L'indien – Le MICROSCOPE

Total Page:16

File Type:pdf, Size:1020Kb

L'indien – Le MICROSCOPE L’Indien – Le Microscope Ces constellations ne contiennent pas d'objet céleste observable avec un équipement amateur. Hémisphère Sud Le CAPRICORNE Gamma Galaxie 4,67 N 6925 L’INDIEN – Le MICROSCOPE Alpha 4,87 Le SAGITTAIRE Le POISSON AUSTRAL Lacaille 8760 6,67 Distance 12,9 a.l. 3 Alpha La GRUE 3,11 Galaxie N 8760 Galaxie Galaxie N 7041 Le TELESCOPE N 7049 Galaxie IC 5152 Galaxie Βeta 3,67 Le TOUCAN N7090 Delta Galaxie 4,4 Galaxie N7141 superamas de galaxies du Paon-Indien 200 millions a.l. Epsilon 11,82 années-lumière Le PAON L’OCTANT constellations de l'hémisphère Sud. introduite par Nicolas-Louis de Lacaille en 1752 Les distances qui nous séparent des étoiles Les distances qui nous séparent des Galaxies Le superamas Paon-Indien, aussi appelé superamas du Paon, est un superamas de galaxies voisin du superamas local (qui contient la Voie lactée). Ce superamas est située entre 210 et 260 millions d'années- lumière (entre 64 et 78 mégaparsecs). Il contient trois principaux amas : Abell 3656, Abell 3698, le plus dense, et Abell 3742. Il fait partie d'un mur de galaxies assez proche qui relie l'amas de la Règle au superamas du Centaure. Une publication de 2014 émet l'hypothèse que ce superamas serait juste un lobe de Laniakea, un superamas plus grand centré sur le Grand Attracteur qui contient également le superamas de la Vierge dont nous faisons partie. 465 Millions a.l. Abell S0740 L'Indien, ou Oiseau indien[réf. nécessaire], est une constellation de l'hémisphère sud. La région qu'elle couvre, proche du pôle sud céleste, est relativement pauvre en étoiles et peu sont visibles à l'œil nu. L'acception « Oiseau indien » est relativement peu fréquente, en raison des risques de confusion avec la constellation de l'Oiseau de paradis. L'Indien est une constellation vraisemblablement inventée par les navigateurs néerlandais Pieter Dirkszoon Keyser et Frederick de Houtman à la fin du XVIe siècle et introduite par Johann Bayer dans son Uranometria en 1603. Elle est supposée représenter un Indien d'Amérique, que Bayer voulait honorer d'une place sur la voûte céleste. L'astronome Julius Schiller combina l'Indien et le Paon afin de former une constellation qu'il nomma d'après le personnage biblique Job. Cette constellation — comme toutes les autres créations religieuses de Schiller — ne rencontra pas de succès sur le long terme. La plus brillante, α Indi, de magnitude apparente 3,11, est une étoile géante de classe K0. Située à 100 années-lumière du système solaire, une dizaine de fois plus grande que le Soleil, son spectre montre qu'elle est anormalement enrichie en métaux. C'est également une étoile triple, ses compagnons, vraisemblablement des naines rouges, ne dépassant la magnitude 12. ε Indi est la 19e étoile la plus proche du Soleil, à 11,82 années-lumière de nous. δ Indi et θ Indi sont des étoiles doubles. On y trouve cependant la galaxie naine elliptique IC 5152, distante de 2 millions d'années lumière et appartenant à notre Groupe local, ainsi qu'une partie du superamas de galaxies du Paon-Indien, situé à plus de 200 millions d'années lumière. Quelques autres galaxies notables sont NGC 7090 (galaxie spirale) et NGC 7049 (galaxie elliptique). Indien (constellation). (2019, mars 19). Wikipédia, l'encyclopédie libre. Page consultée le 16:05, mars 19, 2019 à partir de http://fr.wikipedia.org/w/index.php?title=Indien_(constellation)&oldid=157687005. Microscope (constellation). (2018, août 2). Wikipédia, l'encyclopédie libre. Page consultée le 16:35, août 2, 2018 à partir de http://fr.wikipedia.org/w/index.php?title=Microscope_(constellation)&oldid=150921369. La constellation de l'Indien ne contient pas d'objet céleste observable avec un équipement amateur. .
Recommended publications
  • Curriculum Vitae Avishay Gal-Yam
    January 27, 2017 Curriculum Vitae Avishay Gal-Yam Personal Name: Avishay Gal-Yam Current address: Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel. Telephones: home: 972-8-9464749, work: 972-8-9342063, Fax: 972-8-9344477 e-mail: [email protected] Born: March 15, 1970, Israel Family status: Married + 3 Citizenship: Israeli Education 1997-2003: Ph.D., School of Physics and Astronomy, Tel-Aviv University, Israel. Advisor: Prof. Dan Maoz 1994-1996: B.Sc., Magna Cum Laude, in Physics and Mathematics, Tel-Aviv University, Israel. (1989-1993: Military service.) Positions 2013- : Head, Physics Core Facilities Unit, Weizmann Institute of Science, Israel. 2012- : Associate Professor, Weizmann Institute of Science, Israel. 2008- : Head, Kraar Observatory Program, Weizmann Institute of Science, Israel. 2007- : Visiting Associate, California Institute of Technology. 2007-2012: Senior Scientist, Weizmann Institute of Science, Israel. 2006-2007: Postdoctoral Scholar, California Institute of Technology. 2003-2006: Hubble Postdoctoral Fellow, California Institute of Technology. 1996-2003: Physics and Mathematics Research and Teaching Assistant, Tel Aviv University. Honors and Awards 2012: Kimmel Award for Innovative Investigation. 2010: Krill Prize for Excellence in Scientific Research. 2010: Isreali Physical Society (IPS) Prize for a Young Physicist (shared with E. Nakar). 2010: German Federal Ministry of Education and Research (BMBF) ARCHES Prize. 2010: Levinson Physics Prize. 2008: The Peter and Patricia Gruber Award. 2007: European Union IRG Fellow. 2006: “Citt`adi Cefal`u"Prize. 2003: Hubble Fellow. 2002: Tel Aviv U. School of Physics and Astronomy award for outstanding achievements. 2000: Colton Fellow. 2000: Tel Aviv U. School of Physics and Astronomy research and teaching excellence award.
    [Show full text]
  • Dwarfs Walking in a Row the filamentary Nature of the NGC 3109 Association
    A&A 559, L11 (2013) Astronomy DOI: 10.1051/0004-6361/201322744 & c ESO 2013 Astrophysics Letter to the Editor Dwarfs walking in a row The filamentary nature of the NGC 3109 association M. Bellazzini1, T. Oosterloo2;3, F. Fraternali4;3, and G. Beccari5 1 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands 3 Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands 4 Dipartimento di Fisica e Astronomia - Università degli Studi di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei Munchen, Germany Received 24 September 2013 / Accepted 22 October 2013 ABSTRACT We re-consider the association of dwarf galaxies around NGC 3109, whose known members were NGC 3109, Antlia, Sextans A, and Sextans B, based on a new updated list of nearby galaxies and the most recent data. We find that the original members of the NGC 3109 association, together with the recently discovered and adjacent dwarf irregular Leo P, form a very tight and elongated configuration in space. All these galaxies lie within ∼100 kpc of a line that is '1070 kpc long, from one extreme (NGC 3109) to the other (Leo P), and they show a gradient in the Local Group standard of rest velocity with a total amplitude of 43 km s−1 Mpc−1, and a rms scatter of just 16.8 km s−1. It is shown that the reported configuration is exceptional given the known dwarf galaxies in the Local Group and its surroundings.
    [Show full text]
  • Further Definition of the Mass-Metallicity Relation In
    Further Definition of the Mass-Metallicity Relation in Globular Cluster Systems Around Brightest Cluster Galaxies Robert Cockcroft Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada [email protected] William E. Harris Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada [email protected] Elizabeth M. H. Wehner Utrecht University, PO Box 80125, 3508 TC Utrecht, The Netherlands [email protected] Bradley C. Whitmore Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218 [email protected] and Barry Rothberg arXiv:0906.2008v1 [astro-ph.CO] 10 Jun 2009 Naval Research Laboratory, Code 7211, 4555 Overlook Ave SW, Washington D.C. 20375 [email protected] ABSTRACT We combine the globular cluster data for fifteen Brightest Cluster Galaxies and use this material to trace the mass-metallicity relations (MMR) in their glob- ular cluster systems (GCSs). This work extends previous studies which correlate the properties of the MMR with those of the host galaxy. Our combined data sets –2– show a mean trend for the metal-poor (MP) subpopulation which corresponds to a scaling of heavy-element abundance with cluster mass Z ∼ M0.30±0.05. No trend is seen for the metal-rich (MR) subpopulation which has a scaling relation that is consistent with zero. We also find that the scaling exponent is independent of the GCS specific frequency and host galaxy luminosity, except perhaps for dwarf galaxies. We present new photometry in (g’,i’) obtained with Gemini/GMOS for the globular cluster populations around the southern giant ellipticals NGC 5193 and IC 4329.
    [Show full text]
  • An Observer's Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations
    An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Dooley, Gregory A. et al. “An Observer’s Guide to the (Local Group) Dwarf Galaxies: Predictions for Their Own Dwarf Satellite Populations.” Monthly Notices of the Royal Astronomical Society 471, 4 (August 2017): 4894–4909 © 2018 The Author(s) As Published http://dx.doi.org/10.1093/MNRAS/STX1900 Publisher Oxford University Press (OUP) Version Author's final manuscript Citable link https://hdl.handle.net/1721.1/121369 Terms of Use Creative Commons Attribution-Noncommercial-Share Alike Detailed Terms http://creativecommons.org/licenses/by-nc-sa/4.0/ MNRAS 000,1{21 (2017) Preprint 6 September 2017 Compiled using MNRAS LATEX style file v3.0 An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations Gregory A. Dooley1?, Annika H. G. Peter2;3, Tianyi Yang4, Beth Willman5, Brendan F. Griffen1 and Anna Frebel1, 1Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2CCAPP and Department of Physics, The Ohio State University, Columbus, OH 43210, USA 3Department of Astronomy, The Ohio State University, Columbus OH 43210, USA 4Institute of Optics, University of Rochester, Rochester, New York, 14627, USA 5Steward Observatory and LSST, 933 North Cherry Avenue, Tucson, AZ 85721, USA Accepted by MNRAS 2017 July 22. Received 2017 July 22; in original 2016 September 27 ABSTRACT A recent surge in the discovery of new ultrafaint dwarf satellites of the Milky Way has 3 6 inspired the idea of searching for faint satellites, 10 M < M∗ < 10 M , around less massive field galaxies in the Local Group.
    [Show full text]
  • A New X-Ray Selected Sample of Very Extended Galaxy Groups from the ROSAT All-Sky Survey Weiwei Xu1, 2, 3, Miriam E
    Astronomy & Astrophysics manuscript no. main c ESO 2018 September 11, 2018 A New X-ray Selected Sample of Very Extended Galaxy Groups from the ROSAT All-Sky Survey Weiwei Xu1; 2; 3, Miriam E. Ramos-Ceja2, Florian Pacaud2, Thomas H. Reiprich2, and Thomas Erben2 1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China (e-mail: [email protected]) 2 Argelander-Insitut für Astronomie, Universität Bonn, Bonn, Germany 3 University of Chinese Academy of Sciences, Beijing, China Accepted by A&A ABSTRACT Context. Some indications for tension have long been identified between cosmological constraints obtained from galaxy clusters and primary cosmic microwave background (CMB) measurements. Typically, assuming the matter density and fluctuations, as parameterized with Ωm and σ8, estimated from CMB measurements, many more clusters are expected than those actually observed. This has been reinforced recently by the Planck collaboration. One possible explanation could be that certain types of galaxy groups or clusters were missed in samples constructed in previous surveys, resulting in a higher incompleteness than estimated. Aims. In this work, we aim to determine if a hypothetical class of very extended, low surface brightness, galaxy groups or clusters have been missed in previous X-ray cluster surveys based on the ROSAT All-Sky Survey (RASS). Methods. We applied a dedicated source detection algorithm sensitive also to more unusual group or cluster surface brightness distributions. It includes a multiresolution filtering, a source detection algorithm, and a maximum likelihood fitting procedure. To optimize parameters, this algorithm is calibrated using extensive simulations before it is used to reanalyze the RASS data.
    [Show full text]
  • Dwarf Galaxies of the Local Group Offer the Best Opportunity to Study a Representative Sample of These Important, but by Nature, Inconspicuous Galaxies in Detail
    DWARF GALAXIES OF THE LOCAL GROUP Mario Mateo KEY WORDS: Stellar Populations, Local Group Galaxies, Photometry, Galaxy Formation, Spectroscopy, Dark Matter, Interstellar Medium Shortened Title: LOCAL GROUP DWARFS Send Proofs To: Mario Mateo Department of Astronomy; University of Michigan Ann Arbor, MI 48109-1090 Phone: 313 936-1742; Fax: 313 763-6317 Email: [email protected] ABSTRACT The Local Group (LG) dwarf galaxies offer a unique window to the detailed properties of the most common type of galaxy in the Universe. In this review, I update the census of LG dwarfs based on the most recent distance and radial velocity determinations. I then discuss the detailed properties of this sample, including (a) the integrated photometric parameters and optical structures of these galaxies, (b) the content, nature and distribution of their ISM, (c) their heavy-element abundances derived from both stars and nebulae, (d) the arXiv:astro-ph/9810070v1 5 Oct 1998 complex and varied star-formation histories of these dwarfs, (e) their internal kinematics, stressing the relevance of these galaxies to the dark-matter problem and to alternative interpretations, and (f) evidence for past, ongoing and future interactions of these dwarfs with other galaxies in the Local Group and beyond. To complement the discussion and to serve as a foundation for future work, I present an extensive set of basic observational data in tables that summarize much of what we know, and what we still do not know, about these nearby dwarfs. Our understanding of these galaxies has grown impressively in the past decade, but fundamental puzzles remain that will keep the Local Group at the forefront of galaxy evolution studies for some time.
    [Show full text]
  • Naming Objects in Thesky
    - ; Chapter 4 Naming ObjectS in TheSky Astronomers need to be able to assimilate and exchange information about specific objects in the sky. Many systems have been devised over the last few thousand years to identify and name the most conspicuous ones. As our technology has advanced, studies of astronomical objects have become more precise. Today it is common for astronomers to assign numerous designations to a single celestial body. Humans have observed the stars for millennia. Our ancestors named the bright stars as well as larger groups of stars called constellations. As we said in Chapter 1, the ancients named many of the constellations after mythological beasts, gods, demigods, and ordinary household objects. Astronomers continue to use the names of the constellations first recorded by ancient astronomers thousands of years ago. It is here that we may begin to learn about where things are located in the sky and how they are named. Astronomers officially recognize 88 distinct constellations today. TheSky displays all of them quite accurately. From the mid-northern latitudes, you can see over half of them. Most are visible every night from your location at some time during the night. TheSky helps you to find them but you must go outside on any clear night throughout the year and look for them yourself. About a half dozen or so constellations are visible every night from 40°north latitude all year round. These are the circumpolar constellations. They are all located in the northern sky near the North Star, Polaris. Using TheSky will definitely help you locate all these constellations easily during any season of the year.
    [Show full text]
  • An Analysis of the First Three Catalogues of Southern Star Clusters and Nebulae
    ResearchOnline@JCU This file is part of the following reference: Cozens, Glendyn John (2008) An analysis of the first three catalogues of southern star clusters and nebulae. PhD thesis, James Cook University. Access to this file is available from: http://eprints.jcu.edu.au/24051/ The author has certified to JCU that they have made a reasonable effort to gain permission and acknowledge the owner of any third party copyright material included in this document. If you believe that this is not the case, please contact [email protected] and quote http://eprints.jcu.edu.au/24051/ Nicolas-Louis de La Caille, James Dunlop and John Herschel – An analysis of the First Three Catalogues of Southern Star Clusters and Nebulae Thesis submitted by Glendyn John COZENS BSc London, DipEd Adelaide in June 2008 for the degree of Doctor of Philosophy in the Faculty of Science, Engineering and Information Technology James Cook University STATEMENT OF ACCESS I, the undersigned, author of this work, understand that James Cook University will make this thesis available for use within the University Library and, via the Australian Digital Theses network, for use elsewhere. I understand that, as an unpublished work, a thesis has significant protection under the Copyright Act and; I do not wish to place any further restriction on access to this work. ____________________ Signature Date ii STATEMENT OF SOURCES DECLARATION I declare that this thesis is my own work and has not been submitted in any form for another degree or diploma at any university or other institution of tertiary education. Information derived from the published or unpublished work of others has been acknowledged in the text and a list of references is given.
    [Show full text]
  • The Astrology of Space
    The Astrology of Space 1 The Astrology of Space The Astrology Of Space By Michael Erlewine 2 The Astrology of Space An ebook from Startypes.com 315 Marion Avenue Big Rapids, Michigan 49307 Fist published 2006 © 2006 Michael Erlewine/StarTypes.com ISBN 978-0-9794970-8-7 All rights reserved. No part of the publication may be reproduced, stored in a retrieval system, or transmitted, in any form or by any means, electronic, mechanical, photocopying, recording, or otherwise, without the prior permission of the publisher. Graphics designed by Michael Erlewine Some graphic elements © 2007JupiterImages Corp. Some Photos Courtesy of NASA/JPL-Caltech 3 The Astrology of Space This book is dedicated to Charles A. Jayne And also to: Dr. Theodor Landscheidt John D. Kraus 4 The Astrology of Space Table of Contents Table of Contents ..................................................... 5 Chapter 1: Introduction .......................................... 15 Astrophysics for Astrologers .................................. 17 Astrophysics for Astrologers .................................. 22 Interpreting Deep Space Points ............................. 25 Part II: The Radio Sky ............................................ 34 The Earth's Aura .................................................... 38 The Kinds of Celestial Light ................................... 39 The Types of Light ................................................. 41 Radio Frequencies ................................................. 43 Higher Frequencies ...............................................
    [Show full text]
  • Institute for Astronomy University of Hawai'i at M¯Anoa Publications In
    Institute for Astronomy University of Hawai‘i at Manoa¯ Publications in Calendar Year 2009 Abazajian, K. N., et al., including Hoblitt, J., Magnier, E., Bagatin, A. C., Michel, P., & Bus, S. J. Preface to Special Is- Pope, A. C., Price, P. A., Szapudi, I. The Seventh Data sue VII Workshop on Catastrophic Disruption in the Solar Release of the Sloan Digital Sky Survey. ApJS, 182, 543– System. Planet. Space Sci., 57, 109–110 (2009) 558 (2009) Bakos, G. A., Howard, A. W., Noyes, R. W., Hartman, J., Akeson, R., et al., including Johnson, J. The Value of Torres, G., Kovacs,´ G., Fischer, D. A., Latham, D. W., the Keck Observatory to NASA and Its Scientific Com- Johnson, J. A., et al. HAT-P-13b,c: A Transiting Hot munity. astro2010: The Astronomy and Astrophysics Jupiter with a Massive Outer Companion on an Eccentric Decadal Survey, 2010, no. 1P (2009) Orbit. ApJ, 707, 446–456 (2009) Alcock, C., including Kudritzki, R.-P. Statement from AC- Bakos, G. A.,´ et al., including Johnson, J. A. HAT-P-10b: A CORD for ASTRO2010. astro2010: The Astronomy and Light and Moderately Hot Jupiter Transiting A K Dwarf. Astrophysics Decadal Survey, 2010, no. 27P (2009) ApJ, 696, 1950–1955 (2009) Allers, K. N., Liu, M. C., Shkolnik, E., Cushing, Bally, J., Walawender, J., Reipurth, B., & Megeath, S. T. M. C., Dupuy, T. J., Mathews, et al. 2MASS Outflows and Young Stars in Orion’s Large Cometary 22344161+4041387AB: A Wide, Young, Accreting, Clouds L1622 and L1634. AJ, 137, 3843–3858 (2009) Low-Mass Binary in the LkHα233 Group.
    [Show full text]
  • The Secrets of Galaxies How Many Types of Galaxies Are There?
    CESAR Science Case The Secrets of Galaxies How many types of galaxies are there? Student Guide The Secrets of Galaxies 2 CESAR Science Case Table of Contents Background ..................................................................................................... 5 Investigating galaxies ....................................................................................... 7 Activity 1: What is a galaxy? ......................................................................................................................... 7 Activity 2: Getting familiar with ESASky (optional) ........................................................................................ 8 Activity 3: Classifying galaxies ...................................................................................................................... 9 Activity 4: The colours of galaxies .............................................................................................................. 12 Activity 5: Galaxies in different light ............................................................................................................ 14 Extension activity: Evolution of galaxies .......................................................... 19 The Secrets of Galaxies 3 CESAR Science Case The Secrets of Galaxies 4 CESAR Science Case Background A century ago, astronomers believed that our Galaxy, the Milky Way , was the entire Universe. In the 1910s and early 1920s there was much debate about whether the ‘spiral nebulae’ (spiral shaped, milky patches of light)
    [Show full text]
  • DSO List V2 Current
    7000 DSO List (sorted by name) 7000 DSO List (sorted by name) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs Dist SAC NOTES M 1 NGC 1952 SN Rem TAU 8.4 11 8' 05 34.5 +22 01 135 6.3k Crab Nebula; filaments;pulsar 16m;3C144 M 2 NGC 7089 Glob CL AQR 6.5 11 11.7' 21 33.5 -00 49 255 II 36k Lord Rosse-Dark area near core;* mags 13... M 3 NGC 5272 Glob CL CVN 6.3 11 18.6' 13 42.2 +28 23 110 VI 31k Lord Rosse-sev dark marks within 5' of center M 4 NGC 6121 Glob CL SCO 5.4 12 26.3' 16 23.6 -26 32 336 IX 7k Look for central bar structure M 5 NGC 5904 Glob CL SER 5.7 11 19.9' 15 18.6 +02 05 244 V 23k st mags 11...;superb cluster M 6 NGC 6405 Opn CL SCO 4.2 10 20' 17 40.3 -32 15 377 III 2 p 80 6.2 2k Butterfly cluster;51 members to 10.5 mag incl var* BM Sco M 7 NGC 6475 Opn CL SCO 3.3 12 80' 17 53.9 -34 48 377 II 2 r 80 5.6 1k 80 members to 10th mag; Ptolemy's cluster M 8 NGC 6523 CL+Neb SGR 5 13 45' 18 03.7 -24 23 339 E 6.5k Lagoon Nebula;NGC 6530 invl;dark lane crosses M 9 NGC 6333 Glob CL OPH 7.9 11 5.5' 17 19.2 -18 31 337 VIII 26k Dark neb B64 prominent to west M 10 NGC 6254 Glob CL OPH 6.6 12 12.2' 16 57.1 -04 06 247 VII 13k Lord Rosse reported dark lane in cluster M 11 NGC 6705 Opn CL SCT 5.8 9 14' 18 51.1 -06 16 295 I 2 r 500 8 6k 500 stars to 14th mag;Wild duck cluster M 12 NGC 6218 Glob CL OPH 6.1 12 14.5' 16 47.2 -01 57 246 IX 18k Somewhat loose structure M 13 NGC 6205 Glob CL HER 5.8 12 23.2' 16 41.7 +36 28 114 V 22k Hercules cluster;Messier said nebula, no stars M 14 NGC 6402 Glob CL OPH 7.6 12 6.7' 17 37.6 -03 15 248 VIII 27k Many vF stars 14..
    [Show full text]