Cycle 7 NICMOS Approved Programs
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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. -
Globular Clusters in the Inner Galaxy Classified from Dynamical Orbital
MNRAS 000,1{17 (2019) Preprint 14 November 2019 Compiled using MNRAS LATEX style file v3.0 Globular clusters in the inner Galaxy classified from dynamical orbital criteria Angeles P´erez-Villegas,1? Beatriz Barbuy,1 Leandro Kerber,2 Sergio Ortolani3 Stefano O. Souza 1 and Eduardo Bica,4 1Universidade de S~aoPaulo, IAG, Rua do Mat~ao 1226, Cidade Universit´aria, S~ao Paulo 05508-900, Brazil 2Universidade Estadual de Santa Cruz, Rodovia Jorge Amado km 16, Ilh´eus 45662-000, Brazil 3Dipartimento di Fisica e Astronomia `Galileo Galilei', Universit`adi Padova, Vicolo dell'Osservatorio 3, Padova, I-35122, Italy 4Universidade Federal do Rio Grande do Sul, Departamento de Astronomia, CP 15051, Porto Alegre 91501-970, Brazil Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Globular clusters (GCs) are the most ancient stellar systems in the Milky Way. There- fore, they play a key role in the understanding of the early chemical and dynamical evolution of our Galaxy. Around 40% of them are placed within ∼ 4 kpc from the Galactic center. In that region, all Galactic components overlap, making their disen- tanglement a challenging task. With Gaia DR2, we have accurate absolute proper mo- tions for the entire sample of known GCs that have been associated with the bulge/bar region. Combining them with distances, from RR Lyrae when available, as well as ra- dial velocities from spectroscopy, we can perform an orbital analysis of the sample, employing a steady Galactic potential with a bar. We applied a clustering algorithm to the orbital parameters apogalactic distance and the maximum vertical excursion from the plane, in order to identify the clusters that have high probability to belong to the bulge/bar, thick disk, inner halo, or outer halo component. -
10. Scientific Programme 10.1
10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic -
September Tonight's
September Tonight’s Sky September Tonight’s Sky Constellations As September brings transition from summer to fall, the sky transitions to the stars of autumn. Increasingly prominent in the southeastern sky is Pegasus, the winged horse. The Great Square of stars that outlines the body is a useful guide to the fall patterns around it. Near the Great Square lies the sprawling pattern of Aquarius, the water-bearer. Located within the western part of the constellation is M2, one of the oldest and largest globular star clusters associated with the Milky Way galaxy. It appears as a circular, grainy glow in backyard telescopes. NASA’s Hubble Space Telescope has imaged the cluster, a compact globe of some 150,000 stars that are more than 37,000 light-years away. At approximately 13 billion years old, this cluster formed early in the history of the universe, and offers scientists an opportunity to see how stars of different masses live and die. Results from ESA’s Gaia satellite suggest that this cluster, along with several others, may have once belonged to a dwarf galaxy that merged with the Milky Way. West of Aquarius is the constellation of Capricornus, the sea goat, a figure dating back to the Sumerians and Babylonians. The star at the western end of Capricornus is Alpha Capricorni. Alpha Capricorni is an optical double but not a binary pair. The brighter star, Algedi, is about 100 light- years away. The fainter lies along the same line of sight but is roughly eight times farther away. The pattern hosts another globular star cluster: M30. -
108 Afocal Procedure, 105 Age of Globular Clusters, 25, 28–29 O
Index Index Achromats, 70, 73, 79 Apochromats (APO), 70, Averted vision Adhafera, 44 73, 79 technique, 96, 98, Adobe Photoshop Aquarius, 43, 99 112 (software), 108 Aquila, 10, 36, 45, 65 Afocal procedure, 105 Arches cluster, 23 B1620-26, 37 Age Archinal, Brent, 63, 64, Barkhatova (Bar) of globular clusters, 89, 195 catalogue, 196 25, 28–29 Arcturus, 43 Barlow lens, 78–79, 110 of open clusters, Aricebo radio telescope, Barnard’s Galaxy, 49 15–16 33 Basel (Bas) catalogue, 196 of star complexes, 41 Aries, 45 Bayer classification of stellar associations, Arp 2, 51 system, 93 39, 41–42 Arp catalogue, 197 Be16, 63 of the universe, 28 Arp-Madore (AM)-1, 33 Beehive Cluster, 13, 60, Aldebaran, 43 Arp-Madore (AM)-2, 148 Alessi, 22, 61 48, 65 Bergeron 1, 22 Alessi catalogue, 196 Arp-Madore (AM) Bergeron, J., 22 Algenubi, 44 catalogue, 197 Berkeley 11, 124f, 125 Algieba, 44 Asterisms, 43–45, Berkeley 17, 15 Algol (Demon Star), 65, 94 Berkeley 19, 130 21 Astronomy (magazine), Berkeley 29, 18 Alnilam, 5–6 89 Berkeley 42, 171–173 Alnitak, 5–6 Astronomy Now Berkeley (Be) catalogue, Alpha Centauri, 25 (magazine), 89 196 Alpha Orionis, 93 Astrophotography, 94, Beta Pictoris, 42 Alpha Persei, 40 101, 102–103 Beta Piscium, 44 Altair, 44 Astroplanner (software), Betelgeuse, 93 Alterf, 44 90 Big Bang, 5, 29 Altitude-Azimuth Astro-Snap (software), Big Dipper, 19, 43 (Alt-Az) mount, 107 Binary millisecond 75–76 AstroStack (software), pulsars, 30 Andromeda Galaxy, 36, 108 Binary stars, 8, 52 39, 41, 48, 52, 61 AstroVideo (software), in globular clusters, ANR 1947 -
The Cluster Terzan 5 As a Remnant of a Primordial Building Block of the Galactic Bulge
1 The cluster Terzan 5 as a remnant of a primordial building block of the Galactic bulge F.R. Ferraro1, E. Dalessandro1, A. Mucciarelli1, G.Beccari2, M. R. Rich3, L. Origlia4, B. Lanzoni1, R. T. Rood5, E. Valenti6,7, M. Bellazzini4, S. M. Ransom8, G. Cocozza4 1Department of Astronomy, University of Bologna, Via Ranzani, 1, 40127 Bologna, Italy 2ESA, Space Science Department, Keplerlaan 1, 2200 AG Noordwijk, Netherlands 3Department of Physics and Astronomy, Math-Sciences 8979, UCLA, Los Angeles, CA 90095-1562,USA 4INAF- Osservatorio Astronomico di Bologna, Via Ranzani, 1, 40127 Bologna, Italy 5Astronomy Department, University of Virginia, P.O. Box 400325, Charlottesville, VA, 22904,USA 6European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 7Pontificia Universidad Catolica de Chile, Departamento de Astronomia, Avda Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 8National Radio Astronomy Observatory, Charlottesville, VA 22903, USA Globular star clusters are compact and massive stellar systems old enough to have witnessed the entire history of our Galaxy, the Milky Way. Although recent results1,2,3 suggest that their formation may have been more complex than previously thought, they still are the best approximation to a stellar population formed over a relatively short time scale (less than 1 Gyr) and with virtually no dispersion in the iron content. Indeed, only one cluster-like system (ω Centauri) in 2 the Galactic halo is known to have multiple stellar populations with a significant spread in iron abundance and age4,5. Similar findings in the Galactic bulge have been hampered by the obscuration arising from thick and varying layers of interstellar dust. -
Globular Clusters 1
Globular Clusters 1 www.FaintFuzzies.com Globular Clusters 2 www.FaintFuzzies.com Globular Clusters (Includes all known globulars in the Milky Way above declination of -50º plus some extras) by Alvin Huey www.faintfuzzies.com Last updated: March 27, 2014 Globular Clusters 3 www.FaintFuzzies.com Other books by Alvin H. Huey Hickson Group Observer’s Guide The Abell Planetary Observer’s Guide Observing the Arp Peculiar Galaxies Downloadable Guides by FaintFuzzies.com The Local Group Selected Small Galaxy Groups Galaxy Trios and Triple Systems Selected Shakhbazian Groups Globular Clusters Observing Planetary Nebulae and Supernovae Remnants Observing the Abell Galaxy Clusters The Rose Catalogue of Compact Galaxies Flat Galaxies Ring Galaxies Variable Galaxies The Voronstov-Velyaminov Catalogue – Part I and II Object of the Week 2012 and 2013 – Deep Sky Forum Copyright © 2008 – 2014 by Alvin Huey www.faintfuzzies.com All rights reserved Copyright granted to individuals to make single copies of works for private, personal and non-commercial purposes All Maps by MegaStarTM v5 All DSS images (Digital Sky Survey) http://archive.stsci.edu/dss/acknowledging.html This and other publications by the author are available through www.faintfuzzies.com Globular Clusters 4 www.FaintFuzzies.com Table of Contents Globular Cluster Index ........................................................................ 6 How to Use the Atlas ........................................................................ 10 The Milky Way Globular Clusters .................................................... -
GBX2018-Abstract-V2.Pdf
Scientific Rationale The bulge is a primary component of the Milky Way, comprising ∼25% of its mass. All major Galactic stellar populations intersect there, reaching their highest densities. Thus it is truly a crossroads. Current theory suggests that the bulge is the most ancient component of the Galaxy. Therefore, exploring the bulge is fundamental to understanding Galactic formation, structure and evolution. Indeed, thanks to the advent of multiplexed spectrographs on 8m-class telescopes, and to the availability of resolved, wide-field NIR photometry, our knowledge of the structural, chemical and kinematical properties of the Galactic bulge has improved dramatically in the last few years. At the same time, the interpretation of the accumulated data from this complex region is not straightforward, and many fundamental questions still remain to be answered. E.g. What is the age of the oldest stars? How was the metal-poor spheroid formed? What is the 3D shape of the bulge? What is the connection and interplay between the bulge and bar? Is there a separate bulge globular cluster population? What is the relationship of the central supermassive black hole with the bulge? Fortunately, this area of investigation is moving forward at a fast pace: since 2013, when the last large international conference on the bulge was organized, progress has been truly impressive. New massively multiplexed spectroscopic surveys (Gaia-ESO Survey, APOGEE South, MOONS., new deeper NIR photometric surveys (e.g., VVVX, the extension of the VVV Survey. as well as Gaia have recently begun or will begin imminently. Concomitantly, ever more detailed studies of galaxies at high-redshift promise to catch bulges at the time of their formation. -
Study of Globular Cluster Sources Using Erass1 Data
Study of Globular Cluster Sources using eRASS1 data Bachelorarbeit aus der Physik Vorgelegt von Roman Laktionov 27. April 2021 Dr. Karl Remeis-Sternwarte Friedrich-Alexander-Universit¨at Erlangen-Nu¨rnberg Betreuerin: Prof. Dr. Manami Sasaki Abstract Due to the high stellar density in globular clusters (GCs), they provide an ideal envi- ronment for the formation of X-ray luminous objects, e.g. cataclysmic variables and low-mass X-ray binaries. Those X-ray sources have, in the advent of ambitious observa- tion campaigns like the eROSITA mission, become accessible for extensive population studies. During the course of this thesis, X-ray data in the direction of the Milky Way's GCs was extracted from the eRASS1 All-Sky Survey and then analyzed. The first few chap- ters serve to provide an overview on the physical properties of GCs, the goals of the eROSITA mission and the different types of X-ray sources. Afterwards, the methods and results of the analysis will be presented. Using data of the eRASS1 survey taken between December 13th, 2019 and June 11th, 2020, 113 X-ray sources were found in the field of view of 39 GCs, including Omega Cen- tauri, 47 Tucanae and Liller 1. A Cross-correlation with optical/infrared catalogs and the subsequent analysis of various diagrams enabled the identification of 6 foreground stars, as well as numerous background candidates and stellar sources. Furthermore, hardness ratio diagrams were used to select 16 bright sources, possibly of GC origin, for a spectral analysis. By marking them in X-ray and optical images, it was concluded that 6 of these sources represent the bright central emission of their host GC, while 10 are located outside of the GC center. -
Cycle 20 Approved Programs
Cycle 20 Approved Programs Phase II First Name Last Name Institution Country Sci Cat Type Title A High-Resolution Survey of the Very Youngest Brown 12944 Katelyn Allers Bucknell University USA CS GO Dwarfs Pontificia Universidad Catolica de Unveiling the giant jet from Sanduleak's star in the Large 12868 Rodolfo Angeloni Chile ISM GO Chile Magellanic Cloud Signatures of turbulence in directly imaged protoplanetary 12814 Philip Armitage University of Colorado at Boulder USA SF AR disks UV Imaging of Luminous Infrared Galaxies in the GOALS 13007 Lee Armus California Institute of Technology USA USP SNAP Sample Institute of Space & Astronautical A unique opportunity to discover how energy is 13035 Sarah Badman Japan SS GO Science transported through Jupiter's magnetosphere The Age-Metallicity Relation of Galaxies in a LambdaCDM 12837 Jeremy Bailin University of Michigan USA RSP AR Universe 13021 Jacob Bean University of Chicago USA EXO GO Revealing the Diversity of Super-Earth Atmospheres Spatially Resolving the Disk Mass Accretion Process In 12963 Tracy Beck Space Telescope Science Institute USA SF GO Young Star Binaries A search for binaries with massive companions in the core 12911 Luigi Bedin Osservatorio Astronomico di Padova Italy RSP GO of the closest globular cluster M4 Hunting for Intermediate-Mass Black Holes: Archival 12845 Andrea Bellini Space Telescope Science Institute USA RSP AR Proper-Motion Analysis of Globular Clusters Precise Orbit Determination for New Horizons Candidate 12887 Susan Benecchi Carnegie Institution of Washington -
Origin of the System of Globular Clusters in the Milky Way D
A&A 630, L4 (2019) Astronomy https://doi.org/10.1051/0004-6361/201936135 & c ESO 2019 Astrophysics LETTER TO THE EDITOR Origin of the system of globular clusters in the Milky Way D. Massari1,2,3 , H. H. Koppelman1, and A. Helmi1 1 Kapteyn Astronomical Institute, University of Groningen, 9747 AD Groningen, The Netherlands 2 Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy e-mail: [email protected] 3 INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, Italy Received 19 June 2019 / Accepted 9 September 2019 ABSTRACT Context. The assembly history experienced by the Milky Way is currently being unveiled thanks to the data provided by the Gaia mission. It is likely that the globular cluster system of our Galaxy has followed a similarly intricate formation path. Aims. To constrain this formation path, we explore the link between the globular clusters and the known merging events that the Milky Way has experienced. Methods. To this end, we combined the kinematic information provided by Gaia for almost all Galactic clusters, with the largest sample of cluster ages available after carefully correcting for systematic errors. To identify clusters with a common origin we analysed their dynamical properties, particularly in the space of integrals of motion. Results. We find that about 40% of the clusters likely formed in situ. A similarly large fraction, 35%, appear to be possibly associated to known merger events, in particular to Gaia-Enceladus (19%), the Sagittarius dwarf galaxy (5%), the progenitor of the Helmi streams (6%), and to the Sequoia galaxy (5%), although some uncertainty remains due to the degree of overlap in their dynamical characteristics. -
第 28 届国际天文学联合会大会 Programme Book
IAU XXVIII GENERAL ASSEMBLY 20-31 AUGUST, 2012 第 28 届国际天文学联合会大会 PROGRAMME BOOK 1 Table of Contents Welcome to IAU Beijing General Assembly XXVIII ........................... 4 Welcome to Beijing, welcome to China! ................................................ 6 1.IAU EXECUTIVE COMMITTEE, HOST ORGANISATIONS, PARTNERS, SPONSORS AND EXHIBITORS ................................ 8 1.1. IAU EXECUTIVE COMMITTEE ..................................................................8 1.2. IAU SECRETARIAT .........................................................................................8 1.3. HOST ORGANISATIONS ................................................................................8 1.4. NATIONAL ADVISORY COMMITTEE ........................................................9 1.5. NATIONAL ORGANISING COMMITTEE ..................................................9 1.6. LOCAL ORGANISING COMMITTEE .......................................................10 1.7. ORGANISATION SUPPORT ........................................................................ 11 1.8. PARTNERS, SPONSORS AND EXHIBITORS ........................................... 11 2.IAU XXVIII GENERAL ASSEMBLY INFORMATION ............... 14 2.1. LOCAL ORGANISING COMMITTEE OFFICE .......................................14 2.2. IAU SECRETARIAT .......................................................................................14 2.3. REGISTRATION DESK – OPENING HOURS ...........................................14 2.4. ON SITE REGISTRATION FEES AND PAYMENTS ................................14