A Catalog of Automatically Detected Ring Galaxy Candidates in Panstarrs
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Flat Rotation Curves and Low Velocity Dispersions in KMOS Star-Forming Galaxies at Z ∼ 1? E
A&A 594, A77 (2016) Astronomy DOI: 10.1051/0004-6361/201628315 & c ESO 2016 Astrophysics Flat rotation curves and low velocity dispersions in KMOS star-forming galaxies at z ∼ 1? E. M. Di Teodoro1; 2, F. Fraternali1; 3, and S. H. Miller4 1 Department of Physics and Astronomy, University of Bologna, 6/2 Viale Berti Pichat, 40127 Bologna, Italy 2 Research School of Astronomy and Astrophysics – The Australian National University, Canberra, ACT, 2611, Australia e-mail: [email protected] 3 Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, The Netherlands 4 University of California – Irvine, Irvine, CA 92697, USA Received 15 February 2016 / Accepted 18 July 2016 ABSTRACT The study of the evolution of star-forming galaxies requires the determination of accurate kinematics and scaling relations out to high redshift. In this paper we select a sample of 18 galaxies at z ∼ 1; observed in the Hα emission line with KMOS, to derive accurate kinematics using a novel 3D analysis technique. We use the new code 3DBarolo, which models the galaxy emission directly in 3D observational space, without the need to extract kinematic maps. This major advantage of this technique is that it is not affected by beam smearing and thus it enables the determination of rotation velocity and intrinsic velocity dispersion, even at low spatial resolution. We find that (1) the rotation curves of these z ∼ 1 galaxies rise very steeply within few kiloparsecs and remain flat out to the outermost radius and (2) the Hα velocity dispersions are low, ranging from 15 to 40 km s−1, which leads to V/σ = 3–10. -
Galactic-Scale Macro-Engineering: Looking for Signs of Other Intelligent Species, As an Exercise in Hope for Our Own
Galactic-scale macro-engineering: Looking for signs of other intelligent species, as an exercise in hope for our own * Joseph Voros Senior Lecturer in Strategic Foresight Faculty of Business & Law, Swinburne University of Technology, Melbourne, Australia Abstract If we consider Big History as simply ‘our’ example of the process of cosmic evolution playing out, then we can seek to broaden our view of our possible fate as a species by asking questions about what paths or trajectories other species’ own versions of Big History might take or have taken. This paper explores the broad outlines of possible scenarios for the evolution of long-lived intelligent engineering species—scenarios which might have been part of another species’ own Big History story, or which may yet lie ahead in our own distant future. A sufficiently long-lived engineering-oriented species may decide to undertake a program of macro-engineering projects that might eventually lead to a re-engineered galaxy so altered that its artificiality may be detectable from Earth. We consider activities that lead ultimately to a galactic structure consisting of a central inner core surrounded by a more distant ring of stars separated by a relatively sparser ‘gap’, where star systems and stellar materials may have been removed, ‘lifted’ or turned into Dyson Spheres. When one looks to the sky, one finds that such galaxies do indeed exist—including the beautiful ringed galaxy known as ‘Hoag’s Object’ (PGC 54559) in the constellation Serpens. This leads us to pose the question: Is Hoag’s Object an example of galaxy-scale macro-engineering? And this suggests a program of possible observational activities and theoretical explorations, several of which are presented here, that could be carried out in order to begin to investigate this beguiling question. -
Broad-Band Photometry and Long-Slit Spectroscopy of the Peculiar Ring Galaxy FM 287-14
A&A 559, A8 (2013) Astronomy DOI: 10.1051/0004-6361/201219721 & c ESO 2013 Astrophysics Broad-band photometry and long-slit spectroscopy of the peculiar ring galaxy FM 287-14 M. Faúndez-Abans1, P. C. da Rocha-Poppe2,3, V. A. Fernandes-Martin2,3, M. de Oliveira-Abans1,5, I. F. Fernandes2,3,E.Wenderoth4, and A. Rodríguez-Ardila1 1 MCTI/Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, CEP 37504-364 Itajubá, MG, Brazil e-mail: [max;mabans;aardila]@lna.br 2 UEFS, Departamento de Física, Av. Transnordenstina, S/N, Novo Horizonte, CEP 44036-900 Feira de Santana, BA, Brazil 3 UEFS, Observatório Astronômico Antares, Rua da Barra, 925, Jardim Cruzeiro, CEP 44015-430 Feira de Santana, BA, Brazil e-mail: [paulopoppe;vmartin][email protected]; [email protected] 4 Gemini Observatory, Southern Operations Center, c/o AURA, 603 Casilla, La Serena, Chile e-mail: [email protected] 5 UNIFEI, Instituto de Engenharia de Produção e Gestão, Av. BPS, 1303, Pinheirinho, CEP 37500-903 Itajubá, MG, Brazil Received 30 May 2013 / Accepted 21 August 2013 ABSTRACT Aims. We report detailed morphological and kinematical insights into the disturbed galaxy FM 287-14, which is reported in the literature as a member of strongly interacting galaxies with a clear case of mergers. The main purpose of this paper is to provide a first observational study of this double-nuclei object based on photometry and spectroscopy. Methods. The study is based on BVR photometry with the 1.6-m telescope at OPD, and long-slit spectroscopy with Gemini South’s GMOS spectrograph, with two-gratings centered at 5 011 Å and 6 765 Å. -
Astronomy 2008 Index
Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs. -
Star Formation in Ring Galaxies Susan C
East Tennessee State University Digital Commons @ East Tennessee State University Undergraduate Honors Theses Student Works 5-2016 Star Formation in Ring Galaxies Susan C. Olmsted East Tennessee State Universtiy Follow this and additional works at: https://dc.etsu.edu/honors Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation Olmsted, Susan C., "Star Formation in Ring Galaxies" (2016). Undergraduate Honors Theses. Paper 322. https://dc.etsu.edu/honors/ 322 This Honors Thesis - Open Access is brought to you for free and open access by the Student Works at Digital Commons @ East Tennessee State University. It has been accepted for inclusion in Undergraduate Honors Theses by an authorized administrator of Digital Commons @ East Tennessee State University. For more information, please contact [email protected]. Star Formation in Ring Galaxies Susan Olmsted Honors Thesis May 5, 2016 Student: Susan Olmsted: ______________________________________ Mentor: Dr. Beverly Smith: ____________________________________ Reader 1: Dr. Mark Giroux: ____________________________________ Reader 2: Dr. Michele Joyner: __________________________________ 1 Abstract: Ring galaxies are specific types of interacting galaxies in which a smaller galaxy has passed through the center of the disk of another larger galaxy. The intrusion of the smaller galaxy causes the structure of the larger galaxy to compress as the smaller galaxy falls through, and to recoil back after the smaller galaxy passes through, hence the ring-like shape. In our research, we studied the star-forming regions of a sample of ring galaxies and compared to those of other interacting galaxies and normal galaxies. Using UV, optical, and IR archived images in twelve wavelengths from three telescopes, we analyzed samples of star-forming regions in ring and normal spiral galaxies using photometry. -
A “Smashing” Polar-Ring Galaxy
A “Smashing” Polar-ring Galaxy Image Credit: Gemini Observatory/AURA Gemini Observatory Legacy Image Gemini Observatory Facts The Gemini Observatory is operated A “Smashing” Polar-ring Galaxy by the Association of Universities for PRIMARY MIRRORS: Research in Astronomy, Inc., under a cooperative agreement with the This Gemini North telescope image captures the “bloody” Diameter: 8.1 meters; 26.57 feet; 318.84 inches National Science Foundation on behalf of the Gemini Partnership. aftermath of one galaxy piercing the heart of another. All Mass: 22.22 metric tonnes; 24.5 U.S. tons the action appears in a single frame, with the stunning Composition: Corning Ultra-Low Expansion (ULE) Glass Surface Accuracy: 15.6 nm RMS (between 1/1000 - 1/10,000 polar-ring galaxy NGC 660 as the focus of attention. thickness of human hair) NGC 660 spans some 40,000 light years across and lies TELESCOPE STRUCTURES: United States about 40 million light years distant in the direction of Height: 21.7 meters; 71.2 feet; 7 stories (from “Observing Floor”) the constellation of Pisces. It has an unusually high Weight: 380 metric tonnes; 419 U.S. tons gas content and resolves into hundreds of objects, a Optomechanical Design: Cassegrain ; Alt-azimuth Canada considerable fraction of which are blue and red supergiant DOMES: stars. The ring’s youngest detected stars formed only Height: 46 meters; 151 feet; 15 stories (from ground) about seven million years ago, indicating a long and Weight: 780 metric tonnes; 860 U.S. tons (moving mass) Rotation: 360 degrees in 2 minutes ongoing process of formation. -
Bibliography of Refereed Papers: Roger L
Bibliography of refereed papers: Roger L. Davies 203 refereed papers, >24,000 citations, h=75 62 papers >100 citations; 13 papers >500 citations and one has more than 1000 citations. [203] Francesco D'Eugenio, Matthew Colless, Nicholas Scott, Arjen van der Wel, Roger L. Davies, Jesse van de Sande, Sarah M. Sweet, Sree Oh, Brent Groves, Rob Sharp, Matt S. Owers, Joss Bland-Hawthorn, Scott M. Croom, Sarah Brough, Julia J. Bryant, Michael Goodwin, Jon S. Lawrence, Nuria P. F. Lorente, and Samuel N. Richards. The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane. MNRAS, April 2021. [202] Scott M. Croom, Matt S. Owers, Nicholas Scott, Henry Poetrodjojo, Brent Groves, Jesse van de Sande, Tania M. Barone, Luca Cortese, Francesco D'Eugenio, Joss Bland-Hawthorn, Julia Bryant, Sree Oh, Sarah Brough, James Agostino, Sarah Casura, Barbara Catinella, Matthew Colless, Gerald Cecil, Roger L. Davies, Michael J. Drinkwater, Simon P. Driver, Ignacio Ferreras, Caroline Foster, Amelia Fraser-McKelvie, Jon Lawrence, Sarah K. Leslie, Jochen Liske, Angel´ R. L´opez-S´anchez, Nuria P. F. Lorente, Rebecca McElroy, Anne M. Medling, Danail Obreschkow, Samuel N. Richards, Rob Sharp, Sarah M. Sweet, Dan S. Taranu, Edward N. Taylor, Edoardo Tescari, Adam D. Thomas, James Tocknell, and Sam P. Vaughan. The SAMI Galaxy Survey: the third and final data release. MNRAS, February 2021. [201] Romina Ahumada and others. The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra. ApJS, 249(1):3, July 2020. [200] S. -
Cetus - the Whale
May 18 2021 Cetus - The Whale Observed: No Object Her Type Mag Alias/Notes IC 5384 Non-Existent NGC 7813 MCG -2-1-16 MK 936 IRAS 15-1215 PGC 287 IC 1528 Non-Existent NGC 7826 H29-8 Non-Existent Asterism IC 1533 Non-Existent NGC 34 Non-Existent NGC 17 NGC 58 Non-Existent NGC 47 PGC 967 MCG -1-1-55 IRAS 119-726 NGC 54 Glxy SB(r)a? 14.6 MCG -1-1-60 PGC 1011 NGC 59 Glxy SA(rs)0-: 13.1 ESO 539-4 MCG -4-1-26 PGC 1034 NGC 62 Glxy (R)SB(r)a: 12.3 MCG -2-1-43 IRAS 145-1345 PGC 1125 NGC 64 Glxy SB(s)bc 14 MCG -1-1-68 IRAS 149-706 PGC 1149 IC 5 Glxy E 14.8 MCG -2-1-47 IRAS 148-951 PGC 1145 NGC 73 Glxy SAB(rs)bc: 13.5 MCG -3-1-26 PGC 1211 NGC 65 Glxy SAB(rs)0-: 14.4 ESO 473-10A MCG -4-2-1 PGC 1229 NGC 66 Glxy SB(r)b pec 14.2 ESO 473-10 MCG -4-2-2 IRAS 165-2312 PGC 1236 IC 9 Glxy Sb(r) 16.1 MCG -2-2-1 IRAS 171-1423 PGC 1271 NGC 77 Glxy SA0-: 15.7 ESO 473-15 PGC 1290 NGC 102 Glxy S0/a 14.4 MCG -2-2-11 PGC 1542 NGC 107 Glxy Sbc 14.6 MCG -2-2-14 PGC 1606 NGC 111 Non-Existent NGC 113 Glxy SA0-: 13.5 MCG -1-2-16 PGC 1656 NGC 114 Glxy SB(rs)0: 14.7 UGC 259 MCG 0-2-27 MK 946 CGCG 383-14 KUG 24-20A PGC 1660 NGC 116 Non-Existent MCG -1-2-17 PGC 1671 NGC 117 Glxy S0+: sp 15.3 MCG 0-2-29 CGCG 383-15 PGC 1674 NGC 118 Glxy I0? 14.8 UGC 264 MCG 0-2-32 MK 947 CGCG 383-16 UM244 3ZW9 IRAS 247-203 PGC 1678 NGC 120 Glxy SB0^: 14.4 UGC 267 MCG 0-2-33 CGCG 383-17 PGC 1693 NGC 122 Non-Existent NGC 123 Non-Existent NGC 124 Glxy SA(s)c 13.7 UGC 271 MCG 0-2-38 CGCG 383-18 IRAS 253-205 PGC 1715 IC 15 Non-Existent IC 16 Glxy E? 14.7 MCG -2-2-17 IRAS 255-1322 PGC 1730 IC 17 -
The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-To-Light Ratio
The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio Gene G. Byrd – University of Alabama Tarsh Freeman – Bevill State Community College Ronald J. Buta – University of Alabama Deposited 06/13/2018 Citation of published version: Byrd, G., Freeman, T., Buta, R. (2006): The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio. The Astronomical Journal, 131(3). DOI: 10.1086/499944 © 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. The Astronomical Journal, 131:1377–1393, 2006 March # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE INNER RESONANCE RING OF NGC 3081. II. STAR FORMATION, BAR STRENGTH, DISK SURFACE MASS DENSITY, AND MASS-TO-LIGHT RATIO Gene G. Byrd,1 Tarsh Freeman,2 and Ronald J. Buta1 Received 2005 July 19; accepted 2005 November 19 ABSTRACT We complement our Hubble Space Telescope (HST ) observations of the inner ring of the galaxy NGC 3081 using an analytical approach and n-body simulations. We find that a gas cloud inner (r) ring forms under a rotating bar perturbation with very strong azimuthal cloud crowding where the ring crosses the bar major axis. Thus, star forma- tion results near to and ‘‘downstream’’ of the major axis. From the dust distribution and radial velocities, the disk rotates counterclockwise (CCW) on the sky like the bar pattern speed. We explain the observed CCW color asym- metry crossing the major axis as due to the increasing age of stellar associations inside the r ring major axis. -
The X-Ray Luminosity Function of Ultra Luminous X-Ray Sources in Collisional Ring Galaxies
Draft version June 8, 2018 Typeset using LATEX twocolumn style in AASTeX62 The X-Ray Luminosity Function of Ultra Luminous X-Ray Sources in Collisional Ring Galaxies Anna Wolter,1 Antonella Fruscione,2 and Michela Mapelli3 1INAF-Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy 2Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambdidge, MA, 02138 3INAF-Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122, Padova, Italy (Received March, 7th, 2018; Accepted June, 5th, 2018) Submitted to The Astrophysical Journal ABSTRACT Ring galaxies are fascinating laboratories: a catastrophic impact between two galaxies (one not much smaller than the other) has produced fireworks especially in the larger one, when hit roughly perpendicularly to the plane. We analyze the point sources, produced by the starburst episode following the impact, in the rings of seven galaxies and determine their X-ray luminosity function (XLF). In 39 −1 total we detect 63 sources, of which 50 have luminosity LX ≥ 10 erg s , classifying them as ultra luminous X-ray sources (ULXs). We find that the total XLF is not significantly different from XLFs derived for other kinds of galaxies, with a tendency of having a larger fraction of high X-ray luminosity objects. Both the total number of ULXs and the number of ULXs per unit star formation rate are found in the upper envelope of the more normal galaxies distribution. Further analysis would be needed to address the issue of the nature of the compact component in the binary system. Keywords: galaxies: individual (AM0644-741, Arp143, Arp148) - galaxies: peculiar - galaxies: star formation - X-ray binaries 1. -
The Green Valley: How to Rejuvenate an S0 Galaxy Through Minor Mergers
Galaxies 2015, 3, 192-201; doi:10.3390/galaxies3040192 OPEN ACCESS galaxies ISSN 2075-4434 www.mdpi.com/journal/galaxies Article Back to the Green Valley: How to Rejuvenate an S0 Galaxy through Minor Mergers Michela Mapelli INAF—Astronomical Observatory of Padova, Vicolo dell’Osservatorio 5, Padova 35122, Italy; E-Mail: [email protected] Academic Editors: Alexei Moiseev, José Alfonso López Aguerri and Enrichetta Iodice Received: 14 October 2015 / Accepted: 10 November 2015 / Published: 13 November 2015 Abstract: About half of the S0 galaxies in the nearby Universe show signatures of recent or ongoing star formation. Whether these S0 galaxies were rejuvenated by the accretion of fresh gas is still controversial. We study minor mergers of a gas-rich dwarf galaxy with an S0 galaxy, by means of N-body smoothed-particle hydrodynamics simulations. We find that minor mergers trigger episodes of star formation in the S0 galaxy, lasting for ∼10 Gyr. One of the most important fingerprints of the merger is the formation of a gas ring in the S0 galaxy. The ring is reminiscent of the orbit of the satellite galaxy, and its lifetime depends on the merger properties: polar and counter-rotating satellite galaxies induce the formation of long-lived smooth gas rings. Keywords: galaxies: interactions; methods: numerical; galaxies: kinematics and dynamics; galaxies: ISM; galaxies: star formation 1. Introduction S0 galaxies are intriguing objects: they are early-type galaxies (ETGs), but are characterized by a stellar disc (although with no spiral arms). About half of S0 galaxies [1] lie in the region of the colour-magnitude diagram (CMD) of galaxies that is called green valley. -
VLT-VIMOS Integral Field Spectroscopy of Luminous and Ultraluminous
A&A 479, 687–702 (2008) Astronomy DOI: 10.1051/0004-6361:20078451 & c ESO 2008 Astrophysics VLT-VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies I. The sample and first results S. Arribas1,L.Colina1, A. Monreal-Ibero2 , J. Alfonso1, M. García-Marín1, and A. Alonso-Herrero1 1 Departamento de Astrofísica Molecular e Infrarroja (DAMIR), Instituto de Estructura de la Materia (IEM/CSIC), C/ Serrano 121, 28006 Madrid, Spain e-mail: [arribas;colina;julia;maca;aalonso]@damir.iem.csic.es 2 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: [email protected] Received 9 August 2007 / Accepted 19 October 2007 ABSTRACT Context. (Ultra)Luminous Infrared Galaxies [(U)LIRGs] are much more numerous at cosmological distances than locally, and are likely the precursors of elliptical galaxies. Studies of the physical structure and kinematics of representative samples of these galaxies at low redshift are needed in order to understand the interrelated physical processes involved. Integral field spectroscopy (IFS) offers the possibility of performing such a detailed analysis. Aims. Our goal is to carry out IFS of 42 southern systems which are part of a representative sample of about 70 low redshift (z ≤ 0.26) 11 12.6 (U)LIRGs, covering different morphologies from spirals to mergers over the entire infrared luminosity range (LIR = 10 −10 L). Methods. The present study is based on optical IFS obtained with the VIMOS instrument on the VLT. Results. The first results of the survey are presented here with the study of two galaxies representative of the two major morphological types observed in (U)LIRGs, interacting pairs and morphologically- regular, weakly-interacting spirals, respectively.