Jahresstatistik 2018 Max-Planck-Institut Für
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Science Olympiad Astronomy C Division Event University of Chicago Invitational
Science Olympiad Astronomy C Division Event University of Chicago Invitational University of Chicago Chicago, IL January 11, 2020 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2) Do not forget to put your team name and team number at the top of all answer pages. 3) Write all answers on the lines on the answer pages. Any marks elsewhere will not be scored. 4) Do not worry about significant figures. Use 3 or more in your answers, regardless of how many are in the question. 5) Please do not access the internet during the event. If you do so, your team will be disqualified. 6) Feel free to take apart the test and staple it back together at the end! 7) Good luck! And may the stars be with you! 1 Section A: Use the Image/Illustration Set to answer the following questions. Each sub-question in this section is worth one point. 1. Image 1 shows the Bullet Cluster. (a) What part of the electromagnetic spectrum was this image taken in? (b) What do the blue regions correspond to? (c) How was the matter in the blue regions detected? (d) Which other image shows this cluster? 2. Image 2 shows part of M87. (a) What part of M87 does this image show? (b) What part of the electromagnetic spectrum was this image taken in? (c) Which image shows a zoomed-in radio observation of this region? (d) What type of astronomical object is shown in the image from part (c)? 3. -
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: Gw170817 and Grb 170817A
Draft version October 15, 2017 Typeset using LATEX twocolumn style in AASTeX61 GRAVITATIONAL WAVES AND GAMMA-RAYS FROM A BINARY NEUTRON STAR MERGER: GW170817 AND GRB 170817A B. P. Abbott,1 R. Abbott,1 T. D. Abbott,2 F. Acernese,3, 4 K. Ackley,5, 6 C. Adams,7 T. Adams,8 P. Addesso,9 R. X. Adhikari,1 V. B. Adya,10 C. Affeldt,10 M. Afrough,11 B. Agarwal,12 M. Agathos,13 K. Agatsuma,14 N. Aggarwal,15 O. D. Aguiar,16 L. Aiello,17, 18 A. Ain,19 P. Ajith,20 B. Allen,10, 21, 22 G. Allen,12 A. Allocca,23, 24 M. A. Aloy,25 P. A. Altin,26 A. Amato,27 A. Ananyeva,1 S. B. Anderson,1 W. G. Anderson,21 S. V. Angelova,28 S. Antier,29 S. Appert,1 K. Arai,1 M. C. Araya,1 J. S. Areeda,30 N. Arnaud,29, 31 K. G. Arun,32 S. Ascenzi,33, 34 G. Ashton,10 M. Ast,35 S. M. Aston,7 P. Astone,36 D. V. Atallah,37 P. Aufmuth,22 C. Aulbert,10 K. AultONeal,38 C. Austin,2 A. Avila-Alvarez,30 S. Babak,39 P. Bacon,40 M. K. M. Bader,14 S. Bae,41 P. T. Baker,42 F. Baldaccini,43, 44 G. Ballardin,31 S. W. Ballmer,45 S. Banagiri,46 J. C. Barayoga,1 S. E. Barclay,47 B. C. Barish,1 D. Barker,48 K. Barkett,49 F. Barone,3, 4 B. Barr,47 L. Barsotti,15 M. Barsuglia,40 D. Barta,50 J. -
Measuring the Hubble Constant with a Sample of Kilonovae
Measuring the Hubble Constant with a sample of kilonovae Michael W. Coughlin1;2,∗ Sarah Antier3, Tim Dietrich4;5, Ryan J. Foley6, Jack Heinzel7;8, Mattia Bulla9, Nelson Christensen7;8, David A. Coulter6, Lina Issa9;10, and Nandita Khetan11 1School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA 2Division of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 3APC, UMR 7164, 10 rue Alice Domon et Leonie´ Duquet, 75205 Paris, France 4Institut fur¨ Physik und Astronomie, Universitat¨ Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany 5Nikhef, Science Park 105, 1098 XG Amsterdam, The Netherlands 6Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA 7Artemis, Universite´ Coteˆ d’Azur, Observatoire Coteˆ d’Azur, CNRS, CS 34229, F-06304 Nice Cedex 4, France 8Physics and Astronomy, Carleton College, Northfield, MN 55057, USA 9Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, arXiv:2008.07420v1 [astro-ph.HE] 17 Aug 2020 SE-106 91 Stockholm, Sweden 10Universite´ Paris-Saclay, ENS Paris-Saclay, Departement´ de Phyisque, 91190, Gif-sur-Yvette, France. ∗ Corresponding Author: [email protected]. 1 11Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy 1 Abstract Kilonovae produced by the coalescence of compact binaries with at least one neutron star are promising standard sirens for an independent measurement of the Hubble constant (H0). Through their detection via follow-up of gravitational-wave (GW), short gamma-ray bursts (sGRBs) or optical surveys, a large sample of kilonovae (even without GW data) can be used for H0 contraints. -
Uncovering the Orbit of the Hercules Dwarf Galaxy
MNRAS 000,1{15 (2019) Preprint 3 December 2019 Compiled using MNRAS LATEX style file v3.0 Uncovering the Orbit of the Hercules Dwarf Galaxy Alexandra L. Gregory1?, Michelle L. M. Collins1, Denis Erkal1, Erik Tollerud2, Maxime Delorme1, Lewis Hill1, David J. Sand3, Jay Strader4 Beth Willman5, 1Department of Physics, University of Surrey, Guildford, GU2 7XH, Surrey, UK 2Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA 3Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USA 4Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 5National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, AZ 85719, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present new chemo{kinematics of the Hercules dwarf galaxy based on Keck II{ DEIMOS spectroscopy. Our 21 confirmed members have a systemic velocity of vHerc = −1 +1:4 −1 46:4 1:3 kms and a velocity dispersion σv;Herc = 4:4−1:2 kms . From the strength of the± Ca II triplet, we obtain a metallicity of [Fe/H]= 2:48 0:19 dex and dispersion +0:18 − ± of σ[Fe=H] = 0:63−0:13 dex. This makes Hercules a particularly metal{poor galaxy, placing it slightly below the standard mass{metallicity relation. Previous photometric and spectroscopic evidence suggests that Hercules is tidally disrupting and may be on a highly radial orbit. From our identified members, we measure no significant velocity gradient. By cross{matching with the second Gaia data release, we determine an ∗ uncertainty{weighted mean proper motion of µα = µα cos(δ) = 0:153 0:074 mas −1 −1 − ± yr , µδ = 0:397 0:063 mas yr . -
Gaia DR2 White Dwarfs in the Hercules Stream Santiago Torres1,2, Carles Cantero1, María E
A&A 629, L6 (2019) Astronomy https://doi.org/10.1051/0004-6361/201936244 & c ESO 2019 Astrophysics LETTER TO THE EDITOR Gaia DR2 white dwarfs in the Hercules stream Santiago Torres1,2, Carles Cantero1, María E. Camisassa3,4, Teresa Antoja5, Alberto Rebassa-Mansergas1,2, Leandro G. Althaus3,4, Thomas Thelemaque6, and Héctor Cánovas7 1 Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain e-mail: [email protected] 2 Institute for Space Studies of Catalonia, c/Gran Capità 2-4, Edif. Nexus 104, 08034 Barcelona, Spain 3 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina 4 Instituto de Astrofísica de La Plata, UNLP-CONICET, Paseo del Bosque s/n, 1900 La Plata, Argentina 5 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain 6 Industrial and Informatic Systems Deparment, EPF - École d’Ingénieurs, 21 boulevard Berthelot, 34000 Montpellier, France 7 European Space Astronomy Centre (ESA/ESAC), Operations Deparment, Villanueva de la Cañada, 28692 Madrid, Spain Received 5 July 2019 / Accepted 7 August 2019 ABSTRACT Aims. We analyzed the velocity space of the thin- and thick-disk Gaia white dwarf population within 100 pc by searching for signatures of the Hercules stellar stream. We aimed to identify objects belonging to the Hercules stream, and by taking advantage of white dwarf stars as reliable cosmochronometers, to derive a first age distribution. Methods. We applied a kernel density estimation to the UV velocity space of white dwarfs. -
The Afterglow and Early-Type Host Galaxy of the Short GRB 150101B at Z = 0.1343
The Afterglow and Early-type Host Galaxy of the Short GRB 150101B at Z = 0.1343 The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Fong, W., R. Margutti, R. Chornock, E. Berger, B. J. Shappee, A. J. Levan, N. R. Tanvir, et al. 2016. “The Afterglow and Early-type Host Galaxy of the Short GRB 150101B at Z = 0.1343.” The Astrophysical Journal 833, no. 2: 151. doi:10.3847/1538-4357/833/2/151. Published Version doi:10.3847/1538-4357/833/2/151 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:30510303 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP DRAFT VERSION SEPTEMBER 1, 2016 Preprint typeset using LATEX style emulateapj v. 01/23/15 THE AFTERGLOW AND EARLY-TYPE HOST GALAXY OF THE SHORT GRB 150101B AT Z = 0:1343 ; ; ; W. FONG1 2 , R. MARGUTTI3 4 , R. CHORNOCK5 , E. BERGER6 , B. J. SHAPPEE7 8 , A. J. LEVAN9 , N. R. TANVIR10 , N. SMITH2 , ; P. A. MILNE2 , T. LASKAR11 12 , D. B. FOX13 , R. LUNNAN14 , P. K. BLANCHARD6 , J. HJORTH15 , K. WIERSEMA10 , A. J. VAN DER HORST16 , D. ZARITSKY2 Draft version September 1, 2016 ABSTRACT We present the discovery of the X-ray and optical afterglows of the short-duration GRB 150101B, pinpointing the event to an early-type host galaxy at z = 0:1343±0:0030. -
Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a Spinning Universe
Journal of High Energy Physics, Gravitation and Cosmology, 2021, 7, 98-122 https://www.scirp.org/journal/jhepgc ISSN Online: 2380-4335 ISSN Print: 2380-4327 Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a Spinning Universe Puthalath Koroth Raghuprasad Independent Researcher, Odessa, TX, USA How to cite this paper: Raghuprasad, P.K. Abstract (2021) Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a This is the final article in our series dealing with the interplay of spin and Spinning Universe. Journal of High Energy gravity that leads to the generation, and continuation of celestial body mo- Physics, Gravitation and Cosmology, 7, tions in the universe. In our prior studies we focused on such interactions in 98-122. https://doi.org/10.4236/jhepgc.2021.71005 the elementary particles, and in the celestial bodies in the solar system. Fore- most among the findings was that, along with gravity, matter at all levels ex- Received: March 23, 2020 hibits axial spin. We further noted that all freestanding bodies outside our Accepted: December 19, 2020 solar system, including the largest such units, the stars and galaxies also spin Published: December 22, 2020 on their axes. Also, the axial rotation speed of planets in our solar system has Copyright © 2021 by author(s) and a linear positive relationship to their masses, thus hinting at its fundamental Scientific Research Publishing Inc. and autonomous nature. We have reported that this relationship between the This work is licensed under the Creative size of the body and its axial rotation speed extends to the stars and even the Commons Attribution International License (CC BY 4.0). -
Fermi GBM Observations of GRB 150101B: a Second Nearby Event with a Short Hard Spike and a Soft Tail
The Astrophysical Journal Letters, 863:L34 (9pp), 2018 August 20 https://doi.org/10.3847/2041-8213/aad813 © 2018. The American Astronomical Society. Fermi GBM Observations of GRB 150101B: A Second Nearby Event with a Short Hard Spike and a Soft Tail E. Burns1, P. Veres2 , V. Connaughton3, J. Racusin4 , M. S. Briggs2,4, N. Christensen5,6, A. Goldstein3 , R. Hamburg2,4, D. Kocevski7, J. McEnery4, E. Bissaldi8,9 , T. Dal Canton1, W. H. Cleveland3, M. H. Gibby10, C. M. Hui7, A. von Kienlin11, B. Mailyan2, W. S. Paciesas3 , O. J. Roberts3, K. Siellez12, M. Stanbro4, and C. A. Wilson-Hodge7 1 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; [email protected] 2 Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899, USA 3 Science and Technology Institute, Universities Space Research Association, Huntsville, AL 35805, USA 4 Space Science Department, University of Alabama in Huntsville, Huntsville, AL 35899, USA 5 Physics and Astronomy, Carleton College, MN 55057, USA 6 Artemis, Université Côte d’Azur, Observatoire Côte d’Azur, CNRS, CS 34229, F-06304 Nice Cedex 4, France 7 Astrophysics Branch, ST12, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USA 8 Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy 9 Dipartimento Interateneo di Fisica, Politecnico di Bari, Via E. Orabona 4, I-70125, Bari, Italy 10 Jacobs Technology, Inc., Huntsville, AL 35805, USA 11 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany 12 Center for Relativistic Astrophysics and School of Physics, Georgia Institute of Technology, Atlanta, GA 30332, USA Received 2018 July 13; revised 2018 August 3; accepted 2018 August 4; published 2018 August 17 Abstract In light of the joint multimessenger detection of a binary neutron star merger as the gamma-ray burst GRB 170817A and in gravitational waves as GW170817, we reanalyze the Fermi Gamma-ray Burst Monitor data of one of the closest short gamma-ray bursts (SGRBs): GRB 150101B. -
The Electromagnetic Counterpart of the Binary Neutron Star Merger Ligo/Virgo Gw170817: Viii
DRAFT VERSION OCTOBER 12, 2017 Typeset using LATEX twocolumn style in AASTeX61 THE ELECTROMAGNETIC COUNTERPART OF THE BINARY NEUTRON STAR MERGER LIGO/VIRGO GW170817: VIII. A COMPARISON TO COSMOLOGICAL SHORT-DURATION GAMMA-RAY BURSTS ∗ W. FONG,1 , E. BERGER,2 P. K. BLANCHARD,2 R. MARGUTTI,1 P. S. COWPERTHWAITE,2 R. CHORNOCK,3 K. D. ALEXANDER,2 B. D. METZGER,4 V. A. VILLAR,2 M. NICHOLL,2 T. EFTEKHARI,2 P. K. G. WILLIAMS,2 J. ANNIS,5 D. BROUT,6 D. A. BROWN,7 H.-Y. CHEN,8 Z. DOCTOR,8 H. T. DIEHL,5 D. E. HOLZ,9, 8 A. REST,10, 11 M. SAKO,6 AND M. SOARES-SANTOS5, 12 1Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208 2Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA 3Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USA 4Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA 5Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA 6Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA 7Department of Physics, Syracuse University, Syracuse NY 13224, USA 8Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA 9Enrico Fermi Institute, Department of Physics, Department of Astronomy and Astrophysics 10Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 11Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA 12Department of Physics, Brandeis University, Waltham, MA 02452, USA ABSTRACT We present a comprehensive comparison of the properties of the radio through X-ray counterpart of GW170817 and the properties of short-duration gamma-ray bursts (GRBs). -
MY SO October Showdown Rules
S P A C E - O C T O B E R 2 0 2 0 MY SO STEM SHOWDOWN C O N T E N T , R E C O M M E N D E D M A T E R I A L S & S C O R I N G STEM SHOWDOWN CONTENT The STEM Showdown will consist of a series of online multiple-choice questions. Middle school (Grade 6-9) participant questions will center around the properties and evolution of stars and galaxies as well as their observation using different portions of the electromagnetic spectrum (e.g., Radio, Infrared, Visible, Ultraviolet, X-Ray, Gamma Ray). While high school (Grades 9-12) participants will focus on Star and Galaxy Formation and Evolution. A Showdown participant will have 55- minutes to answer as many questions as possible. The middle school (Grades 6-9) content and skills covered by the Showdown this month is as follows: 1.Stellar and galactic evolution 2.Spectral classification of stars 3.Hubble classification of galaxies 4.Observation using multiple portions of the electromagnetic spectrum 5.The relationship between stellar temperature, radius, and luminosity 6.Magnitude and luminosity scales, distance modulus, inverse square law 7.Identification of the stars, constellations, and deep sky objects included in the list below as they appear on star charts, H-R diagrams, portable star labs, photos, or planetariums. Note: Constellations are underlined; Stars are boldface; Deep Sky Objects are italicized. a.Andromeda: M31 (Andromeda Galaxy) b.Aquila: Altair c.Auriga: Capella d.Bootes: Arcturus e.Cancer: DLA0817g f.Canis Major: Sirius g.Canis Minor: Procyon h.Centaurus: NGC5128 i.Coma Berenices: NGC4676, NGC4555 j.Corvus: NGC4038/NGC4039 k.Crux: Dragonfish Nebula l.Cygnus: Deneb m.Dorado: 30 Doradus, LMC n.Gemini: Castor, Pollux o.Lyra: Vega p.Ophiuchus: Zeta Ophiuchi, Rho Ophiuchi cloud complex q.Orion: Betelgeuse, Rigel & M42 (Orion Nebula) r.Perseus: Algol, NGC1333 Science Olympiad, Inc. -
Printmgr File
ADVANCED SERIES TRUST SEMIANNUAL REPORT ‰ JUNE 30, 2015 Based on the variable contract you own or the portfolios you invested in, AST Advanced Strategies Portfolio you may receive additional reports that provide financial information on AST Balanced Asset Allocation Portfolio those investment choices. Please refer to your variable annuity or variable AST BlackRock Global Strategies Portfolio life insurance contract prospectus to determine which portfolios are AST BlackRock/Loomis Sayles Bond Portfolio available to you. AST Defensive Asset Allocation Portfolio AST FI Pyramis® Quantitative Portfolio The views expressed in this report and information about the Trust’s AST Franklin Templeton Founding Funds portfolio holdings are for the period covered by this report and are subject Plus Portfolio to change thereafter. AST Legg Mason Diversified Growth Portfolio AST PIMCO Limited Maturity Bond Portfolio* The accompanying financial statements as of June 30, 2015, were not AST Preservation Asset Allocation Portfolio audited and, accordingly, no auditor’s opinion is expressed on them. AST Prudential Growth Allocation Portfolio AST RCM World Trends Portfolio Please note that this document may include prospectus supplements that AST Schroders Global Tactical Portfolio are separate from and not a part of this report. Please refer to your variable AST Schroders Multi-Asset World annuity or variable life insurance contract prospectus to determine which Strategies Portfolio supplements are applicable to you. AST T. Rowe Price Asset Allocation Portfolio AST T. Rowe Price Growth Opportunities Portfolio For information regarding enrollment in the e-Delivery program, please see the inside front cover of this report. * Effective July 13, 2015, the AST PIMCO Limited Maturity Bond Portfolio has been renamed the AST BlackRock Low Duration Bond Portfolio. -
Ellipticals in the CPG and in the Sample of Sramek (1975) 44
RADIO AND OPTICAL PROPERTIES OF DOUBLE GALAXIES Item Type text; Dissertation-Reproduction (electronic) Authors Stocke, John T. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 27/09/2021 19:19:08 Link to Item http://hdl.handle.net/10150/289608 INFORMATION TO USERS This material was produced from a microfilm copy of the original document. While the most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the original submitted. The following explanation of techniques is provided to help you understand markings or patterns which may appear on this reproduction. 1. The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting thru an image and duplicating adjacent pages to insure you complete continuity. 2. When an image on the film is obliterated with a large round black mark, it is an indication that the photographer suspected that the copy may have moved during exposure and thus cause a blurred image. You will find a good image of the page in the adjacent frame. 3. When a map, drawing or chart, etc., was part of the material being photographed the photographer followed a definite method in "sectioning" the material.