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HST Observations of Young Star Clusters in Interacting Galaxies
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Extragalactic Star Clusters IAU Symposium Series, Vol. Vol. 207, 2001 Eva K. Grebel, Doug Geisler, and Dante Minniti, eds. HST Observations of Young Star Clusters in Interacting Galaxies Kirk D. Borne Raytheon ITSS and NASA-GSFC, Code 631, Astrophysics Data Facility, Greenbelt, MD 20771 USA William C. Keel University of Alabama, Dept. of Physics and Astronomy, Tuscaloosa, AL 35487-0324 USA Philip N. Appleton & Curtis Struck Iowa State University, Dept. of Physics and Astronomy, Ames, IA 50011 USA RayA.Lucas&AlfredB.Schultz STScI, 3700 San Martin Drive, Baltimore, MD 21218 USA Abstract. We present early results from the analysis of HST imaging observations for several pairs of interacting galaxies. We include two cases that were specifically chosen to represent a strong early (young) encounter and a weak late (old) encounter. The goals of the project include a de- termination of the timing, frequency, strength, and characteristics of the young star clusters formed in these two limiting cases of tidal encounters. 1. Results from the Analysis of HST Imaging Observations Multi-band HST imaging data have been obtained for several interacting galaxy systems. These include the Cartwheel Ring Galaxy (Borne et al. 1996; Struck et al. 1996; Appleton et al., in preparation), Arp 81 and Arp 297 (Keel & Borne, in preparation), and a large sample of ULIRGs (Ultra-Luminous Infrared Galax- ies; Borne et al. 2000, and references therein). WFPC2 B-band (F450W) and I-band (F814W) images have been obtained for the Cartwheel, Arp 297, and Arp 81. -
Large-Scale Outflows in Edge-On Seyfert Galaxies. II. Kiloparsec
Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission Edward J. M. Colbert1,2, Stefi A. Baum1, Jack F. Gallimore1,2, Christopher P. O’Dea1, Jennifer A. Christensen1 Received ; accepted arXiv:astro-ph/9604022v1 3 Apr 1996 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 2 Department of Astronomy, University of Maryland, College Park, MD 20742 –2– ABSTRACT We present deep images of the kpc-scale radio continuum emission in 14 edge-on galaxies (ten Seyfert and four starburst galaxies). Observations were taken with the VLA at 4.9 GHz (6 cm). The Seyfert galaxies were selected from a distance-limited sample of 22 objects (defined in paper I). The starburst galaxies were selected to be well-matched to the Seyferts in radio power, recessional velocity and inclination angle. All four starburst galaxies have a very bright disk component and one (NGC 3044) has a radio halo that extends several kpc out of the galaxy plane. Six of the ten Seyferts observed have large-scale (radial extent >1 kpc) radio structures extending outward from the ∼ nuclear region, indicating that large-scale outflows are quite common in Seyferts. Large-scale radio sources in Seyferts are similar in radio power and radial extent to radio halos in edge-on starburst galaxies, but their morphologies do not resemble spherical halos observed in starburst galaxies. The sources have diffuse morphologies, but, in general, they are oriented at skewed angles with respect to the galaxy minor axes. This result is most easily understood if the outflows are AGN-driven jets that are somehow diverted away from the galaxy disk on scales >1 kpc. -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V
Astronomy Letters, Vol. 27, No. 4, 2001, pp. 207–212. Translated from Pis’ma v Astronomicheskiœ Zhurnal, Vol. 27, No. 4, 2001, pp. 243–249. Original Russian Text Copyright © 2001 by Dubrovich. Formation Mechanisms of “Negative”-Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V. K. Dubrovich* Special Astrophysical Observatory, Russian Academy of Sciences, pos. Nizhniœ Arkhyz, Stavropol kraœ, 357147 Russia Received June 2, 2000; in final form, October 2, 2000 Abstract—We consider the formation mechanisms of “negative”-intensity spots in the radio band for various astrophysical conditions. For wavelengths λ < 1.5 mm, the regions of reduced temperature (relative to the cos- mic microwave background radiation, CMBR) are shown to be produced only by high-redshift objects moving at peculiar velocities. The main processes are CMBR Thomson scattering and bremsstrahlung. We show that the effect δT/T can be ~ 10–5 in magnitude. We derive simple analytic expressions, which allow the redshifts, electron densities, and linear sizes of these regions to be estimated from observed spectral and spatial parame- ters. Additional observational methods for refining these parameters are outlined. © 2001 MAIK “Nauka/Inter- periodica”. Key words: theoretical and observational cosmology INTRODUCTION only two formation mechanisms of the “glow.” One of In the last 30 years, much attention has been given them is the Doppler distortion of external, equilibrium, to the search for and a detailed analysis of spatial fluc- and isotropic radiation (CMBR). For this to occur, the tuations in cosmic microwave background radiation object must have a peculiar velocity Vp and some non- zero opacity. -
The Outermost Hii Regions of Nearby Galaxies
THE OUTERMOST HII REGIONS OF NEARBY GALAXIES by Jessica K. Werk A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Astronomy and Astrophysics) in The University of Michigan 2010 Doctoral Committee: Professor Mario L. Mateo, Co-Chair Associate Professor Mary E. Putman, Co-Chair, Columbia University Professor Fred C. Adams Professor Lee W. Hartmann Associate Professor Marion S. Oey Professor Gerhardt R. Meurer, University of Western Australia Jessica K. Werk Copyright c 2010 All Rights Reserved To Mom and Dad, for all your love and encouragement while I was taking up space. ii ACKNOWLEDGMENTS I owe a deep debt of gratitude to a long list of individuals, institutions, and substances that have seen me through the last six years of graduate school. My first undergraduate advisor in Astronomy, Kathryn Johnston, was also my first Astronomy Professor. She piqued my interest in the subject from day one with her enthusiasm and knowledge. I don’t doubt that I would be studying something far less interesting if it weren’t for her. John Salzer, my next and last undergraduate advisor, not only taught me so much about observing and organization, but also is responsible for convincing me to go on in Astronomy. Were it not for John, I’d probably be making a lot more money right now doing something totally mind-numbing and soul-crushing. And Laura Chomiuk, a fellow Wesleyan Astronomy Alumnus, has been there for me through everything − problem sets and personal heartbreak alike. To know her as a friend, goat-lover, and scientist has meant so much to me over the last 10 years, that confining my gratitude to these couple sentences just seems wrong. -
On Problems Related to Galaxy Formation
On Problems Related To Galaxy Formation Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich-Wilhelms-Universität Bonn vorgelegt von Ahmed Hasan Abdullah aus Baghdad Bonn 2016 Angefertigt mit Genehmigung der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich-Wilhelms-Universität Bonn 1. Gutachter: Prof. Dr. P. Kroupa 2. Gutachterin: Dr. Maria Massi Tag der Promotion: 11.04.2016 Erscheinungsjahr: 2016 To My Parents i Erklärung Hiermit versichere ich, die vorgelegte Arbeit - abgesehen von den ausdrücklich angegebenen Hilfsmit- teln -persönlich, selbstständig und ohne die Benutzung anderer als der angegebenen Hilfsmittel angefer- tigt zu haben. Die aus anderen Quellen direkt und indirekt verwendeten Daten und Konzepte sind unter der Angabe der Quelle kenntlich gemacht. Weder die vorgelegte Arbeit noch eine ähnliche Arbeit sind bereits anderweitig als Dissertation eingereicht worden und von mir wurden zuvor keine Promotionsver- suche unternommen. Für die Erstellung der vorgelegten Arbeit wurde keine fremde Hilfe, insbesondere keine entgeltliche Hilfe von Vermittlungs-, Beratungsdiensten oder Ähnlichem, in Anspruch genom- men. Bonn, den Ahmed Abdullah iii Acknowledgements I owe thanks to many people for their support and guidance which gave me a chance to complete this thesis. I am truly indebted and thankful for their support. First and foremost, I would like to express my deep and sincere gratitude to my advisor, Prof. Dr. Pavel Kroupa, for the continuous support of my study and research, and his motivation, encouragement and patient supervision. It was an honor to have a supervisor who was so patient and willing to help . I would also like to express my gratitude to Dr. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
Im Fokus Hyaden in Den
DAS UMFASSENDE ASTRONOMISCHE JAHRBUCH Himmels- EXTRA 2 | 2016 EXTRA Almanach 2017 DATEN | DETAILLIERTE KARTEN | PRAXISTIPPS TOP-EREIGNISSE 2017 NGC 4513 UGCA 272 UGC 5336 M 81 Arp 300 ρ UGC 4539 64° Bode's Galaxy 64° Holmberg IX NGC 2959 Σ UGC 5028 RV NGC 4108 R 1400 NGC 2961 5 Σ 1573 NGC 3077 5 NGC 4256 NGC 4221 IC 2574 The Garland σ 2 Σ 1349 σ NGC 4332 Coddington's Nebula FBS 0959+685 NGC 2892 1 NGC 4210 Σ 1306 DERNGC 4441 WEGWEISERNGC 3622 NGC 2976 2 63° 3 UGC 4775 63° DRA NGC 4391 Sh 86 π 1 NGC 4125 VY NGC 4521 HCG 49 NGC 4545 NGC 3682 NGC 4510 NGC 4121 Σ 1350 FÜR DAS GESAMTE JAHR π 2 62° NGC 3231 62° 76 6 NGC 4205 ASTRONOMISCHE EREIGNISSE 57 UGC 5188 NGC 4081 NGC 3392 UGC 4159 UGC 7179 38 WOCHE FÜR WOCHE NGC 3394 35 UGC 6316 61° MCG +11-12-10 61° Σ 1559 NGC 2814 TOTALE S NGC 4605 UGC 5576 32 NGC 3259 β 408 NGC 2820 NGC 2805 τ SONNENFINSTERNIS NGC 3266 56 CGCG 292-85 60° NGC 4041 60° RY 28 5 ο BEOBACHTUNGSTIPPS UGC 6534 UGC 5776 NGC 4036 NGC 3668 23 UGC 7406 29 Muscida IN DEN USA UGC 6520 Σ 1351 MCG +11-14-33 T MCG +10-17-64 NGC 2742A MCG +10-18-51VON EXPERTEN NGC 3359 59° NGC 2880 59° NGC 3725 Σ 1315 UGC 6528 16 NGC 4547 VERSTÄNDLICHE ERKLÄRUNGEN RS NGC 3978 NGC 3762 NGC 2654 75 Shk 105 UGC 4289 NGC 3945 α FÜR EINSTEIGER ΟΣ 235 Dubhe MCG +10-12-103 74 TT 58° NGC 3835A NGC 2742 58° β 1077 UMA UGC 4730 NGC 4358 NGC 3471 NGC 4335 NGC 3835 NGC 3796 ΟΣΣ NGC 4500 Shk 124 92 NGC 2726 UGC 4549 M 40 NGC 3435 NGC 3894NGC 3809 Shk 113 NGC 4290 NGC 3895 20 NGC 2768 NGC 4149 Helix Galaxy 57° 57° 70 Arp 336 Abell 28 UGC 7635 Σ 1544 NGC 2685 UGC -
Astro-Ph/0210138
Spiral-like light profiles but elliptical-like kinematics in mergers of galaxies Chanda J. Jog and Aparna Chitre Department of Physics, Indian Institute of Science, Bangalore 560012, India e-mail: [email protected],[email protected] To Appear in A & A Letters, 393, Oct. 2002 arXiv:astro-ph/0210138v1 7 Oct 2002 1 Abstract It is commonly accepted that a merger of two spiral galaxies results in a rem- nant with an elliptical-like surface-brightness profile. Surprisingly, our recent study (Chitre & Jog 2002) of the 2MASS data for twenty-seven advanced mergers of galax- ies has shown that half of these have a light distribution that decreases exponentially with radius. Such a distribution normally characterizes a rotationally supported disk in a spiral galaxy. Here we show from kinematic data for two of these mergers, Arp 224 and Arp 214, that the main support against gravitational collapse comes from pressure due to random motion of stars as seen in an elliptical galaxy rather than from rotation. The origin of the unusual combination of properties seen here is a puzzle. The standard theoretical N-body models in the literature cannot account for these systems. Further observational and dynamical studies of this new class of merger remnants are needed, and would be important for understanding merger dynamics and galaxy evolution. Key words. galaxies: elliptical - galaxies: evolution - galaxies: interactions - galaxies: kinematics and dynamics - galaxies: spiral - galaxies: structure Running Title: Spiral-like light profiles but elliptical-like kinematics in mergers 1. Introduction It is well-established observationally that a merger of two gas-rich spirals can result in an r1/4 de Vaucouleurs radial profile typical of ellipticals (Schweizer 1982, Wright et al. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
Interstellarum 52 • Juni/Juli 2007 1 Inhalt
Editorial fokussiert Liebe Leserinnen und Leser, gibt es tatsächlich Planeten um andere Sterne, die die Vorrausset- zungen für die Entwicklung von Leben erfüllen? Eine derartige Mel- dung machte Ende April die Runde, als die ESO die Entdeckung eines Planeten in der »bewohnbaren«, weil möglicherweise die Existenz fl üs- sigen Wassers erlaubenden Zone um den Stern Gliese 581 bekanntgab (Seite 18). Solche Berichte machen den Eindruck, die Entdeckung von Leben in anderen Sonnensystemen stehe unmittelbar bevor – doch Daniel Fischers Blick hinter die Kulissen zeigt, dass wir noch am Anfang der Suche nach Exoplaneten stehen (Seite 12). Wenn interstellarum Teleskope testet, dann richtig – mit mehrmo- natigem Praxistest und optischer Bank. Diesmal stehen drei apochro- Ronald Stoyan, Chefredakteur matische Refraktoren der neuen Generation auf dem Prüfstand, die die Entscheidung besonders schwer machen – und die Beurteilung zu einem Vergnügen für den Tester. In diesem Heft steht die visuelle Leis- tungsfähigkeit im Vordergrund (Seite 50), in der kommenden Ausgabe werden die fotografi schen Fähigkeiten nachgereicht. Übrigens: Falls Sie einen Fernrohr-Kauf planen, empfehle ich Ihnen unsere Neuer- scheinung »Fernrohrwahl«. Dort sind praktisch alle auf dem deutschen Markt erhältlichen Modelle tabellarisch aufgelistet. Neu im Verlagsprogramm ist ebenfalls eine neue Ausgabe der inter- stellarum Archiv-CD, diesmal mit PDF-Dokumenten der Heftnummern 32 bis 49 – bestellbar über unsere Internetseite www.interstellarum.de. Dort laden wir Sie auch zur Teilnahme an der bisher größten Leserum- frage unserer Geschichte ein, denn wir wollen mehr über Sie und Ihre astronomischen Vorlieben erfahren – natürlich anonym. Bitte helfen Sie uns, interstellarum noch mehr auf Ihre Bedürfnisse auszurichten. Ihr Titelbild: Wie ein Planet eines anderen Sterns aussieht ist reine Spekulation – doch die künstlerische Darstellung der ESO hilft der Vorstellungskraft auf die Sprünge. -
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