Atlas of Peculiar Galaxies by Halton Arp
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CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, -
HST Observations of Young Star Clusters in Interacting Galaxies
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Extragalactic Star Clusters IAU Symposium Series, Vol. Vol. 207, 2001 Eva K. Grebel, Doug Geisler, and Dante Minniti, eds. HST Observations of Young Star Clusters in Interacting Galaxies Kirk D. Borne Raytheon ITSS and NASA-GSFC, Code 631, Astrophysics Data Facility, Greenbelt, MD 20771 USA William C. Keel University of Alabama, Dept. of Physics and Astronomy, Tuscaloosa, AL 35487-0324 USA Philip N. Appleton & Curtis Struck Iowa State University, Dept. of Physics and Astronomy, Ames, IA 50011 USA RayA.Lucas&AlfredB.Schultz STScI, 3700 San Martin Drive, Baltimore, MD 21218 USA Abstract. We present early results from the analysis of HST imaging observations for several pairs of interacting galaxies. We include two cases that were specifically chosen to represent a strong early (young) encounter and a weak late (old) encounter. The goals of the project include a de- termination of the timing, frequency, strength, and characteristics of the young star clusters formed in these two limiting cases of tidal encounters. 1. Results from the Analysis of HST Imaging Observations Multi-band HST imaging data have been obtained for several interacting galaxy systems. These include the Cartwheel Ring Galaxy (Borne et al. 1996; Struck et al. 1996; Appleton et al., in preparation), Arp 81 and Arp 297 (Keel & Borne, in preparation), and a large sample of ULIRGs (Ultra-Luminous Infrared Galax- ies; Borne et al. 2000, and references therein). WFPC2 B-band (F450W) and I-band (F814W) images have been obtained for the Cartwheel, Arp 297, and Arp 81. -
Large-Scale Outflows in Edge-On Seyfert Galaxies. II. Kiloparsec
Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission Edward J. M. Colbert1,2, Stefi A. Baum1, Jack F. Gallimore1,2, Christopher P. O’Dea1, Jennifer A. Christensen1 Received ; accepted arXiv:astro-ph/9604022v1 3 Apr 1996 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 2 Department of Astronomy, University of Maryland, College Park, MD 20742 –2– ABSTRACT We present deep images of the kpc-scale radio continuum emission in 14 edge-on galaxies (ten Seyfert and four starburst galaxies). Observations were taken with the VLA at 4.9 GHz (6 cm). The Seyfert galaxies were selected from a distance-limited sample of 22 objects (defined in paper I). The starburst galaxies were selected to be well-matched to the Seyferts in radio power, recessional velocity and inclination angle. All four starburst galaxies have a very bright disk component and one (NGC 3044) has a radio halo that extends several kpc out of the galaxy plane. Six of the ten Seyferts observed have large-scale (radial extent >1 kpc) radio structures extending outward from the ∼ nuclear region, indicating that large-scale outflows are quite common in Seyferts. Large-scale radio sources in Seyferts are similar in radio power and radial extent to radio halos in edge-on starburst galaxies, but their morphologies do not resemble spherical halos observed in starburst galaxies. The sources have diffuse morphologies, but, in general, they are oriented at skewed angles with respect to the galaxy minor axes. This result is most easily understood if the outflows are AGN-driven jets that are somehow diverted away from the galaxy disk on scales >1 kpc. -
Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V
Astronomy Letters, Vol. 27, No. 4, 2001, pp. 207–212. Translated from Pis’ma v Astronomicheskiœ Zhurnal, Vol. 27, No. 4, 2001, pp. 243–249. Original Russian Text Copyright © 2001 by Dubrovich. Formation Mechanisms of “Negative”-Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V. K. Dubrovich* Special Astrophysical Observatory, Russian Academy of Sciences, pos. Nizhniœ Arkhyz, Stavropol kraœ, 357147 Russia Received June 2, 2000; in final form, October 2, 2000 Abstract—We consider the formation mechanisms of “negative”-intensity spots in the radio band for various astrophysical conditions. For wavelengths λ < 1.5 mm, the regions of reduced temperature (relative to the cos- mic microwave background radiation, CMBR) are shown to be produced only by high-redshift objects moving at peculiar velocities. The main processes are CMBR Thomson scattering and bremsstrahlung. We show that the effect δT/T can be ~ 10–5 in magnitude. We derive simple analytic expressions, which allow the redshifts, electron densities, and linear sizes of these regions to be estimated from observed spectral and spatial parame- ters. Additional observational methods for refining these parameters are outlined. © 2001 MAIK “Nauka/Inter- periodica”. Key words: theoretical and observational cosmology INTRODUCTION only two formation mechanisms of the “glow.” One of In the last 30 years, much attention has been given them is the Doppler distortion of external, equilibrium, to the search for and a detailed analysis of spatial fluc- and isotropic radiation (CMBR). For this to occur, the tuations in cosmic microwave background radiation object must have a peculiar velocity Vp and some non- zero opacity. -
Dust and CO Emission Towards the Centers of Normal Galaxies, Starburst Galaxies and Active Galactic Nuclei , I
A&A 462, 575–579 (2007) Astronomy DOI: 10.1051/0004-6361:20047017 & c ESO 2007 Astrophysics Dust and CO emission towards the centers of normal galaxies, starburst galaxies and active galactic nuclei, I. New data and updated catalogue M. Albrecht1,E.Krügel2, and R. Chini3 1 Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile e-mail: [email protected] 2 Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany 3 Astronomisches Institut der Ruhr-Universität Bochum (AIRUB), Universitätsstr. 150 NA7, 44780 Bochum, Germany Received 6 January 2004 / Accepted 27 October 2006 ABSTRACT Aims. The amount of interstellar matter in a galaxy determines its evolution, star formation rate and the activity phenomena in the nucleus. We therefore aimed at obtaining a data base of the 12CO line and thermal dust emission within equal beamsizes for galaxies in a variety of activity stages. Methods. We have conducted a search for the 12CO (1–0) and (2–1) transitions and the continuum emission at 1300 µmtowardsthe centers of 88 galaxies using the IRAM 30 m telescope (MRT) and the Swedish ESO Submillimeter Telescope (SEST). The galaxies > are selected to be bright in the far infrared (S 100 µm ∼ 9 Jy) and optically fairly compact (D25 ≤ 180 ). We have applied optical spectroscopy and IRAS colours to group the galaxies of the entire sample according to their stage of activity into three sub-samples: normal, starburst and active galactic nuclei (AGN). The continuum emission has been corrected for line contamination and synchrotron contribution to retrieve the thermal dust emission. -
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, -
An Analysis of the Environment and Gas Content of Luminous Infrared Galaxies
Abstract Title of Dissertation: An Analysis of the Environment and Gas Content of Luminous Infrared Galaxies Bevin Ashley Zauderer, Doctor of Philosophy, 2010 Dissertation directed by: Professor Stuart N. Vogel Department of Astronomy Luminous and ultraluminous infrared galaxies (U/LIRGs) represent a population among the most extreme in our universe, emitting an extraordinary amount of energy at infrared wavelengths from dust heated by prolific star formation and/or an active galactic nucleus (AGN). We present three investigations of U/LIRGs to better understand their global environment, their interstellar medium properties, and their nuclear region where molecular gas feeds a starburst or AGN. To study the global environment, we compute the spatial cluster-galaxy amplitude, Bgc, for 76 z < 0.3 ULIRGs. We find the environment of ULIRGs is similar to galaxies in the field. Comparing our results with other galactic populations, we conclude that ULIRGs might be a phase in the lives of AGNs and QSOs, but not all moderate-luminosity QSOs necessarily pass through a ULIRG phase. To study the interstellar medium properties, we observe H I and other spectral lines in 77 U/LIRGs with the Arecibo telescope. We detect H I in emission or absorption in 61 of 77 galaxies, 52 being new detections. We compute the implied gas mass for galaxies with emission, and optical depths and column densities for the seven sources with absorption detections. To study the molecular gas in the nuclear region of LIRG Arp 193, sub-arcsecond scale angular resolution is required and a method of atmospheric phase correction imperative. We present results of a large experiment observing bright quasars to test the limitations of the Combined Array for Research in Millimeter Astronomy’s Paired Antenna Calibration System (C-PACS) for atmospheric phase correction. -
Interstellarum 52 • Juni/Juli 2007 1 Inhalt
Editorial fokussiert Liebe Leserinnen und Leser, gibt es tatsächlich Planeten um andere Sterne, die die Vorrausset- zungen für die Entwicklung von Leben erfüllen? Eine derartige Mel- dung machte Ende April die Runde, als die ESO die Entdeckung eines Planeten in der »bewohnbaren«, weil möglicherweise die Existenz fl üs- sigen Wassers erlaubenden Zone um den Stern Gliese 581 bekanntgab (Seite 18). Solche Berichte machen den Eindruck, die Entdeckung von Leben in anderen Sonnensystemen stehe unmittelbar bevor – doch Daniel Fischers Blick hinter die Kulissen zeigt, dass wir noch am Anfang der Suche nach Exoplaneten stehen (Seite 12). Wenn interstellarum Teleskope testet, dann richtig – mit mehrmo- natigem Praxistest und optischer Bank. Diesmal stehen drei apochro- Ronald Stoyan, Chefredakteur matische Refraktoren der neuen Generation auf dem Prüfstand, die die Entscheidung besonders schwer machen – und die Beurteilung zu einem Vergnügen für den Tester. In diesem Heft steht die visuelle Leis- tungsfähigkeit im Vordergrund (Seite 50), in der kommenden Ausgabe werden die fotografi schen Fähigkeiten nachgereicht. Übrigens: Falls Sie einen Fernrohr-Kauf planen, empfehle ich Ihnen unsere Neuer- scheinung »Fernrohrwahl«. Dort sind praktisch alle auf dem deutschen Markt erhältlichen Modelle tabellarisch aufgelistet. Neu im Verlagsprogramm ist ebenfalls eine neue Ausgabe der inter- stellarum Archiv-CD, diesmal mit PDF-Dokumenten der Heftnummern 32 bis 49 – bestellbar über unsere Internetseite www.interstellarum.de. Dort laden wir Sie auch zur Teilnahme an der bisher größten Leserum- frage unserer Geschichte ein, denn wir wollen mehr über Sie und Ihre astronomischen Vorlieben erfahren – natürlich anonym. Bitte helfen Sie uns, interstellarum noch mehr auf Ihre Bedürfnisse auszurichten. Ihr Titelbild: Wie ein Planet eines anderen Sterns aussieht ist reine Spekulation – doch die künstlerische Darstellung der ESO hilft der Vorstellungskraft auf die Sprünge. -
The Role of Environment in Fueling Seyfert AGN
The Role of Environment in Fueling Seyfert AGN Erin K. S. Hicks University of Alaska Anchorage Francisco Müller-Sánchez (CASA), Matt Malkan (UCLA), Po-Chieh Yu (UCLA), Richard Davies (MPE) * Support from NSF AAG under award AST-1008042. UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs. Potential Seyfert AGN fueling mechanisms: i. Major mergers ii. Minor mergers iii. Accretion of gas streamers vi. Secular evolution Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs. Potential Seyfert AGN fueling mechanisms: i. Major mergers Several studies suggest not major mergers: ª Over 50% of z~2 AGN in undisturbed ii. Minor mergers host galaxies (Koceviski et al. 2012) ª AGN at z~2 not in galaxies with iii. Accretion of enhanced star formation (Rosario et gas streamers al. 2013) vi. Secular evolution Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs. Potential Seyfert AGN fueling mechanisms: i. Major mergers ª Minor mergers may be associated with low and intermediate luminosity AGN ii. Minor mergers (Neistein & Netzer 2014) ª Number required to account for iii. Accretion of dust in early type galaxies is gas streamers 250 times greater than predicted (Simões Lopes et al 2007, Martini et al 2013) vi. Secular evolution Erin K. S. Hicks IAU August 2015 UAA Goal: Trace inflow mechanisms on scales of Physics & Astronomy 1kpc down to tens of parsecs. Potential Seyfert AGN fueling mechanisms: i. -
Walter Scott Houston: MÉLY-ÉG CSODÁK 1975-1980 Sky And
Albireo Amat ırcsillagász Klub Walter Scott Houston: MÉLY-ÉG CSODÁK 1975-1980 Sky and Telescope Fordította: Szentmártoni Béla 1975. január Nemrég jártam újra Tucsonban, Arizónában, ahol 40 évvel ezel ıtt a csillagokat és ködöket fényesebbnek láttam, mint bármely más helyen. A Steward Observatory udvarában állva, szabadszemmel egykor 18 csillagot számoltam meg a Pleiades-ben, de ezen az éjjelen 1974- ben semmivel sem többet mint 5-öt. Az ok az volt, hogy épp miel ıtt besötétedett az ég, s őrő szmog felh ık ülepedtek rá a rézkohók fel ıl arra a természetes medencére, melyben Tucson elhelyezkedik. Telefonáltam Ronald Morale-nak, a következ ı éjszaka mi, valamint John Bartek és Daniel Knight mérföldekre kimentünk a sötét sivatagba, az Empire hegyekbe. 3 db 20 cm-es és egy 15 cm-es reflektort vittünk, s a tiszta égen a diffrakciós határig dolgoztak a m őszerek. Kezd ı objektumunk a 9 ½ mg NGC 891 volt, s átengedtük magunkat a gyönyörködésnek. A 20T-vel e 12 x 1’-es élér ıl látszó galaxis csaknem a fél LM-t átérte. Fényes volt és éles szélekkel bírt. De a nagy meglepetés EL-al jött el ıször, majd KL-al is, amint egy sötét ösvény látszott az orsó hosszán végig, s ez az ösvény határozott kagylókkal bírt a szélei mentén. Bár fényképek jól mutatják az NGC 891 porösvényét, ez volt az els ı alkalom, hogy láttam távcs ıvel. Az volt a célunk, hogy olyan objektumokat vizsgáljunk, melyek speciális észlelési problémákkal bírnak. A legtöbb kis távcs ıben az M 1 jobbára csak mint homályos 6x4’-es folt látszik, a 8 ½ mg összfényessége dacára. -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea -
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.