Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
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Lemmings &Ndash; I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 476, 3478–3522 (2018) doi:10.1093/mnras/sty342 Advance Access publication 2018 February 9 Downloaded from https://academic.oup.com/mnras/article-abstract/476/3/3478/4848304 by Southampton Oceanography Centre National Oceanographic Library user on 12 May 2020 LeMMINGs – I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi,1‹ D. R. A. Williams,1 I. M. McHardy,1 R. J. Beswick,2 M. K. Argo,2,3 B. T. Dullo,4 J. H. Knapen,5,6 E. Brinks,7 T. W. B. Muxlow,2 S. Aalto,8 A. Alberdi,9 G. J. Bendo,2,10 S. Corbel,11,12 R. Evans,13 D. M. Fenech,14 D. A. Green,15 H.-R. Klockner,¨ 16 E. Kording,¨ 17 P. Kharb, 18 T. J. Maccarone,19 I. Mart´ı-Vidal,8 C. G. Mundell,20 F. Panessa,21 A. B. Peck,22 M. A. Perez-Torres,´ 9 D. J. Saikia,18 P. Saikia,17,23 F. Shankar,1 R. E. Spencer,2 I. R. Stevens,24 P. Uttley25 and J. Westcott7 Affiliations are listed at the end of the paper Accepted 2018 February 2. Received 2018 January 19; in original form 2018 January 19 ABSTRACT We present the first data release of high-resolution (≤0.2 arcsec) 1.5-GHz radio images of 103 nearby galaxies from the Palomar sample, observed with the eMERLIN array, as part of the LeMMINGs survey. This sample includes galaxies which are active (low-ionization nuclear emission-line regions [LINER] and Seyfert) and quiescent (H II galaxies and absorption line galaxies, ALGs), which are reclassified based upon revised emission-line diagrams. -
Appendix A: the HRS+ Members
Appendix A: The HRS+ Members 207 Table A.1: The general properties of galaxies comprising the HRS+ sample. Each column contains: (1) the HRS+ identification 208 number; (2) an alternative name taken from either the New General Catalogue (NGC; Dreyer, 1888), the Catalogue of Galaxies and Clusters of Galaxies (CGCG; Zwicky et al., 1961), Uppsala General Catalogue (UGC; Nilson, 1973), the Virgo Cluster Catalogue (VCC; Binggeli et al., 1985), and the Index Catalogue (IC; Dreyer, 1908); (3) J2000 right ascension, from NED; (4) J2000 declination, from NED; (5) distance; (6) the morphological classification from NED; (7) total 2MASS K band magnitude −2 (Skrutskie et al., 2006); (8) the optical isophotal distance D25 (25 mag arcsec ); (9) the heliocentric radial velocity from NED; (10) the cluster or cloud membership; and (11) the galactic extinction Schlegel et al., 1998. ◦ ′ ′′ −1 HRS+ Alt.Name R.A.(hms) Dec.( ) D (Mpc) Type KStot D25 (′) V (km s ) Member AB (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) 1 CGCG 123-035 10 17 39.66 +22 48 35.9 15.7 Pec 11.59 1.00 1175 Leo Cl. 0.13 2 UGC 5588 10 20 57.13 +25 21 53.4 17.2 S? 11.03 0.52 1291 Leo Cl. 0.10 3 NGC 3226 10 23 27.01 +19 53 54.7 15.3 E2:pec;LINER;Sy3 8.57 3.16 1169 Leo Cl. 0.10 4 NGC 3227 10 23 30.58 +19 51 54.2 15.4 SAB(s)pec;Sy1.5 7.64 5.37 1148 Leo Cl. -
Identification of Old Tidal Dwarfs Near Early-Type Galaxies from Deep
Mon. Not. R. Astron. Soc. 000,1–11 (2013) Printed 29 October 2018 (MN LATEX style file v2.2) Identification of old tidal dwarfs near early-type galaxies from deep imaging and H I observations Pierre-Alain Duc,1? Sanjaya Paudel,1 Richard M. McDermid,2 Jean-Charles Cuillandre,3 Paolo Serra,4 Fred´ eric´ Bournaud,1 Michele Cappellari,5 Eric Emsellem6;7 1Laboratoire AIM Paris-Saclay, CEA/IRFU/SAp, CNRS/INSU, Universite´ Paris Diderot, 91191 Gif-sur-Yvette Cedex, France 2Gemini Observatory, Northern Operations Centre, 670 N. A‘ohoku Place, Hilo, HI 96720, USA 3Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy., Kamuela, Hawaii 96743 USA 4CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia 5Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH 6European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 7Centre de Recherche Astrophysique de Lyon, Universite´ Lyon 1, Observatoire de Lyon, Ecole Normale Superieure´ de Lyon, CNRS, UMR 5574, 9 avenue Charles Andre,´ F-69230 Saint-Genis Laval, France Accepted for publication in MNRAS ABSTRACT It has recently been proposed that the dwarf spheroidal galaxies located in the Local Group disks of satellites (DoSs) may be tidal dwarf galaxies (TDGs) born in a major merger at least 5 Gyr ago. Whether TDGs can live that long is still poorly constrained by observations. As part of deep optical and H I surveys with the CFHT MegaCam camera and Westerbork Syn- thesis Radio Telescope made within the ATLAS3D project, and follow-up spectroscopic ob- servations with the Gemini-North telescope, we have discovered old TDG candidates around several early-type galaxies. -
The Interstellar and Circumnuclear Medium of Active Nuclei Traced by H I 21 Cm Absorption
The Astronomy and Astrophysics Review (2018) 26:4 https://doi.org/10.1007/s00159-018-0109-x REVIEW ARTICLE The interstellar and circumnuclear medium of active nuclei traced by H i 21 cm absorption Raffaella Morganti1,2 · Tom Oosterloo1,2 Received: 23 April 2018 © The Author(s) 2018 Abstract This review summarises what we have learnt in the last two decades based on H i 21 cm absorption observations about the cold interstellar medium (ISM) in the central regions of active galaxies and about the interplay between this gas and the active nucleus (AGN). Hi absorption is a powerful tracer on all scales, from the parsec-scales close to the central black hole to structures of many tens of kpc tracing interactions and mergers of galaxies. Given the strong radio continuum emission often associated with the central activity, H i absorption observations can be used to study the Hi near an active nucleus out to much higher redshifts than is possible using H i emission. In this way, Hi absorption has been used to characterise in detail the general ISM in active galaxies, to trace the fuelling of radio-loud AGN, to study the feedback occurring between the energy released by the active nucleus and the ISM, and the impact of such interactions on the evolution of galaxies and of their AGN. In the last two decades, significant progress has been made in all these areas. It is now well established that many radio loud AGN are surrounded by small, regularly rotating gas disks that contain a significant fraction of H i. -
Classification of Galaxies Using Fractal Dimensions
UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. -
Abstract Handbook
July 8-11, 2008 Cambridge, Massachusetts at the Harvard Student Organization Center at Hilles Hosted by the Chandra X-Ray Center Chandra X-Ray Center Smithsonian Astrophysical Observatory Scientific Organizing Committee: SOC Chairs: Ralph Kraft and Aneta Siemiginowska (SAO) Elizabeth Blanton (BU) Geoff Bicknell (Stromlo) Annalisa Celotti (SISSA) Jean Eilek (NRAO/NMIMT) Dan Evans (Harvard) Heino Falcke (Radboud) Paul Green (SAO) Martin Hardcastle (Hertfordshire) Dan Harris (SAO) Sebastian Heinz (UWisc) Jun Kataoka (TokyoTech) Herman Marshall (MIT) Paul Nulsen (SAO) Chris Reynolds (UMd) Jeremy Sanders (IoA) Dan Schwartz (SAO) Marek Sikora (CAMK, Warsaw) Local Organizing Committee Paul Green (Chair) Lauren Deknis Ryan Foltz Michele Hall Michelle Henson Cathy Oskin Lisa Paton Su Tuttle This Chandra science workshop is sponsored by the Chandra Director’s Office (CDO) at the Chandra X-ray Center (CXC), part of the Smithsonian Astrophysical Observatory in Cambridge, MA. RADIO GALAXIES IN THE CHANDRA ERA July 8-11, 2008 PROGRAM TUESDAY JULY 8 9:00-9:15 Opening Remarks - Ralph Kraft and Harvey Tananbaum 9:15-9:50 Invited Talk: Dave De Young Radio Galaxies in X-ray Light: Problems and Processes SESSION I - RADIO GALAXIES IN THE LOCAL UNIVERSE CHAIR: DAN SCHWARTZ 9:50-10:25 Invited Talk: Mark Birkinshaw AGN Jet Flows 10:25-10:40 Talk I-1 : D. Harris Impulsive Brightening and Variability Timescales in the M87 Jet 10:40-11:10 Coffee 11:10-11:25 Talk I-2 : R. Daly The Properties of the Most Powerful FRII Radio Galaxies 11:25-11:40 Talk I-3 : C. Jones Centaurus A 11:40-11:55 Talk I-4 : R. -
MASSIVE Galaxies with Supermassive Black Holes
Hubble Space Telescope Cycle 23 GO Proposal 750 Homogeneous Distances and Central Profiles for MASSIVE Survey Galaxies with Supermassive Black Holes Scientific Category: UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE Scientific Keywords: Black Holes, Cosmological Parameters And Distance Scale, Galaxy Centers, Galaxy Morphology And Structure Instruments: WFC3 Proprietary Period: 12 Proposal Size: Small Orbit Request Prime Parallel Cycle 23 34 0 Abstract Massive early-type galaxies are the subject of intense interest: they exhibit the most massive black holes (BHs), most extreme stellar IMFs, and most dramatic size evolution over cosmic time. Yet, their complex formation histories remain obscure. Enter MASSIVE: a volume-limited survey of the structure and dynamics of the 100 most massive early-type galaxies within ~100 Mpc. We use integral-field spectroscopy (IFS) on sub-arcsecond (with AO) and large scales for simultaneous dynamical modeling of the supermassive BH, stars, and dark matter. The goals of MASSIVE include precise constraints on BH-galaxy scaling relations, the stellar IMF, and late-time assembly of ellipticals. We have already obtained much of the needed IFS and wide-field imaging for this project; here, we propose to add the one missing ingredient: high-resolution imaging with HST. This will nail down the central profiles, greatly reducing the degeneracy between M/L and BH masses in our dynamical orbit modeling. Further, we will measure efficient, high-quality WFC3/IR SBF distances for all targets, thereby removing potentially large errors from peculiar velocities (especially in the high-density regions occupied by massive early-types) or heterogeneous distance methods. Distance errors are insidious: they affect BH masses and galaxy properties in dissimilar ways, and thus can bias both the scatter and slopes of the scaling relations. -
Lord Rosse, Robinson, South and the Discovery of Spiral Structure in 1845
Journal of Astronomical History and Heritage, 15(1), 19-29 (2012). THE M51 MYSTERY: LORD ROSSE, ROBINSON, SOUTH AND THE DISCOVERY OF SPIRAL STRUCTURE IN 1845 Wolfgang Steinicke Gottenheimerstr. 18, D-79224, Umkirch, Germany. E-mail: [email protected] Abstract: In April 1845 Lord Rosse discovered the spiral structure of M51 with his 72-inch reflector at Birr Castle. Already in March the new telescope had been pointed at the object in Canes Venatici, later nicknamed the ‘Whirlpool Nebula’. Two experienced astronomers were present: Sir James South and the Reverend Thomas Romney Robin- son. The problem is that there is no record that they noticed the spiral structure, even though it was immediately seen by Lord Rosse the next month. The solution presented here is based on evidentiary facts, highlighting the nine- teenth century astronomical praxis. Focal points are bias, fantasy and a sometimes fatal conspiracy of eye and brain. Keywords: Spiral structure, nebulae, star clusters, Lord Rosse, Birr Castle, Leviathan of Parsonstown, Whirlpool Nebula, nebular hypothesis, visual observation, drawings. 1 DISCOVERY OF M51 AND JOHN the core, surrounded by a divided ring (Figure 2); it HERSCHEL’S ‘RING NEBULA’ appears as Figure 25 in the Slough catalogue. Herschel M51 (NGC 5194) is a nearby Sbc-galaxy with a visual magnitude 8.4 and a size of 11.2 × 6.9. It was dis- covered on 13 October 1773 by Charles Messier (1730–1817) with a 3.5-inch refractor at Paris. The description, published in his famous catalogue of 1781, reads: “… very faint nebula without stars …” 1 (Messier, 1781: 247). -
SAC's 110 Best of the NGC
SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
Arxiv:1801.08245V2 [Astro-Ph.GA] 14 Feb 2018
Draft version June 21, 2021 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE MASSIVE SURVEY IX: PHOTOMETRIC ANALYSIS OF 35 HIGH MASS EARLY-TYPE GALAXIES WITH HST WFC3/IR1 Charles F. Goullaud Department of Physics, University of California, Berkeley, CA, USA; [email protected] Joseph B. Jensen Utah Valley University, Orem, UT, USA John P. Blakeslee Herzberg Astrophysics, Victoria, BC, Canada Chung-Pei Ma Department of Astronomy, University of California, Berkeley, CA, USA Jenny E. Greene Princeton University, Princeton, NJ, USA Jens Thomas Max Planck-Institute for Extraterrestrial Physics, Garching, Germany. Draft version June 21, 2021 ABSTRACT We present near-infrared observations of 35 of the most massive early-type galaxies in the local universe. The observations were made using the infrared channel of the Hubble Space Telescope (HST ) Wide Field Camera 3 (WFC3) in the F110W (1.1 µm) filter. We measured surface brightness profiles and elliptical isophotal fit parameters from the nuclear regions out to a radius of ∼10 kpc in most cases. We find that 37% (13) of the galaxies in our sample have isophotal position angle rotations greater than 20◦ over the radial range imaged by WFC3/IR, which is often due to the presence of neighbors or multiple nuclei. Most galaxies in our sample are significantly rounder near the center than in the outer regions. This sample contains six fast rotators and 28 slow rotators. We find that all fast rotators are either disky or show no measurable deviation from purely elliptical isophotes. Among slow rotators, significantly disky and boxy galaxies occur with nearly equal frequency. -
Investigating Planet Formation and Composition Through Observations of Carbon and Oxygen Species in Stars, Disks, and Planets
Connecting the Dots: Investigating Planet Formation and Composition Through Observations of Carbon and Oxygen Species in Stars, Disks, and Planets Item Type text; Electronic Dissertation Authors Teske, Johanna Kavanagh Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 26/09/2021 06:42:44 Link to Item http://hdl.handle.net/10150/318831 CONNECTING THE DOTS: INVESTIGATING PLANET FORMATION AND COMPOSITION THROUGH OBSERVATIONS OF CARBON AND OXYGEN SPECIES IN STARS, DISKS, AND PLANETS by Johanna Kavanagh Teske A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2014 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the dis- sertation prepared by Johanna Kavanagh Teske entitled “Connecting the Dots: Investigating Planet Formation and Composition Through Observations of Car- boy and Oxygen Species in Disks, Stars, and Planets” and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Phi- losophy. Date: 11 April 2014 Caitlin Griffith Date: 11 April 2014 Katia Cunha Date: 11 April 2014 Simon Schuler Date: 11 April 2014 Daniel Apai Date: 11 April 2014 George Rieke Final approval and acceptance of this dissertation is contingent upon the candi- date’s submission of the final copies of the dissertation to the Graduate College.