Some Astrophysical and Cosmological Findings from TGD Point of View
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Constructing a Galactic Coordinate System Based on Near-Infrared and Radio Catalogs
A&A 536, A102 (2011) Astronomy DOI: 10.1051/0004-6361/201116947 & c ESO 2011 Astrophysics Constructing a Galactic coordinate system based on near-infrared and radio catalogs J.-C. Liu1,2,Z.Zhu1,2, and B. Hu3,4 1 Department of astronomy, Nanjing University, Nanjing 210093, PR China e-mail: [jcliu;zhuzi]@nju.edu.cn 2 key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, PR China 3 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China 4 Graduate School of Chinese Academy of Sciences, Beijing 100049, PR China e-mail: [email protected] Received 24 March 2011 / Accepted 13 October 2011 ABSTRACT Context. The definition of the Galactic coordinate system was announced by the IAU Sub-Commission 33b on behalf of the IAU in 1958. An unrigorous transformation was adopted by the Hipparcos group to transform the Galactic coordinate system from the FK4-based B1950.0 system to the FK5-based J2000.0 system or to the International Celestial Reference System (ICRS). For more than 50 years, the definition of the Galactic coordinate system has remained unchanged from this IAU1958 version. On the basis of deep and all-sky catalogs, the position of the Galactic plane can be revised and updated definitions of the Galactic coordinate systems can be proposed. Aims. We re-determine the position of the Galactic plane based on modern large catalogs, such as the Two-Micron All-Sky Survey (2MASS) and the SPECFIND v2.0. This paper also aims to propose a possible definition of the optimal Galactic coordinate system by adopting the ICRS position of the Sgr A* at the Galactic center. -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties. -
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 ....................... -
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. -
Arxiv:1802.07727V1 [Astro-Ph.HE] 21 Feb 2018 Tion Systems to Standard Candles in Cosmology (E.G., Wijers Et Al
Astronomy & Astrophysics manuscript no. XSGRB_sample_arxiv c ESO 2018 2018-02-23 The X-shooter GRB afterglow legacy sample (XS-GRB)? J. Selsing1;??, D. Malesani1; 2; 3,y, P. Goldoni4,y, J. P. U. Fynbo1; 2,y, T. Krühler5,y, L. A. Antonelli6,y, M. Arabsalmani7; 8, J. Bolmer5; 9,y, Z. Cano10,y, L. Christensen1, S. Covino11,y, P. D’Avanzo11,y, V. D’Elia12,y, A. De Cia13, A. de Ugarte Postigo1; 10,y, H. Flores14,y, M. Friis15; 16, A. Gomboc17, J. Greiner5, P. Groot18, F. Hammer14, O.E. Hartoog19,y, K. E. Heintz1; 2; 20,y, J. Hjorth1,y, P. Jakobsson20,y, J. Japelj19,y, D. A. Kann10,y, L. Kaper19, C. Ledoux9, G. Leloudas1, A.J. Levan21,y, E. Maiorano22, A. Melandri11,y, B. Milvang-Jensen1; 2, E. Palazzi22, J. T. Palmerio23,y, D. A. Perley24,y, E. Pian22, S. Piranomonte6,y, G. Pugliese19,y, R. Sánchez-Ramírez25,y, S. Savaglio26, P. Schady5, S. Schulze27,y, J. Sollerman28, M. Sparre29,y, G. Tagliaferri11, N. R. Tanvir30,y, C. C. Thöne10, S.D. Vergani14,y, P. Vreeswijk18; 26,y, D. Watson1; 2,y, K. Wiersema21; 30,y, R. Wijers19, D. Xu31,y, and T. Zafar32 (Affiliations can be found after the references) Received/ accepted ABSTRACT In this work we present spectra of all γ-ray burst (GRB) afterglows that have been promptly observed with the X-shooter spectrograph until 31=03=2017. In total, we obtained spectroscopic observations of 103 individual GRBs observed within 48 hours of the GRB trigger. Redshifts have been measured for 97 per cent of these, covering a redshift range from 0.059 to 7.84. -
Planck: Dust Emission in Galactic Environments
Planck’s impact on interstellar medium science new insights and new directions Peter Martin CITA, University of Toronto On behalf of the Planck collaboration Perspective Wasted opportunity Fractionally, there are not many baryons, and even though Planck has given us a bit more, still most of these baryons are not in galaxies. Extragalactic context: Ellipticals Elliptical galaxies: red and dead. Very little ISM: gas and dust used up and/or expelled. NGC 4660 in the Virgo Cluster Hubble Space Telescope Elliptical envy With no ISM – no Galactic foregrounds – imagine the clear view of the CMB from inside such a galaxy! Galactic centre microwave haze Planck intermediate results. IX. Detection of the Galactic haze with Planck Here be monsters Non-thermal emission. Relativistic particles. Extragalactic context: Spirals Spiral galaxies: gas and dust available in an ISM for ongoing star formation NGC 3982 HST Dusty disk – like we live in Spiral galaxy: edge on, dust lane In our Galaxy, a foreground to the CMB. NGC 4565 CFHT An overarching question in interstellar medium (ISM) science Why is there still an ISM in the Milky Way in which stars are continually forming? How does the Milky Way tick? Curious Expeditions: Augustinian friar’s astrological clock. Spirals: gratitude Would we be able to figure out, ab initio and theoretically, how stars form, if we did not have an ISM “up close” in the Galaxy and so the empirical evidence and constraints? Or more to the point, could we answer why star formation is so disruptive of the ISM and so inefficient? Or would we have any fun at all? An ISM research program Galactic ecology: the cycling of the ISM from the diffuse atomic phase to dense molecular clouds, the sites of star formation/evolution, and back. -
Error in Modern Astronomy
Error in Modern Astronomy Eric Su [email protected] https://sites.google.com/view/physics-news/home (Dated: August 1, 2019) The conservation of the interference pattern from double slit interference proves that the wave- length is conserved in all inertial reference frames. However, there is a popular belief in modern astronomy that the wavelength can be changed by the choice of reference frame. This erroneous belief results in the problematic prediction of the radial speed of galaxy. The reflection symmetry shows that the elapsed time is conserved in all inertial reference frames. From both conservation properties, the velocity of the light is proved to be different in a different reference frame. This different velocity was confirmed by lunar laser ranging test at NASA in 2009. The relative motion between the light source and the light detector bears great similarity to the magnetic force on a moving charge. The motion changes the interference pattern but not the wavelength in the rest frame of the star. This is known as the blueshift or the redshift in astronomy. The speed of light in the rest frame of the grism determines how the spectrum is shifted. Wide Field Camera 3 in Hubble Space Telescope provides an excellent example on how the speed of light can change the spectrum. I. INTRODUCTION location of the light band is y1. The separation between the parallel slits is d1. The double slit interference can be formulated with the If d1 << y1 and d1 << D1, the constructive interfer- principle of superposition[1]. The interference pattern is ence can be described by the equation of phase shift[1] a function of the incident wavelength. -
New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope&amp;#39;s view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way. -
Structure, Kinematics and Dynamics of the Galaxy
Outline Structure of the Galaxy Kinematics of the Galaxy Galactic dynamics STRUCTURE OF GALAXIES 1. Structure, kinematics and dynamics of the Galaxy Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands February 2010 Piet van der Kruit, Kapteyn Astronomical Institute Structure, kinematics and dynamics of the Galaxy Outline Structure of the Galaxy Kinematics of the Galaxy Galactic dynamics Outline Structure of the Galaxy History All-sky pictures Kinematics of the Galaxy Differential rotation Local approximations and Oort constants Rotation curves and mass distributions Galactic dynamics Fundamental equations Epicycle orbits Vertical motion Piet van der Kruit, Kapteyn Astronomical Institute Structure, kinematics and dynamics of the Galaxy Outline Structure of the Galaxy History Kinematics of the Galaxy All-sky pictures Galactic dynamics Structure of the Galaxy Piet van der Kruit, Kapteyn Astronomical Institute Structure, kinematics and dynamics of the Galaxy Outline Structure of the Galaxy History Kinematics of the Galaxy All-sky pictures Galactic dynamics History Our Galaxy can be seen on the sky as the Milky Way, a band of faint light. Piet van der Kruit, Kapteyn Astronomical Institute Structure, kinematics and dynamics of the Galaxy Outline Structure of the Galaxy History Kinematics of the Galaxy All-sky pictures Galactic dynamics The earliest attempts to study the structure of the Milky Way Galaxy (the Sidereal System; really the whole universe) on a global scale were based on star counts. William Herschel (1738 – 1822) performed such “star gauges” and assumed that (1) all stars have equal intrinsic luminostities and (2) he could see stars out ot the edges of the system. -
Lecture 4: Dark Matter in Galaxies
LectureLecture 4:4: DarkDark MatterMatter inin GalaxiesGalaxies OutlineOutline WhatWhat isis darkdark matter?matter? HowHow muchmuch darkdark mattermatter isis therethere inin thethe Universe?Universe? EvidenceEvidence ofof darkdark mattermatter ViableViable darkdark mattermatter candidatescandidates TheThe coldcold darkdark mattermatter (CDM)(CDM) modelmodel ProblemsProblems withwith CDMCDM onon galacticgalactic scalesscales AlternativesAlternatives toto darkdark mattermatter WhatWhat isis DarkDark Matter?Matter? Dark Matter Luminous Matter FirstFirst detectiondetection ofof darkdark mattermatter FritzFritz ZwickyZwicky (1933):(1933): DarkDark mattermatter inin thethe ComaComa ClusterCluster HowHow MuchMuch DarkDark MatterMatter isis ThereThere inin TheThe Universe?Universe? ΩΩ == ρρ // ρρ Μ Μ c ~2% RecentRecent measurements:measurements: (Luminous) Ω ∼ 0.25, Ω ∼ 0.75 ΩΜ ∼ 0.25, Ω Λ ∼ 0.75 ΩΩ ∼∼ 0.0050.005 Lum ~98% (Dark) HowHow DoDo WeWe KnowKnow ThatThat itit Exists?Exists? CosmologicalCosmological ParametersParameters ++ InventoryInventory ofof LuminousLuminous materialmaterial DynamicsDynamics ofof galaxiesgalaxies DynamicsDynamics andand gasgas propertiesproperties ofof galaxygalaxy clustersclusters GravitationalGravitational LensingLensing DynamicsDynamics ofof GalaxiesGalaxies II Galaxy ≈ Stars + Gas + Dust + Supermassive Black Hole + Dark Matter DynamicsDynamics ofof GalaxiesGalaxies IIII Visible galaxy Observed Vrot Expected R R Dark matter halo Visible galaxy DynamicsDynamics ofof GalaxyGalaxy ClustersClusters Balance -
Disk Heating, Galactoseismology, and the Formation of Stellar Halos
galaxies Article Disk Heating, Galactoseismology, and the Formation of Stellar Halos Kathryn V. Johnston 1,*,†, Adrian M. Price-Whelan 2,†, Maria Bergemann 3, Chervin Laporte 1, Ting S. Li 4, Allyson A. Sheffield 5, Steven R. Majewski 6, Rachael S. Beaton 7, Branimir Sesar 3 and Sanjib Sharma 8 1 Department of Astronomy, Columbia University, 550 W 120th st., New York, NY 10027, USA; cfl[email protected] 2 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA; [email protected] 3 Max Planck Institute for Astronomy, Heidelberg 69117, Germany; [email protected] (M.B.); [email protected] (B.S.) 4 Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA; [email protected] 5 Department of Natural Sciences, LaGuardia Community College, City University of New York, 31-10 Thomson Ave., Long Island City, NY 11101, USA; asheffi[email protected] 6 Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USA; [email protected] 7 The Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA; [email protected] 8 Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia; [email protected] * Correspondence: [email protected]; Tel.: +1-212-854-3884 † These authors contributed equally to this work. Academic Editors: Duncan A. Forbes and Ericson D. Lopez Received: 1 July 2017; Accepted: 14 August 2017; Published: 26 August 2017 Abstract: Deep photometric surveys of the Milky Way have revealed diffuse structures encircling our Galaxy far beyond the “classical” limits of the stellar disk.