Progenitor Mass Constraints for Core-Collapse Supernovae
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John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C
VITA NAME: John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C. EDUCATION: 1970 B.A. George Washington University, Washington, D.C. 1972 M.S. Case Institute of Technology, Cleveland, OH 1976 Ph.D. University of Maryland, College Park, MD PROFESSIONAL EXPERIENCE: 2002–present David Ross Boyd Professor, University of Oklahoma, 2002–2002 Research Fellow, University of Texas, Austin, TX 1998–2002 Samuel Roberts Noble Foundation Presidential Professor, University of Oklahoma, Norman, OK 1997–1998 Big XIIFaculty Fellow,University ofOklahoma 1991–1992 Visiting Professor, Department of Astronomy, Columbia University, New York, NY 1989–present Professor, Department of Physics and Astronomy, University of Oklahoma, Norman, OK 1988–1994 Consultant and Participating Guest, Lawrence Livermore National Laboratory, Livermore, CA 1987–1988 Visiting Research Associate, Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 1984–1989 Associate Professor, University of Oklahoma 1979–1984 Assistant Professor, University of Oklahoma 1976–1979 Postdoctoral Research Fellow, Harvard-Smithsonian Center for Astrophysics, Harvard University PROFESSIONAL AND HONORARY SOCIETIES: American Astronomical Society International Astronomical Union Phi Beta Kappa RESEARCH INTERESTS: Stellar evolution, supernovae, nucleosynthesis and abundances Radio observations of supernovae and galaxies JOHN J. COWAN Page 2 PUBLICATIONS J. J. Cowan and W. K. Rose, “Production of 17O and 18O by Means of the Hot CNO Tri-Cycle,” Astrophys. J. (Letters) 201, L45 (1975) J. J. Cowan, M. Kafatos, and W. K. Rose, “Sources of Excitation of the Interstellar Gas and Galactic Structure,” Astrophys. J. 195, 47 (1975) M. F. A’Hearn and J. J. Cowan, “Molecular Production Rates in Comet Kohoutek,” As- tron. -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”. -
The Very Young Resolved Stellar Populations Around Stripped-Envelope Supernovae
MNRAS 000,1– ?? (2016) Preprint 22 December 2017 Compiled using MNRAS LATEX style file v3.0 The very young resolved stellar populations around stripped-envelope supernovae Justyn R. Maund?y Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, U.K. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The massive star origins for Type IIP supernovae (SNe) have been established through direct detection of their red supergiants progenitors in pre-explosion observations; however, there has been limited success in the detection of the progenitors of H-deficient SNe. The final fate of more massive stars, capable of undergoing a Wolf-Rayet phase, and the origins of Type Ibc SNe remains debated, including the relative importance of single massive star progeni- tors or lower mass stars stripped in binaries. We present an analysis of the ages and spatial distributions of massive stars around the sites of 23 stripped-envelope SNe, as observed with the Hubble Space Telescope, to probe the possible origins of the progenitors of these events. Using a Bayesian stellar populations analysis scheme, we find characteristic ages for the pop- ulations observed within 150 pc of the target Type IIb, Ib and Ic SNe to be log¹tº = 7:20, 7:05 and 6:57, respectively. The Type Ic SNe in the sample are nearly all observed within 100 pc of young, dense stellar populations. The environment around SN 2002ap is an important ex- ception both in terms of age and spatial properties. These findings may support the hypothesis that stars with Minit > 30M produce a relatively large proportion of Type Ibc SNe, and that these SN subtypes arise from progressively more massive progenitors. -
Gone Without a Bang: an Archival HST Survey for Disappearing Massive Stars
MNRAS 453, 2885–2900 (2015) doi:10.1093/mnras/stv1809 Gone without a bang: an archival HST survey for disappearing massive stars Thomas M. Reynolds,1,2‹ Morgan Fraser1 and Gerard Gilmore1 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vais¨ al¨ antie¨ 20, FI-21500 Piikkio,¨ Finland Downloaded from Accepted 2015 August 4. Received 2015 July 16; in original form 2015 May 27 ABSTRACT It has been argued that a substantial fraction of massive stars may end their lives without http://mnras.oxfordjournals.org/ an optically bright supernova (SN), but rather collapse to form a black hole. Such an event would not be detected by current SN surveys, which are focused on finding bright transients. Kochanek et al. proposed a novel survey for such events, using repeated observations of nearby galaxies to search for the disappearance of a massive star. We present such a survey, using the first systematic analysis of archival Hubble Space Telescope images of nearby galaxies with the aim of identifying evolved massive stars which have disappeared, without an accompanying optically bright SN. We consider a sample of 15 galaxies, with at least three epochs of Hubble Space Telescope imaging taken between 1994 and 2013. Within this data, we find one candidate at CERN - European Organization for Nuclear Research on September 15, 2016 which is consistent with a 25–30 M yellow supergiant which has undergone an optically dark core-collapse. Key words: stars: evolution – stars: massive – supernovae: general. plosion, and Type IIL (Linear) SNe which have a steady decline 1 INTRODUCTION in luminosity from peak. -
9905625.PDF (3.665Mb)
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 free, while others may be from any type o f 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 afreet reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are m is^ g pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., m ^ s, drawings, charts) are reproduced by sectioning the orignal, begnning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. KGgher quality 6” x 9” black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. UMI A Bell & Howell Infoimation Compaiy 300 North Zeeb Road, Ann Arbor MI 48106-1346 USA 313/761-4700 800/521-0600 UNIVERSITY OF OKLAHOMA GRADUATE COLLEGE “ ‘TIS SOMETHING, NOTHING”, A SEARCH FOR RADIO SUPERNOVAE A DISSERTATION SUBMITTED TO THE GRADUATE FACULTY in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY By CHRISTOPHER R. -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
Fundamental Properties of Core-Collapse Supernova and GRB Progenitors: Predicting the Look of Massive Stars Before Death
A&A 558, A131 (2013) Astronomy DOI: 10.1051/0004-6361/201321906 & c ESO 2013 Astrophysics Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death Jose H. Groh1, Georges Meynet1, Cyril Georgy2, and Sylvia Ekström1 1 Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics group, EPSAM, Keele University, Lennard-Jones Labs, ST5 5BG Keele, UK Received 16 May 2013 / Accepted 20 August 2013 ABSTRACT We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini = 9−20 M, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the + following types of SN progenitors: WO1–3 (Mini ≥ 32 M), WN10–11 (25 < Mini < 32 M), LBV (20 ≤ Mini ≤ 25 M), G1 Ia (18 < Mini < 20 M), and RSGs (9 ≤ Mini ≤ 18 M). For non-rotating models, we found spectral types WO1–3 (Mini > 40 M), WN7–8 (25 < Mini ≤ 40 M), WN11h/LBV (20 < Mini ≤ 25 M), and RSGs (9 ≤ Mini ≤ 20 M). -
Monthly Newsletter of the Durban Centre - March 2018
Page 1 Monthly Newsletter of the Durban Centre - March 2018 Page 2 Table of Contents Chairman’s Chatter …...…………………….……….………..….…… 3 Andrew Gray …………………………………………...………………. 5 The Hyades Star Cluster …...………………………….…….……….. 6 At the Eye Piece …………………………………………….….…….... 9 The Cover Image - Antennae Nebula …….……………………….. 11 Galaxy - Part 2 ….………………………………..………………….... 13 Self-Taught Astronomer …………………………………..………… 21 The Month Ahead …..…………………...….…….……………..…… 24 Minutes of the Previous Meeting …………………………….……. 25 Public Viewing Roster …………………………….……….…..……. 26 Pre-loved Telescope Equipment …………………………...……… 28 ASSA Symposium 2018 ………………………...……….…......…… 29 Member Submissions Disclaimer: The views expressed in ‘nDaba are solely those of the writer and are not necessarily the views of the Durban Centre, nor the Editor. All images and content is the work of the respective copyright owner Page 3 Chairman’s Chatter By Mike Hadlow Dear Members, The third month of the year is upon us and already the viewing conditions have been more favourable over the last few nights. Let’s hope it continues and we have clear skies and good viewing for the next five or six months. Our February meeting was well attended, with our main speaker being Dr Matt Hilton from the Astrophysics and Cosmology Research Unit at UKZN who gave us an excellent presentation on gravity waves. We really have to be thankful to Dr Hilton from ACRU UKZN for giving us his time to give us presentations and hope that we can maintain our relationship with ACRU and that we can draw other speakers from his colleagues and other research students! Thanks must also go to Debbie Abel and Piet Strauss for their monthly presentations on NASA and the sky for the following month, respectively. -
Arxiv:Astro-Ph/9902377V1 26 Feb 1999 Sus Uha H Omcxrybcgon.Ide,Tedis the Indeed, Background
The distribution of absorbing column densities among Seyfert 2 galaxies G. Risaliti Dipartimento di Astronomia e Scienza dello Spazio, Univerit`adi Firenze, L. E. Fermi 5, I-50125, Firenze, Italy R. Maiolino and M. Salvati Osservatorio Astrofisico di Arcetri, L. E. Fermi 5, I-50125 Firenze, Italy ABSTRACT We use hard X-ray data for an “optimal” sample of Seyfert 2 galaxies to derive the distribution of the gaseous absorbing column densities among obscured active nuclei in the local Universe. Of all Seyfert 2 galaxies in the sample, 75% are heavily obscured 23 −2 24 −2 (NH > 10 cm ) and about half are Compton thick (NH > 10 cm ). Intermediate type 1.8–1.9 Seyferts are characterized by an average NH much lower than “strict” Seyfert 2s. No correlation is found between NH and the intrinsic luminosity of the nuclear source. This NH distribution has important consequences for the synthesis of the cosmic X-ray background. Also, the large fraction of Compton thick objects implies that most of the obscuring gas is located within a radius of a few 10 pc from the nucleus. Subject headings: Galaxies: active — Galaxies: nuclei — Galaxies: Seyfert — X-rays: galaxies arXiv:astro-ph/9902377v1 26 Feb 1999 1. Introduction According to the so-called unified model (Antonucci 1993) the same engine is at work in all Active Galactic Nuclei (AGNs). The differences between type 1 and type 2 AGNs are ascribed solely to orientation effects: our line of sight to the nucleus may (type 2) or may not (type 1) be obstructed by optically thick material, perhaps distributed in a toroidal geometry. -
Exploding Star in NGC 2397 31 March 2008
Exploding star in NGC 2397 31 March 2008 Camera for Surveys (ACS). One atypical feature of this Hubble image is the view of supernova SN 2006bc taken when it was still fairly faint and its brightness on the increase. Astronomers from Queen's University Belfast in Northern Ireland, led by Professor of Astronomy Stephen J. Smartt, requested the image as part of a long project studying the massive exploding stars — supernovae. Exactly which types of star will explode and the lowest mass of star that can produce a supernova are not known. When a supernova is discovered in a nearby galaxy the group begins a painstaking search of earlier Hubble images of the same galaxy to locate the NGC 2397, pictured in this image from Hubble, is a star that later exploded; often one of hundreds of classic spiral galaxy with long prominent dust lanes millions of stars in the galaxy. This is a little like along the edges of its arms, seen as dark patches and sifting through days of CCTV footage to find one streaks silhouetted against the starlight. Hubble's frame showing a suspect. If the astronomers find a exquisite resolution allows the study of individual stars in star at the location of the later explosion, they may nearby galaxies. Located nearly 60 million light-years work out the mass and type of star from its away from Earth, the galaxy NGC 2397 is typical of most spirals, with mostly older, yellow and red stars in its brightness and colour. Only six such stars have central portion, while star formation continues in the been identified before they exploded and the outer, bluer spiral arms. -
Curriculum Vitae
Christopher J. Stockdale Assistant Professor, Department of Physics Marquette University EDUCATION: 2001 Ph.D. in Physics University of Oklahoma, Norman, OK Dissertation Title: A Radio and X-ray Search for Intermediate-age Supernovae: Tuning Into the Oldies, Advisor John J. Cowan, Ph.D. 1995 M.S. in Physics University of Oklahoma, Norman, OK 1992 B.S. in Physics Washington University, St. Louis, MO PROFESSIONAL EXPERIENCE: 2003–present Assistant Professor, Marquette University, Milwaukee, WI 2001–2003 Postdoctoral Fellow, Naval Research Laboratory, Washington, DC 1998–2001 Adjunct Professor, Oklahoma City Community College, Oklahoma City AWARDS: 2001 National Research Council Postdoctoral Fellowship 2001 Nielsen Prize for Outstanding Dissertation – Homer L. Dodge Department of Physics, University of Oklahoma PROFESSIONAL SOCIETIES: American Astronomical Society 1996-present Sigma Pi Sigma, The National Physics Honor Society 2004-present Sigma Xi, The Scientific Research Society 2005-present SERVICE TO SCIENCE COMMUNITY: GALEX Science Proposal Review Congressional Visits Day with American Astronomical Society – May 2007 Swift Science Proposal Review NSF Reviewer for Course, Curriculum, and Laboratory Improvement Grants Chandra Science Proposal Review Co-host for the 16th Annual meeting of the NASA Wisconsin Space Grant Consortium SERVICE TO MARQUETTE COMMUNITY: Member – Provost’s Task Force on E-Learning – November 2006 – June 2007 Member – Academic and Technology Advisory Committee – August 2005 - present Member – “Bringing Science at Marquette from Good to Great” and Designing A New Science Building Task Force – summer 2005, 2006 New Course Designed, PHYS 121/122 – Introduction to Theoretical and Observational Astrophysics New Course Designed, PHYS 13/14 – Classical Physics 1: Mechanics and Waves and Classical Physics 2: Heat, Electromagnetism, and Optics Stockdale p. -
Characterizing the V-Band Light-Curves of Hydrogen-Rich Type Ii Supernovae∗
The Astrophysical Journal, 786:67 (35pp), 2014 May 1 doi:10.1088/0004-637X/786/1/67 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE∗ Joseph P. Anderson1,2, Santiago Gonzalez-Gait´ an´ 1, Mario Hamuy1,3, Claudia P. Gutierrez´ 1,3, Maximilian D. Stritzinger4, Felipe Olivares E.5, Mark M. Phillips6, Steve Schulze7, Roberto Antezana1, Luis Bolt8, Abdo Campillay6, Sergio Castellon´ 6, Carlos Contreras4, Thomas de Jaeger1,3,Gaston´ Folatelli9, Francisco Forster¨ 1, Wendy L. Freedman10, Luis Gonzalez´ 1, Eric Hsiao6, Wojtek Krzeminski´ 11, Kevin Krisciunas12, Jose´ Maza1, Patrick McCarthy10, Nidia I. Morrell6, Sven E. Persson10, Miguel Roth6, Francisco Salgado13, Nicholas B. Suntzeff12, and Joanna Thomas-Osip6 1 Departamento de Astronom´ıa, Universidad de Chile, Casilla 36-D, Santiago, Chile; [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 3 Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile 4 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 5 Departamento de Ciencias Fisicas, Universidad Andres Bello, Avda. Republica 252, Santiago, Chile 6 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 7 Instituto de Astrof´ısica, Facultad de F´ısica, Pontif´ıcia Universidad Catolica´ de Chile, Casilla 306, Santiago 22, Chile 8 Argelander Institut fur¨ Astronomie, Universitat¨ Bonn, Auf dem Hugel¨ 71, D-53111 Bonn, Germany 9 Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan 10 Observatories of the Carnegie Institution for Science, Pasadena, CA 91101, USA 11 N.