DOCSLIB.ORG

A Study of HI-Selected Galaxies in the Hercules Cluster

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
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. Sensitive single-dish H i line spectra were obtained for 20 of them, and for one (47-154) the VLA detection was not confirmed. Optical surface photometry was obtained of 10 objects, for 8 of which optical spectroscopy was obtained as well. Based on various selection criteria, two (ce-143 and ne-204) can be classified as dwarfs. The objects of which optical observations were made show star formation properties similar to those of published samples of actively star forming galaxies, and approximately half of them have properties intermediate between those of dwarf galaxies and low-luminosity disc galaxies. No optical redshifts could be obtained for two of the galaxies (sw-103 and sw-194) and their physical association with the H i clouds detected at their positions therefore remains uncertain. Unique among the objects is the Tidal Dwarf Galaxy ce-061 in a tail of the IC 1182 merger system. arXiv:astro-ph/0304287v1 15 Apr 2003 Key words. galaxies: abundances – galaxies: dwarf – galaxies: clusters: general – galaxies: clusters: individual: Hercules cluster 1. Introduction oxygen abundance significantly higher than expected from the luminosity-metallicity relation for field dwarf galaxies. It is well known from numerous studies based on ob- i servations and simulations that the environment plays a In this paper we present single-dish 21 cm H -line as fundamental role in the evolution of bright galaxies, via well as optical imaging and spectroscopy observations of galaxy-galaxy interactions and/or interactions of galax- a sample of galaxies in the Hercules cluster, selected from i ies with the intergalactic medium. The present work is the objects detected in the blind VLA H line survey of the part of an ongoing study of the properties of H i-selected cluster by Dickey (1997). One of our aims is to examine galaxies in clusters, for which the results on dwarfs in the which of them can be considered dwarf galaxies. Hydra cluster have already been published (Duc et al. The Hercules supercluster is one of the most mas- 1999, 2001a; hereafter Paper I and II, respectively). The sive structures in the nearby Universe (Freudling 1995). most remarkable result is the existence of dwarfs with an It appears to be a collection of three clusters, grav- itationally bound, but far from dynamical relaxation: Send offprint requests to: [email protected] Abell 2151, classified as richness class 2, and Abell 2147 2 Iglesias-P´aramo et al. and Abell 2152, both classified as richness class 1 (Barmby with optical counterparts on the Digital Sky Survey (DSS) & Huchra 1998). In a previous single-dish study of the H i and showing line widths smaller than 270 km s−1 detected properties of a sample of galaxies in the Hercules super- in the 4 fields by D97, we observed the following 18 in cluster, Giovanelli et al. (1981) found a strong deficiency the H i line at Arecibo: ne-112, ne-142, ne-178, ne-204, in the H i mass-to-optical luminosity ratio of galaxies in ne-208, ne-240, ce-042, ce-048, ce-060, ce-061, ce-143, ce- the Abell 2147 cluster, while an almost normal, or mildly 176, ce-200, sw-103, sw-222, 47-138, 47-166 and 47-211. deficient, ratio was found for the galaxies in Abell 2151, The 7 others were ruled out because they are very likely the richest and densest of the three clusters. We have as- face-on spirals: ne-169, ne-222, ne-264, ce-122, ce-166, sw- sumed a distance of 150 Mpc to the Hercules supercluster, 159 and 47-030. In addition, we included in our list four based on an average redshift of 11,050 kms−1 for the clus- galaxies showing line widths larger than 270 km s−1 but ter spirals (see D97) and a Hubble constant of 75 km s−1 with only tentative optical counterparts on the DSS (ne- Mpc−1. 250, ne-398, sw-194 and 47-154) in order to confirm the H i The paper is organized as follows: the sample selection detections and to verify whether the optical associations and H i and optical observations are described in section 2. are real or not. A summary of the observations obtained The optical and H i properties of the sample galaxies are for our survey, together with the centre positions and W50 described insection 3, and a discussion of the results is line widths from D97, is given in Table 1. presented in section 4. Comments on individual objects For our optical imaging and spectroscopic observa- are given in an Appendix. tions, only the central (ce) and southern (sw) fields could be covered. 2. Observations 2.2. H I line observations 2.1. Sample selection We made our H i line observations of the 22 H i-selected Our study of the Hercules cluster is aimed at H i-selected galaxies in the Hercules cluster with the refurbished 305 m galaxies, as well as at reported H i clouds without optical Arecibo Gregorian radio telescope in May and June 2002. counterparts on Digital Sky Survey (DSS) images, selected For further technical details on the observations and the from the blind VLA 21 cm H i line survey of the cluster data reduction we refer to van Driel et al. (2003). by Dickey (1997, hereafter D97) and reobserved by us at The total net integration time (on+off) was on aver- Arecibo in order to confirm the detections and to obtain age 70 minutes per source, depending on the line strength, H i line profiles with a better velocity resolution. Our fail- from 40 minutes for the strongest lines to 110 minutes for ure to confirm the H i clouds without optical counterparts the weakest signals, in ne-398 and 47-154. The velocity indicate that these were spurious, as described in van Driel coverage is about 2500 kms−1, the velocity resolution is et al. (2003). 1.3 km s−1, and the telescope’s HPBW at 21 cm is 3.′4×3.′6. For our studies of H i-selected dwarf galaxies in the For the telescope’s pointing positions the centre coordi- Hydra cluster (Papers I and II) we used the VLA H i study nates of the VLA H i sources as given in D97 were used by McMahon (1993), which has a velocity resolution of 42 (see Table 1 of D97). The data were reduced using IDL kms−1, similar to that of the D97 survey. We selected routines developed at Arecibo Observatory. A first-order on H i line widths at 20% of peak flux density value, W20, baseline was then fitted to the data and the velocities were smaller than 130 km s−1, as objects with such narrow lines corrected to the heliocentric system, using the optical con- are good dwarf candidates. Of the 20 selected objects only vention. All data were boxcar smoothed to a velocity res- 4 were found not to be dwarfs. olution of 9.1 km s−1 for further analysis, while the data We could not apply such an effective H i line width of ne-398 and 47-154 were smoothed to 19.5 kms−1. criterion aimed at selecting dwarfs to the D97 data, how- ever. As the Hercules cluster is about three times more distant (150 Mpc) than the Hydra cluster (45 Mpc), the 2.3. Optical observations H i profiles are correspondingly weaker and their widths more uncertain. The D97 H i mass detection limit of about Our optical observations are limited to objects in the ce 8 5 10 M⊙ allows the detection of only the most gas-rich and sw fields of the D97 survey. Of all 10 sample galaxies dwarf systems, while we estimate that the uncertainty in in these two fields we obtained deep CCD images, and −1 the FWHM line widths, W50, is about 100 kms for the low-to-medium resolution spectra for the 8 among these fainter H i detections, following Fouqu´eet al.
Load more

Recommended publications
  • The Large–Scale Distribution of Galaxies in the Shapley Concentration
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The large{scale distribution of galaxies in the Shapley Concentration S. Bardelli Osservatorio Astronomico di Trieste, via Tiepolo 11, I{34131 Trieste, Italy E. Zucca, G. Zamorani Osservatorio Astronomico di Bologna, via Zamboni 33, I{40126 Bologna, Italy Abstract. We present the results of a galaxy redshift survey in the central region of the Shapley Concentration. Our total sample contains 2000 radial velocities of galaxies both in the clusters and in the inter- cluster∼ field. We reconstruct the density profile of this supercluster, cal- culate its overdensity and total mass. Moreover we detect a massive structure behind the Shapley Concentration, at 30000 km/s. ∼ 1. Introduction The Shapley Concentration stands out as the richest system of Abell clusters in the list of Zucca et al. (1993), at every density excess. In particular, at a density contrast of 2, it has 25 members (at mean velocity 14000 km/s), while at the same density∼ contrast the Great Attractor, which is∼ the largest mass 1 condensation within 80 h− Mpc, has only 6 members and the Corona Borealis and Hercules superclusters are formed by 10 and 8 clusters, respectively. While the cluster distribution in the Shapley Concentration has been well studied, little is known about the distribution of the galaxies. Determining the properties of these galaxies is very important in order to assess the physical reality and extension of the structure and to determine if galaxies and clusters trace the matter distribution in the same way.
    [Show full text]
  • Diplomarbeit Fossile Galaxiensysteme
    DIPLOMARBEIT Titel der Diplomarbeit Fossile Galaxiensysteme angestrebter akademischer Grad Magistra der Naturwissenschaften (Mag. rer. nat.) Verfasser: Eveline Glaßner Matrikel-Nummer: 9500110 Studienrichtung: Astronomie A413 Betreuer: Ao. Univ.-Prof. Dr. Werner Zeilinger Wien, Juni 2009 Zusammenfassung In meiner Arbeit wurden dynamische Endstadien von Galaxiensystemen, sog. Fos- sile Galaxiensysteme untersucht. Sie zeichnen sich durch eine massereiche zentrale Elliptische Galaxie aus, die von deutlich leuchtkraftschw¨acheren Galaxien umgeben ist. Diese Galaxien sind in einen diffusen, r¨aumlich ausgedehnten R¨ontgenhalo ein- gebettet, der auf ein ehemaliges Galaxiensystem schließen l¨asst. Insgesamt wurden 49 solcher Systeme untersucht, wobei nur 45 die Definition eines Fossilen Systems erfullen.¨ Die Auswahl setzt sich aus zwei Katalogen zusammen. Der erste Katalog stellt eine Zusammenfassung aller entdeckten Fossilen Systeme bis 2005 dar, der zweite stammt aus der Suche in der Sloan Digital Sky Survey im Jahre 2007. Als Erstes wurde die zentrale Elliptische Galaxie nach ihren photometrischen Eigen- schaften untersucht. Dies umfasst ein Fl¨achenhelligkeitsprofil, die Elliptizit¨at, den Positionswinkel und die Fourier-Koeffizienten h¨oherer Ordnung der Isophoten, die fur¨ die Bestimmung der Form (boxy bzw. disky) der Elliptischen Galaxie herange- zogen wurden. Es zeigt sich eine etwa gleichm¨aßige Aufteilung zwischen boxy und disky Elliptischen Galaxien. Der zweite Teil umfasst die spektrale Analyse der Elliptischen Galaxien. Weniger als die H¨alfte aller Elliptischen Galaxien zeigen nukleare Aktivit¨aten. Der dritte Schwerpunkt befasst sich mit der Analyse der Umgebung Fossiler Sys- teme. Bis zu einem Radius von 5 Mpc ausgehend von der zentralen Elliptischen Galaxie wurde nach weiteren Galaxien mit spektral bestimmten Rotverschiebungen gesucht. Dasselbe erfolgte auch fur¨ benachbarte Galaxiensysteme.
    [Show full text]
  • Arxiv:1305.7264V2 [Astro-Ph.EP] 21 Apr 2014 Spain
    Draft version September 18, 2018 Preprint typeset using LATEX style emulateapj v. 08/22/09 THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE YEARS Timothy D. Brandt1, Masayuki Kuzuhara2, Michael W. McElwain3, Joshua E. Schlieder4, John P. Wisniewski5, Edwin L. Turner1,6, J. Carson7,4, T. Matsuo8, B. Biller4, M. Bonnefoy4, C. Dressing9, M. Janson1, G. R. Knapp1, A. Moro-Mart´ın10, C. Thalmann11, T. Kudo12, N. Kusakabe13, J. Hashimoto13,5, L. Abe14, W. Brandner4, T. Currie15, S. Egner12, M. Feldt4, T. Golota12, M. Goto16, C. A. Grady3,17, O. Guyon12, Y. Hayano12, M. Hayashi18, S. Hayashi12, T. Henning4, K. W. Hodapp19, M. Ishii12, M. Iye13, R. Kandori13, J. Kwon13,22, K. Mede18, S. Miyama20, J.-I. Morino13, T. Nishimura12, T.-S. Pyo12, E. Serabyn21, T. Suenaga22, H. Suto13, R. Suzuki13, M. Takami23, Y. Takahashi18, N. Takato12, H. Terada12, D. Tomono12, M. Watanabe24, T. Yamada25, H. Takami12, T. Usuda12, M. Tamura13,18 Draft version September 18, 2018 ABSTRACT We present results from the first three years of observations of moving group targets in the SEEDS high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of ∼105 at 100 and ∼106 beyond 200 around 63 proposed members of nearby kinematic moving groups. We review each of the kinematic associations to which our targets belong, concluding that five, β Pictoris (∼20 Myr), AB Doradus (∼100 Myr), Columba (∼30 Myr), Tucana-Horogium (∼30 Myr), and TW Hydrae (∼10 Myr), are sufficiently well-defined to constrain the ages of individual targets.
    [Show full text]
  • 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%.
    [Show full text]
  • 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
    [Show full text]
  • 195 9Apj. . .130. .629B the HERCULES CLUSTER OF
    .629B THE HERCULES CLUSTER OF NEBULAE* .130. G. R. Burbidge and E. Margaret Burbidge 9ApJ. Yerkes and McDonald Observatories Received March 26, 1959 195 ABSTRACT The northern of two clusters of nebulae in Hercules, first listed by Shapley in 1933, is an irregular group of about 75 bright nebulae and a larger number of faint ones, distributed over an area about Io X 40'. A set of plates of parts of this cluster, taken by Dr. Walter Baade with the 200-inch Hale reflector, is shown and described. More than three-quarters of the bright nebulae have been classified, and, of these, 69 per cent are spirals or irregulars and 31 per cent elliptical or SO. Radial velocities for 7 nebulae were obtained by Humason, and 10 have been obtained by us with the 82-inch reflector. The mean red shift is 10775 km/sec. From this sample, the total kinetic energy of the nebulae has been esti- mated. By measuring the distances between all pairs on a 48-inch Schmidt enlargement, the total poten- tial energy has been estimated. From these results it is concluded that, if the cluster is to be in a stationary state, the average galactic mass must be ^1012Mo. Three possibilities are discussed: that the masses are indeed as large as this, that there is a large amount of intergalactic matter, and that the cluster is expanding. The data for the Coma and Virgo clusters are also reviewed. It is concluded that both the Hercules and the Virgo clusters are probably expanding, but the situation is uncertain in the case of the Coma cluster.
    [Show full text]
  • Radio Investigations of Clusters of Galaxies
    • • RADIO INVESTIGATIONS OF CLUSTERS OF GALAXIES a study of radio luminosity functions, wide-angle head-tailed radio galaxies and cluster radio haloes with the Westerbork Synthesis Radio Telescope proefschrift ter verkrijging van degraad van Doctor in de Wiskunde en Natuurwetenschappen aan de Rijksuniversiteit te Leiden, op gezag van de Rector Magnificus Or. D.J. Kuenen, hoogleraar in de Faculteit der Wiskunde en Natuurwetenschappen, volgens besluit van het College van Dekanen te verdedigen op woensdag 20 december 1978 teklokke 15.15 uur door Edwin Auguste Valentijn geboren te Voorburg in 1952 Sterrewacht Leiden 1978 elve/labor vincit - Leiden Promotor: Prof. Dr. H. van der Laan aan Josephine aan mijn ouders Cover: Some radio contours (1415 MHz) of the extended radio galaxies NGC6034, NGC6061 and 1B00+1SW2 superimposed to a smoothed galaxy distribution (number of galaxies per unit area, taken from Shane) of the Hercules Superoluster. The 90 % confidence error boxes of the Ariel VandUHURU observations of the X-ray source A1600+16 are also included. In the region of overlap of these two error boxes the position of a oD galaxy is indicated. The combined picture suggests inter-galactic material pervading the whole superaluster. CONTENTS CHAPTER 1 GENERAL INTRODUCTION AND SUMMARY 9 PART 1 OBSERVATIONS OF THE COI1A CLUSTER AT 610 MHZ 15 CHAPTER 2 COMA CLUSTER GALAXIES 17 Observation of the Coma Cluster at 610 MHz (Paper III, with W.J. Jaffe and G.C. Perola) I Introduction 17 II Observations 18 III Data Reduction 18 IV Radio Source Parameters 19 V Optical Data 20 VI The Radio Luminosity Function of the Coma Cluster Galaxies 21 a) LF of the (E+SO) Galaxies 23 b) LF of the (S+I) Galaxies 25 c) Radial Dependence of the LF 26 VII Other Properties of the Detected Cluster Galaxies 26 a) Spectral Indexes b) Emission Lines VIII The Central Radio Sources 27 a) 5C4.85 = NGC4874 27 b) 5C4.8I - NGC4869 28 c) Coma C 29 CHAPTER 3 RADIO SOURCES IN COMA NOT IDENTIFIED WITH CLUSTER GALAXIES 31 Radio Data and Identifications (Paper IV, with G.C.
    [Show full text]
  • Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a Spinning Universe
    Journal of High Energy Physics, Gravitation and Cosmology, 2021, 7, 98-122 https://www.scirp.org/journal/jhepgc ISSN Online: 2380-4335 ISSN Print: 2380-4327 Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a Spinning Universe Puthalath Koroth Raghuprasad Independent Researcher, Odessa, TX, USA How to cite this paper: Raghuprasad, P.K. Abstract (2021) Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a This is the final article in our series dealing with the interplay of spin and Spinning Universe. Journal of High Energy gravity that leads to the generation, and continuation of celestial body mo- Physics, Gravitation and Cosmology, 7, tions in the universe. In our prior studies we focused on such interactions in 98-122. https://doi.org/10.4236/jhepgc.2021.71005 the elementary particles, and in the celestial bodies in the solar system. Fore- most among the findings was that, along with gravity, matter at all levels ex- Received: March 23, 2020 hibits axial spin. We further noted that all freestanding bodies outside our Accepted: December 19, 2020 solar system, including the largest such units, the stars and galaxies also spin Published: December 22, 2020 on their axes. Also, the axial rotation speed of planets in our solar system has Copyright © 2021 by author(s) and a linear positive relationship to their masses, thus hinting at its fundamental Scientific Research Publishing Inc. and autonomous nature. We have reported that this relationship between the This work is licensed under the Creative size of the body and its axial rotation speed extends to the stars and even the Commons Attribution International License (CC BY 4.0).
    [Show full text]
  • FY13 High-Level Deliverables
    National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................
    [Show full text]
  • 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).
    [Show full text]
  • 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,
    [Show full text]
  • Youth Capture the Colorful Cosmos Ii: Star Stories of the Dawnland
    YOUTH CAPTURE THE COLORFUL COSMOS II: STAR STORIES OF THE DAWNLAND The Abbe Museum, in association with the Smithsonian Institution, is pleased to participate in the Youth Capture the Colorful Cosmos II (YCCC II) program. By partnering with schools in the Wabanaki communities, students have the opportunity to research, learn about, and photograph the cosmos using telescopes owned and maintained by the Harvard-Smithsonian Center for Astrophysics. The MicroObservatory is a network of automated telescopes that can be controlled over the Internet. This network was developed by scientists and educators, and designed to enable youth nationwide to investigate the wonders of the deep sky. The remote observing network is composed of several three-foot-tall reflecting telescopes, each of which has a six- inch mirror to capture the light from distant objects in space. Instead of an eyepiece, the telescopes focus the collected light onto an electronic chip that records the image as a picture file. The goal of the YCCC II program is to use hands-on exercises to teach youth how to control the MicroObservatory robotic telescopes over the internet and take their own images of the universe. Here at the Abbe, the project also encouraged students to choose subjects based on Wabanaki stories about the stars. Each student had the opportunity to research traditional stories and interpret them in a modern context using 21st century technology. Originally beginning as an online exhibit featuring the Indian Township School, the Youth Capture the Colorful Cosmos exhibit features photos taken by children in the Passamaquoddy, Maliseet, Penobscot, and Micmac communities in Maine.
    [Show full text]