Cluster-Cluster Lensing in Abell 2152
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Galaxy Cluster's Rotation
Mon. Not. R. Astron. Soc. 000, 000{000 (0000) Printed 14 June 2018 (MN LATEX style file v2.2) Galaxy cluster's rotation M. Manolopoulou1;2?, M. Plionis2;3 1 Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK. 2 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, Aristotle University of Thessaloniki, 54 124, Thessaloniki, Greece. 3 Instituto Nacional de Astrof´ısica Optica y Electr´onica, AP 51 y 216, 72000, Puebla, M´exico. 14 June 2018 ABSTRACT We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algo- rithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z . 0:1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure ve- locities for rotation, provided by our Monte-Carlo simulation analysis, we find that ∼ 23% of our clusters are rotating under a set of strict criteria. Loosening the strict- ness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ∼ 28%. -
Curriculum Vitae John P
Curriculum Vitae John P. Blakeslee National Research Council of Canada Phone: 1-250-363-8103 Herzberg Astronomy & Astrophysics Programs Fax: 1-250-363-0045 5071 West Saanich Road Cell: 1-250-858-1357 Victoria, B.C. V9E 2E7 Email: [email protected] Canada Citizenship: USA Education 1997 Ph.D., Physics, Massachusetts Institute of Technology (supervisor: Prof. John Tonry) 1991 B. A., Physics, University of Chicago (Honors; supervisor: Prof. Donald York) Employment History 2007 – present Astronomer, Senior Research Officer NRC Herzberg Institute of Astrophysics 2008 – present Adjunct Associate Professor Department of Physics, University of Victoria 2008 – 2013 Adjunct Professor Washington State University 2005 – 2007 Assistant Professor of Physics Washington State University 2004 – 2005 Research Scientist Johns Hopkins University 2000 – 2004 Associate Research Scientist Johns Hopkins University 1999 – 2000 Postdoctoral Research Associate University of Durham, U.K. 1996 – 1999 Fairchild Postdoctoral Scholar California Institute of Technology Fellowships and Awards 2004 Ernest F. Fullam Award for Innovative Research in Astronomy, Dudley Observatory 2003 NASA Certificate for contributions to the success of HST Servicing Mission 3B 1996 – 1999 Sherman M. Fairchild Postdoctoral Fellowship in Astronomy, Caltech Professional Service 2016 – present Canadian Large Synoptic Survey Telescope (LSST) Consortium, Co-PI 2014 – present Chair, NOAO Time Allocation Committee (TAC) Extragalactic Panel 2008 – present National Representative, Gemini International -
Interstellarum 40 Erreicht Die Heftzahl Der Neuen Folge Nun Gleich- Stand Mit Den Ausgaben Der Früheren Deep-Sky-Zeitschrift
fokussiert Liebe Leserinnen, liebe Leser, 20 Hefte Zeitschrift für praktische Astronomie Als interstellarum sich mit der Ausgabe 20 vom »Magazin für Deep-Sky- Beobachter« zur »Zeitschrift für praktische Astronomie« wandelte, gab es nicht nur positive Kommentare, wie die Leserbriefe in Heft 21 zeigten. Mit interstellarum 40 erreicht die Heftzahl der neuen Folge nun Gleich- stand mit den Ausgaben der früheren Deep-Sky-Zeitschrift. Im Rückblick zeigt sich, wie richtig der damals auch in der Redaktion viel diskutierte Schritt war: interstellarum konnte seine Aufl age seit 2001 vervierfachen. Für Heft 40 wurde diese noch einmal erhöht – diese Ausgabe geht mit knapp 9000 Heften in den Handel. Dort ist interstellarum inzwischen in Deutschland, Österreich, der Schweiz und Italien am Kiosk erhältlich. Astrofotografen für interstellarum Einen besonderen Anteil am Erfolg von interstellarum haben die zahl- reichen Astrofotografen, die die Illustration jeder Ausgabe mit großarti- gen Fotos ermöglichen. Um ihr Engagement zu honorieren, heben wir ab sofort die Namen derjenigen Astrofotografen im Impressum (Seite 78) hervor, die interstellarum regelmäßig ihre Aufnahmen einsenden. Die Redaktion möchte damit auch andere führende Astrofotografen einla- den, ihre Bildergebnisse der Zeitschrift zur Verfügung zu stellen. Weitere Informationen zu unserem Angebot für Astrofotografen können Sie im Internet unter www.interstellarum.de nachlesen. Stefan Seip Südhimmel-Sehnsucht Das Kreuz des Südens, Omega Centauri, die Magellanschen Wolken – wer träumt nicht von einer Exkursion zu den spektakulären Zielen des südlichen Sternhimmels, die bei uns immer unsichtbar bleiben? In einem zweiteiligen Artikel huldigen wir dem Südhimmel und seinen schönsten Deep-Sky-Objekten mit Astrofotos und Zeichnungen gleichermaßen. Las- sen Sie sich vom Südhimmel-Virus anstecken und mitnehmen auf eine Reise zu Katzenpfoten, Kohlensack und Käfernebel (Seite 50). -
Cross Identification Between X-Ray and Optical Clusters of Galaxies In
Draft version November 8, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 CROSS IDENTIFICATION BETWEEN X-RAY AND OPTICAL CLUSTERS OF GALAXIES IN THE SDSS DR7 FIELD Lei Wang1, Xiaohu Yang 1, Wentao Luo1, Erwin T. Lau1,2, Yu Wang3, H.J. Mo4, Frank C. van den Bosch5, Q.D. Wang4 Draft version November 8, 2018 ABSTRACT We use the ROSAT all sky survey X-ray cluster catalogs and the optical SDSS DR7 galaxy and group catalogs to cross-identify X-ray clusters with their optical counterparts, resulting in a sample of 201 X-ray clusters in the sky coverage of SDSS DR7. We investigate various correlations between the optical and X-ray properties of these X-ray clusters, and find that the following optical properties are correlated with the X-ray luminosity: the central galaxy luminosity, the central galaxy mass, the 0.43 0.46 characteristic group luminosity (∝ LX ), the group stellar mass (∝ LX ), with typical 1-σ scatter of ∼ 0.67 in log LX. Using the observed number distribution of X-ray clusters, we obtain an unbiased scaling relation between the X-ray luminosity, the central galaxy stellar mass and the characteristic satellite stellar mass as log LX = −0.26+2.90[log(M∗,c+0.26Msat)−12.0] (and in terms of luminosities, as log LX = −0.15+2.38[log(Lc +0.72Lsat) − 12.0]). We find that the systematic difference between different halo mass estimations, e.g., using the ranking of characteristic group stellar mass or using the X-ray luminosity scaling relation can be used to constrain cosmology. -
A Study of HI-Selected Galaxies in the Hercules Cluster
Astronomy & Astrophysics manuscript no. ms October 29, 2018 (DOI: will be inserted by hand later) A study of HI-selected galaxies in the Hercules cluster J. Iglesias-P´aramo1, W. van Driel2, P.-A. Duc3, P. Papaderos4, J.M. V´ılchez5, V. Cayatte2, C. Balkowski2, K. O’Neil6, J. Dickey7, H. Hern´andez6, and T.X. Thuan8 1 Laboratoire d’Astrophysique de Marseille, Traverse du Siphon - Les Trois Lucs, 13376 Marseille, France e-mail: [email protected] 2 Observatoire de Paris, GEPI, CNRS-UMR 8111 and Universit´e Paris 7, 92195 Meudon Cedex, France e-mail: [email protected],[email protected], [email protected] 3 CNRS URA 2052 and CEA, DSM, DAPNIA, Service d’Astrophysique, 91191 Gif-sur-Yvette Cedex, France e-mail: [email protected] 4 Universit¨ats-Sternwarte, Geismarlandstrasse 11, 37083 G¨ottingen, Germany e-mail: [email protected] 5 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Granada, Spain e-mail: [email protected] 6 Arecibo Observatory, HC3 Box 53995, Arecibo, Puerto Rico 00612, U.S.A. e-mail: [email protected], [email protected] 7 Department of Astronomy, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455, U.S.A. e-mail: [email protected] 8 Astronomy Department, University of Virginia, Charlottesville, VA 22903, U.S.A. e-mail: [email protected] Submitted to Astronomy and Astrophysics – second revised version 17.2.2003 Abstract. The present study is aimed at a sample of 22 galaxies detected in the blind VLA H i survey of the Hercules cluster by Dickey (1997), 18 of which were selected on an H i line width smaller than 270 km s−1 and 4 others with only tentative optical counterparts on the Palomar Sky Survey. -
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 -
Annual Report / Rapport Annuel / Jahresbericht 1998
Annual Report / Rapport annuel / Jahresbericht 1998 EUROPEAN SOUTHERN OBSERVATORY COVER COUVERTURE UMSCHLAG Impressive images were obtained soon after Des images impressionnantes ont été reçues Beeindruckende Aufnahmen wurden ge- the multi-mode VLT Infrared Spectrometer peu de temps après l’installation de l’ins- macht kurz nachdem im November 1998 And Array Camera (ISAAC) instrument trument multi-mode ISAAC (« Infrared das Multimodus-Instrument ISAAC („Infra- was mounted at the first VLT 8.2-m Unit Spectrometer And Array Camera») au pre- red Spektrometer And Array Camera“) am mier télescope VLT de 8,2 mètres (UT1) en Telescope (UT1) in November 1998. This ersten der VLT-Teleskope (UT1) installiert colour composite image of the RCW38 star- novembre 1998. Cette image couleur com- worden war. Diese Farbaufnahme des forming complex combines Z (0.95 µm), H posite du complexe de formation stellaire (1.65 µm) and Ks (2.16 µm) exposures of a RCW38 combine des images prises en Z Sternentstehungsgebiets RCW38 ist zusam- few minutes each. Stars which have recent- (0,95 µm), H (1,65 µm) et Ks (2,16 µm), mengesetzt aus Einzelaufnahmen in Z (0,95 ly formed in clouds of gas and dust in this ayant un temps d’exposition de quelques µm), H (1,65 µm) und Ks (2,16 µm) von je region 5000 light-years away are still heav- minutes chacune. Les étoiles, récemment einigen Minuten Belichtungszeit. Die vor ily obscured and cannot be seen at optical formées dans les nuages de gaz et de pous- kurzem in den Gas- und Staubwolken dieser wavelengths but become visible at infrared sières dans cette région éloignée de 5000 5000 Lichtjahre entfernten Gegend ent- wavelengths where the obscuration is sub- années-lumière, sont extrêmement enfouies standenen Sterne sind immer noch stark stantially lower. -
Édition Juin 2013 « DU SAVOIR AU VÉCU »
Édition juin 2013 « DU SAVOIR AU VÉCU » Le petit nouveau, une réalisation de Pierre Carignan Page 1 sur 47 SOMMAIRE Le mot de l’éditeur ................................................................................................ 4 Événements, nouvelles et anecdotes ................................................................... 6 Le Club Véga à la Journée mondiale de l’astronomie ................................................. 6 Histoire d’une passion ................................................................................................. 6 Colloque du RCAQ ....................................................................................................... 6 Observatoire du Mont Mégantic, 35 ans d’astronomie .............................................. 7 Le ROS un reportage photos de Martin ....................................................................... 8 Encore des photos du ROS .......................................................................................... 9 Une invitation au Mont Mégantic ............................................................................... 9 L’observatoire de Pierre Carignan bientôt à St-Pierre .............................................. 10 Jeune astronome amateur honoré au Club Véga ...................................................... 11 Invitation à la journée de la découverte ................................................................... 12 Conférence de Martin Roy sur le Soleil ..................................................................... 13 -
Colors, Ages, and Metallicities of Galaxies in Six Nearby Galaxy Clusters
Journal of The Korean Astronomical Society 41: 109 » 119, 2008 October ⃝c 2008 The Korean Astronomical Society. All Rights Reserved. COLORS, AGES, AND METALLICITIES OF GALAXIES IN SIX NEARBY GALAXY CLUSTERS Jong Chul Lee, Myung Gyoon Lee, and Taehyun Kim Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea E-mail: [email protected], [email protected], & [email protected] (Received July 15, 2008; Accepted October 14, 2008 ) ABSTRACT We present an optical-infrared photometric study of galaxies in six nearby clusters of galaxies at z=0.041»0.098 (A1436, A1773, A1809, A2048, A2142, and A2152). Using BV I photometry obtained at the Bohyunsan Optical Astronomical Observatory and JHKS photometry extracted from the 2-Micron All-Sky Survey catalog, we investigate the colors of galaxies in the clusters. Using the (B ¡ V ) versus (I ¡ KS) color-color diagrams in comparison with the simple stellar population model, we estimate the ages and metallicities of bright early-type member galaxies. Early-type galaxies in each cluster show the color-magnitude relation. Ages and metallicities of early-type members show little dependence on their velocity dispersions. Mean ages of early-types in the clusters range from 3 Gyr to 20 Gyr, showing a large dispersion, and mean metallicities range from Z = 0:03 to 0.05 above the solar value, showing a negligible dispersion. Key words : galaxy clusters : individual (A1436, A1773, A1809, A2048, A2142, and A2152) — galaxy : photometry — galaxy : color, age, and metallictiy — galaxy : formation and evolution I. INTRODUCTION more massive galaxies are more metal-rich, because they can retain gas for longer than less massive galax- One of the well-known observational properties of ies (Kodama et al. -
DSO List V2 Current
7000 DSO List (sorted by constellation - magnitude) 7000 DSO List (sorted by constellation - magnitude) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs SAC NOTES M 31 NGC 224 Galaxy AND 3.4 13.5 189' 00 42.7 +41 16 60 Sb Andromeda Galaxy;Local Group;nearest spiral NGC 7686 OCL 251 Opn CL AND 5.6 - 15' 23 30.1 +49 08 88 IV 1 p 20 6.2 H VIII 69;12* mags 8...13 NGC 752 OCL 363 Opn CL AND 5.7 - 50' 01 57.7 +37 40 92 III 1 m 60 9 H VII 32;Best in RFT or binocs;Ir scattered cl 70* m 8... M 32 NGC 221 Galaxy AND 8.1 12.4 8.5' 00 42.7 +40 52 60 E2 Companion to M31; Member of Local Group M 110 NGC 205 Galaxy AND 8.1 14 19.5' 00 40.4 +41 41 60 SA0 M31 Companion;UGC 426; Member Local Group NGC 272 OCL 312 Opn CL AND 8.5 - 00 51.4 +35 49 90 IV 1 p 8 9 NGC 7662 PK 106-17.1 Pln Neb AND 8.6 5.6 17'' 23 25.9 +42 32 88 4(3) 14 Blue Snowball Nebula;H IV 18;Barnard-cent * variable? NGC 956 OCL 377 Opn CL AND 8.9 - 8' 02 32.5 +44 36 62 IV 1 p 30 9 NGC 891 UGC 1831 Galaxy AND 9.9 13.6 13.1' 02 22.6 +42 21 62 Sb NGC 1023 group;Lord Rosse drawing shows dark lane NGC 404 UGC 718 Galaxy AND 10.3 12.8 4.3' 01 09.4 +35 43 91 E0 Mirach's ghost H II 224;UGC 718;Beta AND sf 6' IC 239 UGC 2080 Galaxy AND 11.1 14.2 4.6' 02 36.5 +38 58 93 SBa In NGC 1023 group;vsBN in smooth bar;low surface br NGC 812 UGC 1598 Galaxy AND 11.2 12.8 3' 02 06.9 +44 34 62 Sbc Peculiar NGC 7640 UGC 12554 Galaxy AND 11.3 14.5 10' 23 22.1 +40 51 88 SBbc H II 600;nearly edge on spiral MCG +08-01-016 Galaxy AND 12 - 1.0' 23 59.2 +46 53 59 Face On MCG +08-01-018 -
The Infrared Properties of Galaxy Clusters-IRAS Observations of The
THE ASTROPHYSICAL JOURNAL, 278:L75-L78, 1984 March 1 ""1984. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1984ApJ...278L..75Y THE INFRARED PROPERTIES OF GALAXY CLUSTERS: IRAS1 OBSERVATIONS OF THE HERCULES CLUSTER (ABELL 2151) E. YOUNG, B. T. SOIFER, F. J. Low, G. NEUGEBAUER, M. ROWAN-ROBINSON, G. MILEY, P. E. CLEGG, T. DE JONG, AND T. N. GAUTIER Received 1983September14; accepted 1983November18 ABSTRACT A total of 41 sources have been detected at 60 µ,m to a level of 50 mJy in a 1 ?6 x 0?5 field centered on the rich galaxy cluster Abell 2151. Twenty-four of these sources can be identified with late-type spiral galaxies of estimated photographic magnitude 17 or brighter. Galaxies classified as E or SO are notably absent in the infrared data. Within the field, eleven of the IRAS sources cannot be easily identified with galaxies in the Hercules Cluster. If the brightest 60 µ,m cluster source (NGC 6045) is neglected, the integral luminosity function in the far-infrared can be fitted well with two power laws of slope -1.1 and - 2.5. Subject headings: galaxies: clustering - infrared: sources I. INTRODUCTION No flux in Table 1 means an upper limit of 6 o. Uncertainties Abell 2151 is an excellent spiral-rich cluster for an initial in the absolute photometric calibration are estimated to be study at middle-infrared and far-infrared wavelengths of 30%. galaxies within a cluster. The individual galaxies are generally distinct at the IRAS angular resolution, yet the main part of III. -
A Giant Planet Candidate Transiting a White Dwarf
A Giant Planet Candidate Transiting a White Dwarf Andrew Vanderburg1;2;3, Saul A. Rappaport4, Siyi Xu5, Ian Crossfield6, Juliette C. Becker7;8, Bruce Gary9, Felipe Murgas10;11, Simon Blouin12, Thomas G. Kaye13;14, Enric Palle10;11, Carl Melis15, Brett M. Morris16, Laura Kreidberg17;18, Varoujan Gorjian19, Caroline V. Morley2, An- drew W. Mann20, Hannu Parviainen10;11, Logan A. Pearce21;22, Elisabeth R. Newton23, Andreia Carrillo2;24, Ben Zuckerman25, Lorne Nelson26, Greg Zeimann27, Warren R. Brown18, Rene´ Tronsgaard28, Beth Klein25, George R. Ricker4, Roland K. Vanderspek4, David W. Latham18, Sara Seager4;29;30, Joshua N. Winn31, Jon M. Jenkins32, Fred C. Adams33;34, Bjorn¨ Benneke35;36, David Berardo4, Lars A. Buchhave28, Douglas A. Caldwell37;32, Jessie L. Christiansen38, Karen A. Collins18, Knicole D. Colon´ 39, Tansu Daylan4;40, John Doty41, Alexandra E. Doyle42, Diana Dragomir43, Courtney Dressing44, Patrick Dufour35;36, Akihiko Fukui45;10, Ana Glidden4;29, Na- talia M. Guerrero4, Xueying Guo4, Kevin Heng16, Andreea I. Henriksen28, Chelsea X. Huang4;46, Lisa Kaltenegger47;48, Stephen R. Kane49, John A. Lewis18, Jack J. Lissauer32, Farisa Morales19;50, Norio Narita51;52;53;10;54, Joshua Pepper55, Mark E. Rose32, Jeffrey C. Smith37;32, Keivan G. Stassun56;57, Liang Yu58;4 1Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USA 2Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3NASA Sagan Fellow 4Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 5NSFs NOIRLab/Gemini Observatory, 670 N. Aohoku Place, Hilo, Hawaii, 96720, USA 6Dept. of Physics and Astronomy, University of Kansas, 1251 Wescoe Hall Dr., Lawrence, KS 66045, USA 7Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 851 Pegasi b Fellow 9Hereford Arizona Observatory, Hereford, AZ 85615, USA 10Instituto de Astrof´ısica de Canarias (IAC), E-38200 La Laguna, Tenerife, Spain 11Dept.