DOCSLIB.ORG

Gamma-Ray Burst Host Galaxies at High Resolution

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Gamma-Ray Burst Host Galaxies at High Resolution GAMMA-RAY BURST HOST GALAXIES AT HIGH RESOLUTION CHRISTINA CARINA THÖNE Dissertation Submitted for the Degree PHILOSOPHIÆ DOCTOR Dark Cosmology Centre Niels Bohr Institut Det Naturvidenskabelige Fakultet Københavns Universitet Submission: July 4th, 2008 Defence: October 3rd, 2008 Supervisor: Assoc. Prof. Johan P. U. Fynbo Opponents: Prof. Max Pettini Dr. Chryssa Kouveliotou Cover art: Going observing brings you not only scientific images, sometimes, there is also time to do pretty pictures, either with the telescope itself or with your own camera. This cover joins both. The panorama at the bottom was taken in a very cold full moon night in August 2008 on La Silla after a thunderstorm and fresh snow in the Cordillera Central. The pictures were taken in raw format and dark- and bias-subtracted before joining them to a panorama. Thanks to Antonio for making this nice panorama from the raw files taken with my small, but apparently not so crappy Olympus. The telescope at the right side of the back cover shows UT1 of the VLT telescopes, taken a few days before under nearly full moon, this time with Antonios camera and a tripod. The dome to the left belongs to one of the two Keck telescopes on Mauna Kea. The main image of the cover is a mosaic of the nebula around η Carinae, a massive luminous blue variable but likely never becoming a GRB, created by its violent outbursts and mass losses over the last 100 years with the star itself hiding behind the dark dust clouds. The mosaic consists of 8 panels taken in V, R and I filters with the Danish 1.54m telescope in February 2006. Thanks to Robert Gendler for processing and merging the images. The little "cosmic explosion" in the upper left of the back cover is a picture of our own sun taken during the solar eclipse 2006 which I watched from a hotel near Antalya/Turkey during a GRB workshop. It marks the end of the eclipse when the sun is shining through the valleys at the edge of the moon creating the diamond ring effect. It is also a symbol for the background picture I had on my mobile phone used for GRB triggering over the last years which showed a picture of the moon with some artistic rays around but which I could not get in high resolution. The cover was put together in Photoshop, thanks to Ana Lucía for helping with various problems in Photoshop. The titlepage of Part I of the thesis is a color composite of the starburst galaxy M82 taken with ALFOSC at the NOT in B, V and Hα filters and symbolizes the absorption lines likely caused by starburst winds from GRB hosts that we detected in the spectra of GRB 030329 and GRB 060206. Thanks to Johan for making the color image. The title of Part II shows a part of the η Carinae mosaic and a color composite of a galaxy whose name I forgot. It was taken at the Brorfelde observatory west of Copenhagen when Chloé and I were training for going observing the first time back in October 2005. The two pictures are a symbol for the resolved host galaxies of GRB 060505 and SN 2008D and for the fact that we were interested in the progenitors of GRBs/SNe in that part of the thesis. CONTENTS Contents v Acronyms xi List of Figures xiii List of Tables xv Acknowledgments xvii Abstract xxi Sammenfatning xxiii Zusammenfassung xxvi 1 Introduction 5 1.1 A serendipitous discovery . 5 1.1.1 Once upon a time... 5 1.1.2 Better localization - the IPN . 5 1.1.3 CGRO . 6 1.1.4 The first afterglows - Beppo SAX and HETE . 7 1.1.5 The Swift era.................................... 8 1.1.6 GLAST and the future . 9 1.2 The most powerfull explosions in the Universe . 11 1.2.1 Prompt emission - the fireball model . 11 1.2.2 Progenitors of GRBs . 15 1.2.3 Cosmology with GRBs? . 18 1.3 The galaxy . 18 1.3.1 Long GRB hosts . 19 1.3.2 Short GRB hosts . 20 1.4 It’s all about being fast or when the mobile rings twice . 21 1.4.1 The GCN Network . 21 1.4.2 ToO observations . 22 1.4.3 Examples of ToO observations and results . 23 v IABSORPTION LINE SPECTROSCOPY OF GRB AFTERGLOWS 29 2 What do we learn from distant GRB hosts? 31 2.1 The high redshift universe . 31 2.1.1 Indirect observations - Quasar absorption line systems . 31 2.1.2 Direct imaging . 33 2.2 Absorption line profiles and column density determinations . 34 2.2.1 Doppler, Lorentz- and Voigt profiles . 34 2.2.2 The Curve of Growth method . 36 2.2.3 Apparent optical depth . 37 2.2.4 Voigt profile fitting . 37 2.3 The metallicity problem . 38 2.3.1 QSO and GRB metallicities . 38 2.3.2 Relative abundances and dust depletion . 40 2.4 Distances . 41 2.4.1 Finestructure lines . 42 2.4.2 Neutral species . 43 2.4.3 Indication for material from the circumburst medium? - NV in GRB sight- lines . 44 2.5 The dynamical universe . 44 2.5.1 Winds from the progenitor star? . 44 2.5.2 Rotating disks and Superwinds . 45 3 Photometry and Spectroscopy of GRB 060526 49 3.1 Introduction . 49 3.2 Observations . 50 3.2.1 Photometry . 50 3.2.2 Spectroscopy . 51 3.2.3 The multi-color light curve . 51 3.2.4 Analysis of the light curve variability . 53 3.2.5 Modelling the light curve numerically with energy injections . 55 3.2.6 The spectral energy distribution and host extinction . 56 3.2.7 Host search . 57 3.3 Spectroscopy results . 59 3.3.1 Line identification . 59 3.3.2 Column densities from curve of growth analysis . 59 3.3.3 Metallicity and relative abundances . 62 3.4 Discussion and conclusions . 63 3.4.1 A highly variable light curve . 63 3.4.2 A moderate metallicity environment . 64 4 ISM studies of GRB 030329 with high resolution spectroscopy 69 4.1 Introduction . 69 4.2 Data sample . 70 4.3 Line analysis . 71 4.3.1 Emission lines . 71 4.3.2 Absorption lines . 73 4.4 Results . 75 4.4.1 Redshift . 75 4.4.2 Broadening of the emission lines . 75 4.4.3 Galactic and host extinction . 76 4.4.4 SFR . 76 4.4.5 Metallicity of the host . 77 4.5 Absorption line kinematics . 77 4.5.1 Fitting of the absorption systems . 77 4.5.2 Interpretation of the Mg I & II velocity structure . 79 4.6 Conclusion . 81 5 The host of GRB 060206: kinematics of a distant galaxy 83 5.1 Introduction . 83 5.2 Observations . 84 5.2.1 Spectroscopy . 84 5.2.2 Imaging . 84 5.3 Extinction along the line-of-sight . 85 5.4 Absorption line analysis . 85 5.5 Velocity components in the host galaxy . 86 5.5.1 Fine structure levels . 86 5.5.2 N V absorption lines . 91 5.5.3 The nature of the absorption systems . 92 5.5.4 Comparison with QSO-DLAs . 93 5.6 The host in emission . 94 5.7 An intervening system at z = 1.48 ........................... 95 5.7.1 Properties of the intervening absorber . 95 5.7.2 Variability of the intervening system? . 96 5.7.3 Identifying the absorber in emission . 96 5.8 Conclusions . 98 II RESOLVED HOST GALAXIES AND THE SN-GRB MYSTERY 101 6 GRBs with Supernovae, Supernovae without GRBs and GRBs without supernova 103 6.1 The SN-GRB connection . 103 6.1.1 The common picture between 1998 and 2006.
Load more

Recommended publications
  • 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.
    [Show full text]
  • Optical and NIR Observations of the Afterglow of GRB 020813 The
    A&A 404, L5–L9 (2003) Astronomy DOI: 10.1051/0004-6361:20030525 & c ESO 2003 Astrophysics Editor Optical and NIR observations of the afterglow of GRB 020813 the 1 1 1 2 3 2 4 1 to S. Covino , D. Malesani , F. Tavecchio , L. A. Antonelli , A. Arkharov , A. Di Paola , D. Fugazza , G. Ghisellini , V. Larionov5,6, D. Lazzati7, F. Mannucci8, N. Masetti9, R. Barrena4, S. Benetti10, A. J. Castro–Tirado11, S. Di Serego Alighieri12, F. Fiore2, F. Frontera9,13, A. Fruchter14, F. Ghinassi4, M. Gladders15, P. B. Hall16,17, G. L. Israel2, S. Klose18, A. Magazz`u4, E. Palazzi9, M. Pedani4, E. Pian19, 1 1 2 P. Romano , M. Stefanon , and L. Stella Letter 1 INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy 2 INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone (Roma), Italy 3 Central Astronomical Observatory at Pulkovo, Pulkovskoe shosse 65, 196140 Saint Petersburg, Russia 4 INAF, Telescopio Nazionale Galileo, Roque de Los Muchachos, PO box 565, 38700 Santa Cruz de La Palma, Spain 5 St. Petersburg University, St. Petersburg, Petrodvorets, Universitetsky pr. 28, 198504 St. Petersburg, Russia 6 Isaac Newton Institute of Chile, St. Petersburg Branch 7 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK 8 Istituto di Radioastronomia, CNR, largo E. Fermi 5, 50125 Firenze, Italy 9 Istituto di Astrofisica Spaziale e Fisica Cosmica, via Gobetti 101, 40129 Bologna, Italy 10 INAF, Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy 11 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, PO Box 03004, 18080 Granada, Spain 12 INAF, Osservatorio Astrofisico di Arcetri, largo E.
    [Show full text]
  • 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”.
    [Show full text]
  • 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).
    [Show full text]
  • A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
    TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques.
    [Show full text]
  • Radio Observations of the Host Galaxies of Short Gamma-Ray Bursts
    Radio observations of the host galaxies of short Gamma-Ray Bursts Dissertation zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) vorgelegt dem Rat der Physikalisch-Astronomischen Fakultat¨ der Friedrich-Schiller-Universitat¨ Jena von M. Sc. Ana Maria Nicuesa Guelbenzu Gutachter 1. Prof. Dr. Katharina Schreyer, Friedrich-Schiller-Universit¨at Jena, Germany 2. Prof. Dr. Ulrich Heber, Friedrich-Alexander-Universit¨at Erlangen-N¨urnberg, Germany 3. Prof. Dr. Giampaolo Piotto, University of Padua, Italy Tag der Disputation: 13.03.2020 a mi madre Magdalena Guelbenzu Bandr´es . Contents 1 Introduction 1 1.1GRBs,theirafterglowsandprogenitors...................... 1 1.1.1 Theburstsandtheirbimodaldistribution.................. 1 1.1.2 Theafterglows............................... 3 1.1.3 GRBprogenitormodels........................... 6 1.1.4 ShortGRBs................................. 7 1.2 Long-GRB host galaxies . .......................... 9 1.2.1 Photometricstudies............................. 9 1.2.2 Spectroscopicstudies............................ 10 1.2.2.1 Starformationrates....................... 11 1.2.2.2 GRBenvironments,ISMmetallicities.............. 11 1.2.3 Legacysamples............................... 14 1.2.4 Radioobservations............................. 15 1.3Short-GRBhostgalaxies.............................. 18 1.3.1 Host galaxies as tracers of the nature of the short-GRB progenitors . 18 1.3.2 IdentifyingthehostgalaxiesofshortGRBs................ 20 1.3.3 Previousradiostudiesofshort-GRBhostgalaxies............
    [Show full text]
  • Gamma-Ray Bursts and the Sociology of Science
    GAMMA-RAY BURSTS AND THE SOCIOLOGY OF SCIENCE ALVARO DE RUJULA´ CERN 1211 Geneva 23, Switzerland E-mail: [email protected] ABSTRACT I discuss what we have learned about Gamma-Ray Bursts (GRBs) by studying their afterglows, and how these are interpreted in the generally-accepted fireball model of GRBs, as well as in the generally-unaccepted cannonball model of the same phenomena. The interpretation of GRBs is a good example around which to frame a discussion of the different approaches to science found in various fields, such as high-energy physics (HEP), high-energy astrophysics, or even the deciphering of ancient languages. I use this example to draw conclusions on post-academic science, and on the current status of European HEP. 1. Motivation Why would one give a talk on the sociology of science at a meeting on Un altro modo di guardare il cielo, or more generally on neutrino physics, the meeting definitely not being centred on sociology? My excuse is that, when talking about GRBs, I have always detected a very considerable interest on their sociology: an extremely negative reaction to my views on the subject in meetings on GRBs, and an extremely surprised and curiosity-driven interest from HEP or general audiences. A talk or article such as this one may seem rather unusual, but it is not. A precedent with quite similar content and conclusions has been written by Charles Dermer1). arXiv:hep-ph/0306140v1 16 Jun 2003 2. Introduction Some three times a day, on average, gamma-ray bursts (GRBs) reach the upper atmosphere from isotropically distributed sky locations.
    [Show full text]
  • Constraining the Progenitor and Central Engine of Gamma-Ray Bursts with Observational Data
    UNLV Theses, Dissertations, Professional Papers, and Capstones 5-1-2015 Constraining the Progenitor and Central Engine of Gamma-ray Bursts with Observational Data Lu Houjun University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/thesesdissertations Part of the Stars, Interstellar Medium and the Galaxy Commons Repository Citation Houjun, Lu, "Constraining the Progenitor and Central Engine of Gamma-ray Bursts with Observational Data" (2015). UNLV Theses, Dissertations, Professional Papers, and Capstones. 2366. http://dx.doi.org/10.34917/7645921 This Dissertation 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 Dissertation 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 Dissertation has been accepted for inclusion in UNLV Theses, Dissertations, Professional Papers, and Capstones by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. CONSTRAINING THE PROGENITOR AND CENTRAL ENGINE OF GAMMA-RAY BURSTS WITH OBSERVATIONAL DATA by HOUJUN L¨u Bachelor of Science Neijiang Normal University, China 2007 Master of Science Guangxi University, China 2010 A dissertation
    [Show full text]
  • The Possible Detection of a Binary Companion to a Type Ibn Supernova Progenitor J
    The Astrophysical Journal, 833:128 (6pp), 2016 December 20 doi:10.3847/1538-4357/833/2/128 © 2016. The American Astronomical Society. All rights reserved. THE POSSIBLE DETECTION OF A BINARY COMPANION TO A TYPE IBN SUPERNOVA PROGENITOR J. R. Maund1,7, A. Pastorello2, S. Mattila3,4, K. Itagaki5, and T. Boles6 1 Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK 2 INAF—Osservatorio Astronomico di Padova. Vicolo Osservatorio 5, I-35122, Padova, Italy 3 Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 4 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 5 Itagaki Astronomical Observatory, Teppo-cho, 990-2492 Yamagata, Japan 6 Coddenham Astronomical Observatory, Suffolk IP6 9QY, UK Received 2016 April 28; revised 2016 August 23; accepted 2016 September 20; published 2016 December 13 ABSTRACT We present late-time observations of the site of the Type Ibn supernova (SN) 2006jc, acquired with the Hubble Space Telescope Advanced Camera for Surveys. A faint blue source is recovered at the SN position, with brightness mFW435 =26.76 0.20, mFW555 =26.60 0.23 and mFW625 =26.32 0.19 mag, although there is no detection in a contemporaneous narrow-band Ha image. The spectral energy distribution of the late-time source is well-fit by a stellar-like spectrum (logTeff > 3.7 and log LL > 4), subject to only a small degree of reddening —consistent with that estimated for SN2006jc itself at early-times. The lack of further outbursts after the explosion of SN2006jc suggests that the precursor outburst originated from the progenitor.
    [Show full text]
  • OGLE-2014-SN-131: a Long-Rising Type Ibn Supernova from a Massive Progenitor E
    Astronomy & Astrophysics manuscript no. output c ESO 2017 March 8, 2017 OGLE-2014-SN-131: A long-rising Type Ibn supernova from a massive progenitor E. Karamehmetoglu1, F. Taddia1, J. Sollerman1, Ł. Wyrzykowski2, S. Schmidl3, M. Fraser4, C. Fremling1, J. Greiner5; 6, C. Inserra7, Z. Kostrzewa-Rutkowska2; 8; 9, K. Maguire7, S. Smartt7, M. Sullivan10, and D. R. Young7 1 Department of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, Sweden. e-mail: [email protected] 2 Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland. 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany. 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. 5 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany. 6 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany. 7 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK. 8 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands. 9 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands. 10 Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK. Received date / Accepted date ABSTRACT Context. Type Ibn supernovae (SNe Ibn) are thought to be the core-collapse explosions of massive stars whose ejecta interact with He-rich circumstellar material (CSM). Aims. We report the discovery of a SN Ibn, with the longest rise-time ever observed, OGLE-2014-SN-131. We discuss the potential powering mechanisms and the progenitor nature of this peculiar stripped-envelope (SE), circumstellar-interacting SN.
    [Show full text]
  • Rapid-Response Mode VLT/UVES Spectroscopy of GRB 060418
    A&A 468, 83–96 (2007) Astronomy DOI: 10.1051/0004-6361:20066780 & c ESO 2007 Astrophysics Rapid-response mode VLT/UVES spectroscopy of GRB 060418 Conclusive evidence for UV pumping from the time evolution of Fe II and Ni II excited- and metastable-level populations P. M. Vreeswijk1,2, C. Ledoux1, A. Smette1, S. L. Ellison3, A. O. Jaunsen4,M.I.Andersen5,A.S.Fruchter6, J. P. U. Fynbo7, J. Hjorth7,A.Kaufer1, P. Møller8, P. Petitjean9,10,S.Savaglio11, and R. A. M. J. Wijers12 1 European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile 3 Department of Physics and Astronomy, University of Victoria, Victoria, BC, Canada 4 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway 5 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany 6 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 7 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark 8 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany 9 Institut d’Astrophysique de Paris – UMR 7095 CNRS & Université Pierre et Marie Curie, 98bis Boulevard Arago, 75014 Paris, France 10 LERMA, Observatoire de Paris, 61 Avenue de l’Observatoire, 75014 Paris, France 11 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching bei München, Germany 12 Astronomical Institute “Anton Pannekoek”, University of Amsterdam & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands Received 20 November 2006 / Accepted 11 March 2007 ABSTRACT We present high-resolution spectroscopic observations of GRB 060418, obtained with VLT/UVES.
    [Show full text]
  • Gamma Ray Bursts in the Afterglow Era
    Chin. J. Astron. Astrophys. Vol. 3 (2003), Suppl., 439–448 Chinese Journal of (http://www.chjaa.org) Astronomy and Astrophysics Gamma Ray Bursts in the Afterglow Era Filippo Frontera ⋆ 1 University of Ferrara, Physics Department, Via Paradiso, 12, 44100 Ferrara, Italy 2 Istituto Astrofisica Spaziale e Fisica Cosmica, INAF, Via P. Gobetti, 101, 44129 Bologna, Italy Abstract In this review paper I will summarize some of the relevant results ob- tained with the Italian satellite BeppoSAX on the prompt and afterglow emission of Gamma Ray Bursts. I will also discuss the most relevant open issues on these events. Key words: gamma–rays: bursts – gamma–rays: observations 1 INTRODUCTION After about 30 years of mystery, the distance scale issue of Gamma Ray Bursts (GRBs) has been definitely settled thanks to the X-ray astronomy mission BeppoSAX , an Italian satellite with Dutch participation (Boella et al. 1997a). BeppoSAX not only has permitted this issue to be resolved but has also provided most of the exciting results of the last seven years in GRB astron- omy. The satellite (see Fig. 1), launched on 1996 April 30, was switched off on April 29, 2002, af- ter 6 years of operational life. The high performance of BeppoSAX for GRB studies was due to a particularly well-matched configuration of its payload, with both wide field instruments (WFIs) and narrow field telescopes (NFTs). The WFIs comprised a γ–ray (40–700 keV) all–sky mon- itor (Gamma-Ray Burst Monitor, GRBM, Frontera et al. 1997) and two Wide Field Cameras (WFCs, 2–28 keV, Jager et al.
    [Show full text]