The Formation of Nebular Spectra in Core-Collapse Supernovae
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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
A Holistic View of the GRB-SN Connection Alicia M Soderberg
A Holistic View of the GRB-SN Connection Alicia M Soderberg Harvard University (Credit: M. Bietenholz) Monday, April 19, 2010 12 Years since GRB 980425 d=38 Mpc Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 12 Years since GRB 980425 d=38 Mpc Happy Birthday Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN Connection L ~ 1053 erg/s L ~ 1042 erg/s Emission Process =? Ni-56 decay Δt ~ seconds Δt ~ 1 month Hard X-ray Optical (Credit: P. Challis) Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003dh at z=0.169 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 SN 2006aj at z=0.03 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169 Most GRBs accompanied by Broad-lined SNe Ic SN 2006aj at z=0.03 Alicia M. -
Ultraviolet Spectroscopy of Type Iib Supernovae: Diversity and the Impact of Circumstellar Material
LJMU Research Online Ben-Ami, S, Hachinger, S, Gal-Yam, A, Mazzali, PA, Filippenko, AV, Horesh, A, Matheson, T, Modjaz, M, Sauer, DN, Silverman, JM, Smith, N and Yaron, O ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL http://researchonline.ljmu.ac.uk/id/eprint/2871/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Ben-Ami, S, Hachinger, S, Gal-Yam, A, Mazzali, PA, Filippenko, AV, Horesh, A, Matheson, T, Modjaz, M, Sauer, DN, Silverman, JM, Smith, N and Yaron, O (2015) ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL. LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ Ultraviolet Spectroscopy of Type IIb Supernovae: Diversity and the Impact of Circumstellar Material Sagi Ben-Ami1,2,3, Stephan Hachinger4,5, Avishay Gal-Yam2,6, Paolo A. -
The Progenitor of Supernova 2011Dh/Ptf11eon in Messier 51
To Appear in ApJ Letters A Preprint typeset using LTEX style emulateapj v. 11/10/09 THE PROGENITOR OF SUPERNOVA 2011DH/PTF11EON IN MESSIER 51 Schuyler D. Van Dyk1, Weidong Li2, S. Bradley Cenko2, Mansi M. Kasliwal3, Assaf Horesh3, Eran O. Ofek3,4, Adam L. Kraus5,6, Jeffrey M. Silverman2, Iair Arcavi7, Alexei V. Filippenko2, Avishay Gal-Yam7, Robert M. Quimby3, Shrinivas R. Kulkarni3, Ofer Yaron7, and David Polishook7 To Appear in ApJ Letters ABSTRACT We have identified a luminous star at the position of supernova (SN) 2011dh/PTF11eon, in pre- SN archival, multi-band images of the nearby, nearly face-on galaxy Messier 51 (M51) obtained by the Hubble Space Telescope with the Advanced Camera for Surveys. This identification has been confirmed, to the highest available astrometric precision, using a Keck-II adaptive-optics image. The available early-time spectra and photometry indicate that the SN is a stripped-envelope, core-collapse Type IIb, with a more compact progenitor (radius ∼ 1011 cm) than was the case for the well-studied SN IIb 1993J. We infer that the extinction to SN 2011dh and its progenitor arises from a low Galactic foreground contribution, and that the SN environment is of roughly solar metallicity. The detected 0 object has absolute magnitude MV ≈ −7.7 and effective temperature ∼ 6000 K. The star’s radius, ∼ 1013 cm, is more extended than what has been inferred for the SN progenitor. We speculate that the detected star is either an unrelated star very near the position of the actual progenitor, or, more likely, the progenitor’s companion in a mass-transfer binary system. -
Optical and Near-Infrared Observations of SN 2011Dh-The First 100 Days
Astronomy & Astrophysics manuscript no. sn2011dh-astro-ph-v2 c ESO 2018 November 4, 2018 Optical and near-infrared observations of SN 2011dh - The first 100 days. M. Ergon1, J. Sollerman1, M. Fraser2, A. Pastorello3, S. Taubenberger4, N. Elias-Rosa5, M. Bersten6, A. Jerkstrand2, S. Benetti3, M.T. Botticella7, C. Fransson1, A. Harutyunyan8, R. Kotak2, S. Smartt2, S. Valenti3, F. Bufano9; 10, E. Cappellaro3, M. Fiaschi3, A. Howell11, E. Kankare12, L. Magill2; 13, S. Mattila12, J. Maund2, R. Naves14, P. Ochner3, J. Ruiz15, K. Smith2, L. Tomasella3, and M. Turatto3 1 The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, 106 91 Stockholm, Sweden 2 Astrophysics Research Center, School of Mathematics and Physics, Queens University Belfast, Belfast, BT7 1NN, UK 3 INAF, Osservatorio Astronomico di Padova, vicolo dell’Osservatorio n. 5, 35122 Padua, Italy 4 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany 5 Institut de Ciències de l’Espai (IEEC-CSIC), Facultat de Ciències, Campus UAB, E-08193 Bellaterra, Spain. 6 Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan 7 INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16 80131 Napoli, Italy 8 Fundación Galileo Galilei-INAF, Telescopio Nazionale Galileo, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja, TF - Spain 9 INAF, Osservatorio Astrofisico di Catania, Via Santa Sofia, I-95123, Catania, Italy 10 Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile 11 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117 12 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 13 Isaac Newton Group, Apartado 321, E-38700 Santa Cruz de La Palma, Spain 14 Observatorio Montcabrer, C Jaume Balmes 24, Cabrils, Spain 15 Observatorio de Cántabria, Ctra. -
Kavli IPMU Annual 2014 Report
ANNUAL REPORT 2014 REPORT ANNUAL April 2014–March 2015 2014–March April Kavli IPMU Kavli Kavli IPMU Annual Report 2014 April 2014–March 2015 CONTENTS FOREWORD 2 1 INTRODUCTION 4 2 NEWS&EVENTS 8 3 ORGANIZATION 10 4 STAFF 14 5 RESEARCHHIGHLIGHTS 20 5.1 Unbiased Bases and Critical Points of a Potential ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙20 5.2 Secondary Polytopes and the Algebra of the Infrared ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙21 5.3 Moduli of Bridgeland Semistable Objects on 3- Folds and Donaldson- Thomas Invariants ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙22 5.4 Leptogenesis Via Axion Oscillations after Inflation ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙23 5.5 Searching for Matter/Antimatter Asymmetry with T2K Experiment ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ 24 5.6 Development of the Belle II Silicon Vertex Detector ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙26 5.7 Search for Physics beyond Standard Model with KamLAND-Zen ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙28 5.8 Chemical Abundance Patterns of the Most Iron-Poor Stars as Probes of the First Stars in the Universe ∙ ∙ ∙ 29 5.9 Measuring Gravitational lensing Using CMB B-mode Polarization by POLARBEAR ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ 30 5.10 The First Galaxy Maps from the SDSS-IV MaNGA Survey ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙32 5.11 Detection of the Possible Companion Star of Supernova 2011dh ∙ ∙ ∙ ∙ ∙ ∙ -
Issue 36, June 2008
June2008 June2008 In This Issue: 7 Supernova Birth Seen in Real Time Alicia Soderberg & Edo Berger 23 Arp299 With LGS AO Damien Gratadour & Jean-René Roy 46 Aspen Instrument Update Joseph Jensen On the Cover: NGC 2770, home to Supernova 2008D (see story starting on page 7 Engaging Our Host of this issue, and image 52 above showing location Communities of supernova). Image Stephen J. O’Meara, Janice Harvey, was obtained with the Gemini Multi-Object & Maria Antonieta García Spectrograph (GMOS) on Gemini North. 2 Gemini Observatory www.gemini.edu GeminiFocus Director’s Message 4 Doug Simons 11 Intermediate-Mass Black Hole in Gemini South at moonset, April 2008 Omega Centauri Eva Noyola Collisions of 15 Planetary Embryos Earthquake Readiness Joseph Rhee 49 Workshop Michael Sheehan 19 Taking the Measure of a Black Hole 58 Polly Roth Andrea Prestwich Staff Profile Peter Michaud 28 To Coldly Go Where No Brown Dwarf 62 Rodrigo Carrasco Has Gone Before Staff Profile Étienne Artigau & Philippe Delorme David Tytell Recent 31 66 Photo Journal Science Highlights North & South Jean-René Roy & R. Scott Fisher Photographs by Gemini Staff: • Étienne Artigau NICI Update • Kirk Pu‘uohau-Pummill 37 Tom Hayward GNIRS Update 39 Joseph Jensen & Scot Kleinman FLAMINGOS-2 Update Managing Editor, Peter Michaud 42 Stephen Eikenberry Science Editor, R. Scott Fisher MCAO System Status Associate Editor, Carolyn Collins Petersen 44 Maxime Boccas & François Rigaut Designer, Kirk Pu‘uohau-Pummill 3 Gemini Observatory www.gemini.edu June2008 by Doug Simons Director, Gemini Observatory Director’s Message Figure 1. any organizations (Gemini Observatory 100 The year-end task included) have extremely dedicated and hard- completion statistics 90 working staff members striving to achieve a across the entire M 80 0-49% Done observatory are worthwhile goal. -
Core-Collapse Supernovae Overview with Swift Collaboration
Publications Spring 2015 Core-Collapse Supernovae Overview with Swift Collaboration Kiranjyot Gill Embry-Riddle Aeronautical University, [email protected] Michele Zanolin Embry-Riddle Aeronautical University, [email protected] Marek Szczepańczyk Embry-Riddle Aeronautical University, [email protected] Follow this and additional works at: https://commons.erau.edu/publication Part of the Astrophysics and Astronomy Commons, and the Physics Commons Scholarly Commons Citation Gill, K., Zanolin, M., & Szczepańczyk, M. (2015). Core-Collapse Supernovae Overview with Swift Collaboration. , (). Retrieved from https://commons.erau.edu/publication/3 This Report is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Core-Collapse Supernovae Overview with Swift Collaboration∗ Kiranjyot Gill,y Dr. Michele Zanolin,z and Marek Szczepanczykx Physics Department, Embry Riddle Aeronautical University (Dated: June 30, 2015) The Core-Collapse supernovae (CCSNe) mark the dynamic and explosive end of the lives of massive stars. The mysterious mechanism, primarily focused with the shock revival phase, behind CCSNe explosions could be explained by detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, as a hint of the times where to search for the emission of GWs. More of these hints would be very helpful. For the first time in history a Harvard group has observed X-ray transients in coincidence with optical CCSNe. -
Direct Identification of Core-‐Collapse SN Progenitors
Direct Identification of Core-Collapse SN Progenitors Schuyler D. Van Dyk (IPAC/Caltech) Main collaborators: Nancy Elias –Rosa, Alex Filippenko, Weidong Li Core-Collapse SNe: Classification Thermonuclear SNe Core Collapse SNe NO Hydrogen Hydrogen NO II/Ib Si II lines hybrid Light curve differences Si II lines Linear Plateau Ia He IIb II-L II-P NO YES H lines Narrow disappear H lines dominate in ~few IIn at all epochs Ic Ib weeks, reappear in nebular (hypernovae, phase Envelope Stripping (adapted froM Ic-bl, SN-GRB) Turatto 2003) Progenitor ID Paucity2 Core-Collapse SNe: Classification 56Ni/56Co decay (Van Dyk & Matheson 2012) Mass of 56Ni depends on Mass of core 3 Core-Collapse SNe: Classification SN II-L 2009kr in NGC 1832 (Elias-Rosa et al. 2010) 4 Core-Collapse SNe: Classification SN IIb 2008ax in NGC 4490 SN IIb 1993J in M81 (Chornock et al. 2011) (Richmond et al. 1996) 5 Core-Collapse SNe: Rates Li et al. (2010) Lick Observatory SN Search 6 Direct Identification of SN Progenitors SN 1978K (IIn) SN 2008bk (II-P) SN 1987A (II pec) SN 2008cn (II-P ?) SN 1993J (IIb) SN 2009hd (II-L ?) SN 1999ev (II-P) SN 2009kr (II-L) SN 2003gd (II-P) SN 2009md (II-P) SN 2004A (II-P) SN 2010jl (IIn) ? SN 2004et (II-P) SN 2011dh (IIb) SN 2005cs (II-P) SN 2012A (II-P) SN 2005gl (IIn) SN 2012aw (II-P) SN 2008ax (IIb) 7 SN II-P Progenitors The Most coMMon core-collapse SNe high-lum II-P “normal” II-P low-lum II-P Inserra et al. -
A Comparative Study of Type II-P and II-L Supernova Rise Times As Exemplified by the Case of Lsq13cuw⋆
A&A 582, A3 (2015) Astronomy DOI: 10.1051/0004-6361/201525868 & c ESO 2015 Astrophysics A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw E. E. E. Gall1,J.Polshaw1,R.Kotak1, A. Jerkstrand1, B. Leibundgut2, D. Rabinowitz3, J. Sollerman5, M. Sullivan6, S. J. Smartt1, J. P. Anderson7, S. Benetti8,C.Baltay9,U.Feindt10,11, M. Fraser4, S. González-Gaitán12,13 ,C.Inserra1, K. Maguire2, R. McKinnon9,S.Valenti14,15, and D. Young1 1 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK e-mail: [email protected] 2 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany 3 Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06520, USA 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 5 Department of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, Sweden 6 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 7 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 8 INAF Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 9 Department of Physics, Yale University, New Haven, CT 06250-8121, USA 10 Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, 12489 Berlin, Germany 11 Physikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, Germany 12 Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile 13 Departamento -
HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land
HET Publication Report HET Board Meeting 3/4 December 2020 Zoom Land 1 Executive Summary • There are now 420 peer-reviewed HET publications – Fifteen papers published in 2019 – As of 27 November, nineteen published papers in 2020 • HET papers have 29363 citations – Average of 70, median of 39 citations per paper – H-number of 90 – 81 papers have ≥ 100 citations; 175 have ≥ 50 cites • Wide angle surveys account for 26% of papers and 35% of citations. • Synoptic (e.g., planet searches) and Target of Opportunity (e.g., supernovae and γ-ray bursts) programs have produced 47% of the papers and 47% of the citations, respectively. • Listing of the HET papers (with ADS links) is given at http://personal.psu.edu/dps7/hetpapers.html 2 HET Program Classification Code TypeofProgram Examples 1 ToO Supernovae,Gamma-rayBursts 2 Synoptic Exoplanets,EclipsingBinaries 3 OneorTwoObjects HaloofNGC821 4 Narrow-angle HDF,VirgoCluster 5 Wide-angle BlazarSurvey 6 HETTechnical HETQueue 7 HETDEXTheory DarkEnergywithBAO 8 Other HETOptics Programs also broken down into “Dark Time”, “Light Time”, and “Other”. 3 Peer-reviewed Publications • There are now 420 journal papers that either use HET data or (nine cases) use the HET as the motivation for the paper (e.g., technical papers, theoretical studies). • Except for 2005, approximately 22 HET papers were published each year since 2002 through the shutdown. A record 44 papers were published in 2012. • In 2020 a total of fifteen HET papers appeared; nineteen have been published to date in 2020. • Each HET partner has published at least 14 papers using HET data. • Nineteen papers have been published from NOAO time. -
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