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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. -
Arxiv:Astro-Ph/0606633V2 4 Jul 2006
submitted to Astrophysical Journal Letters Preprint typeset using LATEX style emulateapj v. 6/22/04 A CURIOUS NEW MILKY WAY SATELLITE IN URSA MAJOR0 D. B. Zucker1, V.Belokurov1, N.W.Evans1, J. T. Kleyna2, M. J. Irwin1,M.I.Wilkinson1,M.Fellhauer1,D.M.Bramich1,G.Gilmore1, H. J. Newberg3,B.Yanny4,J.A.Smith5,6,P.C.Hewett1,E.F.Bell7, H.-W. Rix7, O.Y. Gnedin8,S.Vidrih1,R.F.G.Wyse9,B.Willman10, E. K. Grebel11,D.P.Schneider12,T.C.Beers13,A. Y.Kniazev7,14 J.C. Barentine15,H.Brewington15,J.Brinkmann15,M.Harvanek15, S.J. Kleinman16,J.Krzesinski15,17,D.Long15,A.Nitta18,S.A.Snedden15 submitted to Astrophysical Journal Letters ABSTRACT In this Letter, we study a localized stellar overdensity in the constellation of Ursa Major, first identified in Sloan Digital Sky Survey (SDSS) data and subsequently followed up with Subaru imaging. Its color-magnitude diagram (CMD) shows a well-defined sub-giant branch, main sequence and turn-off, from which we estimate a distance of ∼ 30 kpc and a projected size of ∼ 250 × 125 pc. The CMD suggests a composite population with some range in metallicity and/or age. Based on its extent and stellar population, we argue that this is a previously unknown satellite galaxy of the Milky Way, hereby named Ursa Major II (UMa II) after its constellation. Using SDSS data, we find an absolute magnitude of MV ∼ −3.8, which would make it the faintest known satellite galaxy. UMa II’s isophotes are irregular and distorted with evidence for multiple concentrations; this suggests that the satellite is in the process of disruption. -
A Photometric and Spectroscopic Study of the Southern Open Clusters Pismis 18, Pismis 19, Ngc 6005, and Ngc 6253 Andre S E
THE ASTRONOMICAL JOURNAL, 116:801È812, 1998 August ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. A PHOTOMETRIC AND SPECTROSCOPIC STUDY OF THE SOUTHERN OPEN CLUSTERS PISMIS 18, PISMIS 19, NGC 6005, AND NGC 6253 ANDRE S E. PIATTI1,2 AND JUAN J. CLARIA 2 Observatorio Astrono mico, Universidad Nacional de Co rdoba, Laprida 854, 5000 Co rdoba, Argentina; andres=oac.uncor.edu, claria=oac.uncor.edu EDUARDO BICA2 Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, C.P. 15051, Porto Alegre, 91500-970, RS, Brazil; bica=if.ufrgs.br DOUG GEISLER Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, AZ 85726; doug=noao.edu AND DANTE MINNITI Lawrence Livermore National Laboratory, L-413, P.O. Box 808, Livermore, CA 94550; dminniti=igpp.llnl.gov Received 1997 October 3; revised 1998 April 24 ABSTRACT CCD observations in the B, V , and I passbands have been used to generate color-magnitude diagrams (CMDs) for the southern open cluster candidates Pismis 18, Pismis 19, and NGC 6005, as well as for the old open cluster NGC 6253. The sample consists of about 1550 stars reaching down to V D 19 mag. From analysis of the CMDs, the physical reality of the three cluster candidates is conÐrmed and their reddening, distance, and age are derived, as well as those of NGC 6253. In addition, integrated spectra for Pismis 18, Pismis 19, and NGC 6253 covering a range from 3500 to 9200A were obtained. The reddening, age, and metallicity of these three clusters were derived from Balmer and Ca II triplet equiva- lent widths by comparing the observed spectra with those of template clusters. -
The Metallicity of Palomar 1 1
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The metallicity of Palomar 1 1 A. Rosenberg Telescopio Nazionale Galileo, Osservatorio Astronomico di Padova, Italy G. Piotto, I. Saviane Dipartimento di Astronomia, Universit`a di Padova, Italy A. Aparicio Instituto de Astrof´ısica de Canarias, Spain R. Gratton Osservatorio Astronomico di Padova, Italy Received ; accepted 1Based on observations made with the Isaac Newton Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos and the IAC-80 Telescope operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide, both of the Instituto de Astrof´ısica de Canarias. –2– ABSTRACT Palomar 1 is a peculiar galactic globular cluster, suspected to be younger than the bulk of the Galactic halo objects. However, such a low age can be confirmed only after a reliable determination of the metallicity. In the present paper, we use the equivalent widths (W ) of the Ca II triplet on medium resolution spectra in order to determine the metal content of Pal 1. From the comparison of the luminosity corrected W ’s in four stars of Palomar 1 with those of a sample of stars in each of three calibration clusters (M2, M15, and M71), we derive [Fe/H]=−0.6 ± 0.2 on the Zinn & West (1984) scale or [Fe/H]=−0.7 ± 0.2 on the Carretta & Gratton (1997) scale. We also obtain a radial velocity Vr = −82.8 ± 3.3 Km/s for Pal 1. -
Astronomy & Astrophysics Integrated Photometric Characteristics of Galactic Open Star Clusters
A&A 388, 158–167 (2002) Astronomy DOI: 10.1051/0004-6361:20020450 & c ESO 2002 Astrophysics Integrated photometric characteristics of galactic open star clusters S. Lata1,A.K.Pandey1, R. Sagar1,2, and V. Mohan1 1 State Observatory, Manora peak, Nainital 263129, Uttaranchal, India e-mail: sneh, pandey, sagar, [email protected] 2 Indian Institute of Astrophysics, Bangalore 560034, India Received 19 November 2001 / Accepted 19 February 2002 Abstract. Integrated UBVRI photometric parameters of 140 galactic open clusters have been computed. Integrated I(V − R)0 and I(V − I)0 colours as well as integrated parameters for 71 star clusters have been obtained for the first time. These, in combination with published data, altogether 352 objects, are used to study the integrated photometric characteristics of the galactic open clusters. The I(MV ) values range from −9.0to 4 −1.0 mag corresponding to a range in total mass of the star clusters from ∼25 to 4×10 M . The integrated colours have a relatively narrow range, e.g., I(B − V )0 varies from −0.4 to 1.2 mag. The scatter in integrated colours at a given integrated magnitude can be understood in terms of differences in fraction of red giants/supergiants in the clusters. The observed integrated magnitudes and colours agree with the synthetic ones, except the dependences of I(V − R)0 and I(V − I)0 colours for clusters younger than ∼100 Myrs and also of the integrated magnitudes of oldest clusters. The large sample provides the most accurate age dependence of integrated magnitudes and colours determined so far. -
На Правах Рукописи Удк 524.3, 524.4, 524.6 Глушкова Елена
МОСКОВСКИЙ ГОСУДАРСТВЕННЫЙ УНИВЕРСИТЕТ имени М.В. ЛОМОНОСОВА ГОСУДАРСТВЕННЫЙ АСТРОНОМИЧЕСКИЙ ИНСТИТУТ имени П.К. ШТЕРНБЕРГА На правах рукописи УДК 524.3, 524.4, 524.6 Глушкова Елена Вячеславовна КОМПЛЕКСНОЕ ИССЛЕДОВАНИЕ РАССЕЯННЫХ ЗВЁЗДНЫХ СКОПЛЕНИЙ ГАЛАКТИКИ Специальность 01.03.02 ± астрофизика и звёздная астрономия Диссертация на соискание ученой степени доктора физико-математических наук Москва ± 2014 1 Оглавление Введение ...................................................................................................................................................4 Глава 1. Собственные движения и лучевые скорости РЗС..................................................................19 1.1. Абсолютные собственные движения..........................................................................................19 1.1.1 Абсолютизация собственных движений звёзд в 21 рассеянном скоплении.....................20 1.1.2 Оценка ошибок каталога 4М...............................................................................................27 1.1.3 Оценка параметров кривой вращения по собственным движениям 21 РЗС....................28 1.1.4 Абсолютные собственные движения 181 молодого скопления.........................................28 1.1.5 Кривая вращения подсистемы молодых рассеянных скоплений......................................37 1.1.6 Каталог абсолютных собственных движений РЗС.............................................................38 1.1.7 Членство звёзд в скоплениях...............................................................................................39 -
The Star Clusters Young & Old Newsletter
SCYON The Star Clusters Young & Old Newsletter edited by Holger Baumgardt, Ernst Paunzen and Pavel Kroupa SCYON can be found at URL: http://astro.u-strasbg.fr/scyon SCYON Issue No. 34 16 July 2007 EDITORIAL Here is the 34th issue of the SCYON newsletter. The current issue contains 35 abstracts from refereed journals, and an announcement for the MODEST-8 meeting in Bonn in December. The next issue will be sent out in September. We wish everybody a productive summer... Thank you to all those who sent in their contributions. Holger Baumgardt, Ernst Paunzen and Pavel Kroupa ................................................... ................................................. CONTENTS Editorial .......................................... ...............................................1 SCYON policy ........................................ ...........................................2 Mirror sites ........................................ ..............................................2 Abstract from/submitted to REFEREED JOURNALS ........... ................................3 1. Star Forming Regions ............................... ........................................3 2. Galactic Open Clusters............................. .........................................6 3. Galactic Globular Clusters ......................... ........................................16 4. Galactic Center Clusters ........................... ........................................23 5. Extragalactic Clusters............................ ..........................................24 -
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 -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Deep Sky Explorer Atlas
Deep Sky Explorer Atlas Reference manual Star charts for the southern skies Compiled by Auke Slotegraaf and distributed under an Attribution-Noncommercial 3.0 Creative Commons license. Version 0.20, January 2009 Deep Sky Explorer Atlas Introduction Deep Sky Explorer Atlas Reference manual The Deep Sky Explorer’s Atlas consists of 30 wide-field star charts, from the south pole to declination +45°, showing all stars down to 8th magnitude and over 1 000 deep sky objects. The design philosophy of the Atlas was to depict the night sky as it is seen, without the clutter of constellation boundary lines, RA/Dec fiducial markings, or other labels. However, constellations are identified by their standard three-letter abbreviations as a minimal aid to orientation. Those wishing to use charts showing an array of invisible lines, numbers and letters will find elsewhere a wide selection of star charts; these include the Herald-Bobroff Astroatlas, the Cambridge Star Atlas, Uranometria 2000.0, and the Millenium Star Atlas. The Deep Sky Explorer Atlas is very much for the explorer. Special mention should be made of the excellent charts by Toshimi Taki and Andrew L. Johnson. Both are free to download and make ideal complements to this Atlas. Andrew Johnson’s wide-field charts include constellation figures and stellar designations and are highly recommended for learning the constellations. They can be downloaded from http://www.cloudynights.com/item.php?item_id=1052 Toshimi Taki has produced the excellent “Taki’s 8.5 Magnitude Star Atlas” which is a serious competitor for the commercial Uranometria atlas. His atlas has 149 charts and is available from http://www.asahi-net.or.jp/~zs3t-tk/atlas_85/atlas_85.htm Suggestions on how to use the Atlas Because the Atlas is distributed in digital format, its pages can be printed on a standard laser printer as needed. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Pegasus Pegasus
Lateinischer Name: Deutscher Name: Peg Pegasus Pegasus Atlas Karte (2000.0) Kulmination um Cambridge Star :7, 13 Mitternacht: Atlas Benachbarte 4, 9, 16, Sternbilder: Sky Atlas : 17 And Aqr Cyg Del Equ 1. September Lac Psc Vul Deklinationsbereich: 2° ... 37° Fläche am Himmel: 1121° 2 Mythologie und Geschichte: Pegasus, oder Pegasos, ist das berühmte geflügelte Pferd, das Kind der Medusa, gezeugt von Poseidon, dem Gott der Weltmeere. Die Medusa war eine der Gorgonen, welche Schlangen statt Haare trugen und deren grausiger Anblick einen versteinern ließen. Perseus hatte die Medusa enthauptet und aus dem abgeschlagenen Hals sprang Pegasos mit blutbespritzter Mähne hervor. Pegasos lebte am Wohnsitz der Götter, er trug für Zeus die Blitze und die Donner und nur der Held Bellerophontes konnte es einst mit einem goldenen Zaumzeug zähmen, das ihm Athene, die Göttin der Wissenschaft und Kunst, schenkte. Unglaubliche Taten und Abenteuer hat Bellerophontes mit seinem Pegasos bestanden, ja sogar die Chimaira hat er besiegt und erlegt, jenes Ungeheuer der griechischen Sage, welches ein feuerspeiendes Löwenhaupt auf einem Ziegen- und Drachenkörper trug. Doch als Bellerophontes in seinem Übermut auf dem Pegasos sogar den Himmel erstürmen wollte, da hat er offenbar das goldene Zaumzeug der Athene missbraucht, denn das Pferd schüttelte ihn ab und kehrte zum Wohnsitz der Götter zurück. Pegasus , das Geflügelte Pferd , Equus Ales (ales = geflügelt), Cornipes (hornfüssig, hufetragend), Sonipes (mit tönendem Fuße, Ross), Sonipes Ales , Equus Pegasus , Pegasus Equus alatus und Bellerophon waren einige Bezeichnungen, die dieses Sternbild trug. [bk20 ] Sternbild: Pegasus ist mit einer Fläche von 1121 Quadratgrad ein großes, aber weniger auffälliges Sternbild. Das markanteste ist das große Pegasus-Rechteck mit einem kleinen, gleichseitigen Dreieck an dessen nordwestlichen Ecke.