wel14, Megan Donahue15, Steven A. Rodney5, Narciso Ben´ıtez16, Stephanie Jouvel10,17, Stella Seitz9,18, Daniel D. Kelson19, and Piero Rosati20 Accepted for publication in the Astrophysical Journal, Monday 29th October, 2012 ABSTRACT We present a candidate for the most distant galaxy known to date with a photometric redshift +0:6 z = 10:7−0:4 (95% confidence limits; with z < 9:5 galaxies of known types ruled out at 7.2-σ). This J-dropout Lyman Break Galaxy, named MACS0647-JD, was discovered as part of the Cluster Lensing and Supernova survey with Hubble (CLASH). We observe three magnified images of this galaxy due to strong gravitational lensing by the galaxy cluster MACSJ0647.7+7015 at z = 0:591. The images are magnified by factors of ∼8, 7, and 2, with the brighter two observed at ∼26th magnitude AB (∼0.15µJy) in the WFC3/IR F160W filter (∼1.4{1.7µm) where they are detected at &12-σ. All three images are also confidently detected at &6-σ in F140W (∼1.2{1.6µm), dropping out of detection from 15 lower wavelength HST filters (∼0.2{1.4µm), and lacking bright detections in Spitzer/IRAC 3.6µm and 4.5µm imaging (∼3.2{5.0µm).