The Key Role of Bepposax in the GRB History ?
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The Optical Afterglow of GRB 000911: Evidence for an Associated Supernova??
A&A 378, 996–1002 (2001) Astronomy DOI: 10.1051/0004-6361:20011282 & c ESO 2001 Astrophysics The optical afterglow of GRB 000911: Evidence for an associated supernova?? D. Lazzati1,S.Covino2, G. Ghisellini2,D.Fugazza2,S.Campana2,P.Saracco2,P.A.Price3,4,E.Berger3, S. Kulkarni3, E. Ramirez–Ruiz1,A.Cimatti5, M. Della Valle5, S. di Serego Alighieri5,A.Celotti6, F. Haardt7,G.L.Israel8, and L. Stella8 1 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK 2 Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate (Lc), Italy 3 Palomar Observatory, 105-24, California Institute of Technology, Pasadena, CA 91125, USA 4 Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia 5 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy 6 SISSA/ISAS, via Beirut 4, 34014 Trieste, Italy 7 Universit`a dell’Insubria, Via Lucini 3, 22100 Como, Italy 8 Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monteporzio Catone, Italy Received 12 July 2001 / Accepted 12 September 2001 Abstract. We present photometric and spectroscopic observations of the late afterglow of GRB 000911, starting ∼1 day after the burst event and lasting ∼8 weeks. We detect a moderately significant re–brightening in the R, I and J lightcurves, associated with a sizable reddening of the spectrum. This can be explained through the presence of an underlying supernova, outshining the afterglow ∼30 days after the burst event. Alternative explanations are discussed. Key words. gamma rays: bursts – supernovae: general 1. Introduction (Djorgovskij et al. 1999), a moderate amount of multiband data but lacked spectroscopic coverge. -
Precollimator for X-Ray Telescope (Stray-Light Baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017
Mindrum.com Precollimator for X-Ray Telescope (stray-light baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017 1 Overview Mindrum.com Precollimator •Past •Present •Future 2 Past Mindrum.com • Space X-Ray Telescopes (XRT) • Basic Structure • Effectiveness • Past Construction 3 Space X-Ray Telescopes Mindrum.com • XMM-Newton 1999 • Chandra 1999 • HETE-2 2000-07 • INTEGRAL 2002 4 ESA/NASA Space X-Ray Telescopes Mindrum.com • Swift 2004 • Suzaku 2005-2015 • AGILE 2007 • NuSTAR 2012 5 NASA/JPL/ASI/JAXA Space X-Ray Telescopes Mindrum.com • Astrosat 2015 • Hitomi (ASTRO-H) 2016-2016 • NICER (ISS) 2017 • HXMT/Insight 慧眼 2017 6 NASA/JPL/CNSA Space X-Ray Telescopes Mindrum.com NASA/JPL-Caltech Harrison, F.A. et al. (2013; ApJ, 770, 103) 7 doi:10.1088/0004-637X/770/2/103 Basic Structure XRT Mindrum.com Grazing Incidence 8 NASA/JPL-Caltech Basic Structure: NuSTAR Mirrors Mindrum.com 9 NASA/JPL-Caltech Basic Structure XRT Mindrum.com • XMM Newton XRT 10 ESA Basic Structure XRT Mindrum.com • XMM-Newton mirrors D. de Chambure, XMM Project (ESTEC)/ESA 11 Basic Structure XRT Mindrum.com • Thermal Precollimator on ROSAT 12 http://www.xray.mpe.mpg.de/ Basic Structure XRT Mindrum.com • AGILE Precollimator 13 http://agile.asdc.asi.it Basic Structure Mindrum.com • Spektr-RG 2018 14 MPE Basic Structure: Stray X-Rays Mindrum.com 15 NASA/JPL-Caltech Basic Structure: Grazing Mindrum.com 16 NASA X-Ray Effectiveness: Straylight Mindrum.com • Correct Reflection • Secondary Only • Backside Reflection • Primary Only 17 X-Ray Effectiveness Mindrum.com • The Crab Nebula by: ROSAT (1990) Chandra 18 S. -
X-Ray and Gamma-Ray Variability of NGC 1275
galaxies Article X-ray and Gamma-ray Variability of NGC 1275 Varsha Chitnis 1,*,† , Amit Shukla 2,*,† , K. P. Singh 3 , Jayashree Roy 4 , Sudip Bhattacharyya 5, Sunil Chandra 6 and Gordon Stewart 7 1 Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India 2 Discipline of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India 3 Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, SAS Nagar, Manauli 140306, India; [email protected] 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India; [email protected] 5 Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India; [email protected] 6 Centre for Space Research, North-West University, Potchefstroom 2520, South Africa; [email protected] 7 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK; [email protected] * Correspondence: [email protected] (V.C.); [email protected] (A.S.) † These authors contributed equally to this work. Received: 30 June 2020; Accepted: 24 August 2020; Published: 28 August 2020 Abstract: Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission. -
Nustar Observatory Guide
NuSTAR Guest Observer Program NuSTAR Observatory Guide Version 3.2 (June 2016) NuSTAR Science Operations Center, California Institute of Technology, Pasadena, CA NASA Goddard Spaceflight Center, Greenbelt, MD nustar.caltech.edu heasarc.gsfc.nasa.gov/docs/nustar/index.html i Revision History Revision Date Editor Comments D1,2,3 2014-08-01 NuSTAR SOC Initial draft 1.0 2014-08-15 NuSTAR GOF Release for AO-1 Addition of more information about CZT 2.0 2014-10-30 NuSTAR SOC detectors in section 3. 3.0 2015-09-24 NuSTAR SOC Update to section 4 for release of AO-2 Update for NuSTARDAS v1.6.0 release 3.1 2016-05-10 NuSTAR SOC (nusplitsc, Section 5) 3.2 2016-06-15 NuSTAR SOC Adjustment to section 9 ii Table of Contents Revision History ......................................................................................................................................................... ii 1. INTRODUCTION ................................................................................................................................................... 1 1.1 NuSTAR Program Organization ..................................................................................................................................................................................... 1 2. The NuSTAR observatory .................................................................................................................................... 2 2.1 NuSTAR Performance ........................................................................................................................................................................................................ -
Evidence for Supernova Light in All Gamma-Ray Burst Afterglow A
Clemson University TigerPrints Publications Physics and Astronomy Winter 12-13-2004 Evidence for Supernova Light in all Gamma-Ray Burst Afterglow A. Zeh Thüringer Landessternwarte Tautenburg S. Klose Thüringer Landessternwarte Tautenburg Dieter H. Hartmann Department of Physics and Astronomy, Clemson University, [email protected] Follow this and additional works at: https://tigerprints.clemson.edu/physastro_pubs Recommended Citation Please use publisher's recommended citation. This Article is brought to you for free and open access by the Physics and Astronomy at TigerPrints. It has been accepted for inclusion in Publications by an authorized administrator of TigerPrints. For more information, please contact [email protected]. 22nd Texas Symposium on Relativistic Astrophysics at Stanford University, Dec. 13-17, 2004 Evidence for Supernova Light in All Gamma-Ray Burst Afterglows A. Zeh, S. Klose Thur¨ inger Landessternwarte Tautenburg, 07778 Tautenburg, Germany D. H. Hartmann Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-0978 We present an update of our systematic analyses of all Gamma-Ray Burst (GRB) afterglow data, now published through the end of 2004, in an attempt to detect the predicted supernova light component. We fit the observed photometric light curves as the sum of an afterglow, an underlying host galaxy, and a supernova component. The latter is modeled using published UBV RI light curves of SN 1998bw as a template. The total sample of afterglows with established redshifts contains now 29 bursts (GRB 970228 - GRB 041006). For 13 of them a weak supernova excess (scaled to SN 1998bw) was found. In agreement with our earlier result [47] we find that also in the updated sample all bursts with redshift ∼< 0.7 show a supernova excess in their afterglow light curves. -
Executive Summary
The Boston University Astronomy Department Annual Report 2010 Chair: James Jackson Administrator: Laura Wipf 1 2 TABLE OF CONTENTS Executive Summary 5 Faculty and Staff 5 Teaching 6 Undergraduate Programs 6 Observatory and Facilities 8 Graduate Program 9 Colloquium Series 10 Alumni Affairs/Public Outreach 10 Research 11 Funding 12 Future Plans/Departmental Needs 13 APPENDIX A: Faculty, Staff, and Graduate Students 16 APPENDIX B: 2009/2010 Astronomy Graduates 18 APPENDIX C: Seminar Series 19 APPENDIX D: Sponsored Project Funding 21 APPENDIX E: Accounts Income Expenditures 25 APPENDIX F: Publications 27 Cover photo: An ultraviolet image of Saturn taken by Prof. John Clarke and his group using the Hubble Space Telescope. The oval ribbons toward the top and bottom of the image shows the location of auroral activity near Saturn’s poles. This activity is analogous to Earth’s aurora borealis and aurora australis, the so-called “northern” and “southern lights,” and is caused by energetic particles from the sun trapped in Saturn’s magnetic field. 3 4 EXECUTIVE SUMMARY associates authored or co-authored a total of 204 refereed, scholarly papers in the disciplines’ most The Department of Astronomy teaches science to prestigious journals. hundreds of non-science majors from throughout the university, and runs one of the largest astronomy degree The funding of the Astronomy Department, the Center programs in the country. Research within the for Space Physics, and the Institute for Astrophysical Astronomy Department is thriving, and we retain our Research was changed this past year. In previous years, strong commitment to teaching and service. only the research centers received research funding, but last year the Department received a portion of this The Department graduated a class of twelve research funding based on grant activity by its faculty. -
Software Error Doomed Japanese Hitomi Spacecraft!
Software error doomed Japanese Hitomi spacecraft! ! Space agency declares the astronomy satellite a loss.! ! Japan’s flagship Hitomi astronomical satellite, which launched successfully on 17 February but tumbled out of control five weeks later, may have been doomed by a basic engineering error. Confused about how it was oriented in space and trying to stop itself from spinning, Hitomi's software apparently fired a thruster jet in the wrong direction — accelerating rather than slowing the craft's rotation.! ! http://www.nature.com/news/software-error-doomed-japanese-hitomi- spacecraft-1.19835! 1! Gamma-Ray Bursts- Longair 22.7! • Are bright flashes of γ-rays- for a short period of time (<100 sec )! • fluxes of ~0.1-100 photon/cm2/sec/keV emitted primarily in the 20-500 keV band.! – Distribution is isotropic on the sky! • Because of these properties it took ~30 years from their discovery (1967) to their identification! – They are at very large distances (z up to 8 (!)) with apparent luminosities of 3x1054 erg/sec! – Rate is ~10-7/yr/galaxy ! • What are they??- short timescales imply compact object ; what could the 2 33 energy reservoir be- Mc implies M~10 gms~ Msun if total conversion of mass into energy How does all this energy end up as γ-rays ?! – Location of long γRBs is in and near star forming regions in smallish galaxies- associated with star formation! – a few γRBs have been associated with a type Ic supernova! 2! 3! Gamma-Ray Bursts ! • Cosmic γ-ray bursts (GRBs) were first reported in 1973 by Klebesadel et al (l973) but were first seen -
Solar Orbiter and Sentinels
HELEX: Heliophysical Explorers: Solar Orbiter and Sentinels Report of the Joint Science and Technology Definition Team (JSTDT) PRE-PUBLICATION VERSION 1 Contents HELEX Joint Science and Technology Definition Team .................................................................. 3 Executive Summary ................................................................................................................................. 4 1.0 Introduction ........................................................................................................................................ 6 1.1 Heliophysical Explorers (HELEX): Solar Orbiter and the Inner Heliospheric Sentinels ........ 7 2.0 Science Objectives .............................................................................................................................. 8 2.1 What are the origins of the solar wind streams and the heliospheric magnetic field? ............. 9 2.2 What are the sources, acceleration mechanisms, and transport processes of solar energetic particles? ........................................................................................................................................ 13 2.3 How do coronal mass ejections evolve in the inner heliosphere? ............................................. 16 2.4 High-latitude-phase science ......................................................................................................... 19 3.0 Measurement Requirements and Science Implementation ........................................................ 20 -
Pos(MULTIF15)001 the Impact of Space Exper- (Giovannelli & Sabau-Graziati, 2004) † ∗ [email protected] [email protected] Speaker
Multifrequency Astrophysics: An Updated Review PoS(MULTIF15)001 Franco Giovannelli∗† INAF - Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere, 100, 00133 Roma, Italy E-mail: [email protected] Lola Sabau-Graziati INTA- Dpt. Cargas Utiles y Ciencias del Espacio, C/ra de Ajalvir, Km 4 - E28850 Torrejón de Ardoz, Madrid, Spain E-mail: [email protected] In this paper – a short updated version of our review paper about "The impact of space exper- iments on our knowledge of the physics of the Universe (Giovannelli & Sabau-Graziati, 2004) (GSG2004) and subsequent updating (Giovannelli & Sabau-Graziati, 2012a, 2014a) – we will briefly discuss old and new results obtained in astrophysics, that marked substantially the re- search in this field. Thanks to the results, chosen by us following our knowledge and feelings, we will go along different stages of the evolution of our Universe discussing briefly several examples of results that are the pillars carrying the Bridge between the Big Bang and Biology. We will remark the importance of the joint venture of ‘active physics experiments’ and ‘passive physics experiments’ ground– and space–based either big either small in size that, with their results, are directed towards the knowledge of the physics of our universe. New generation exper- iments open up new prospects for improving our knowledge of the aforementioned main pillars. XI Multifrequency Behaviour of High Energy Cosmic Sources Workshop 25-30 May 2015 Palermo, Italy ∗Speaker. †A footnote may follow. ⃝c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). -
Alerts from High-Energy Observatories (From Space)
ALERTS FROM HIGH-ENERGY OBSERVATORIES (FROM SPACE) DIEGO GÖTZ CEA SACLAY - IRFU/DÉPARTEMENT D’ASTROPHYSIQUE THE CONTEXT H. Ashkar talk Ashkar H. Diego Götz - High Energy Alerts from Space — TS2020 - 25/09/2019 WIDE FIELD HARD X-RAY IMAGING • Above 10 keV it is very difficult to perform direct imaging with mirrors (the maximum energy is proportional to the focal length) • Coded mask (indirect) imaging is a solution (INTEGRAL/IBIS and SPI, BeppoSAX/WFC, Swift/BAT, GRANAT/SIGMA, etc.) often coupled to pixellated CdTe detectors • Each pixel records background and possibly source(s) photons • Image deconvolution techniques are required to reconstruct the sky • Wide field of view → all-sky monitoring of the transient sky, optimal for Gamma-Ray Burst searches (BAT on board Swift or IBIS on board INTEGRAL) • State of the art PSF ~ 12 arc min @ 100 keV • It is difficult to image diffuse sources, and its sensitivity limited (mCrab) due to the high background • Can be used up to a few MeV (SPI on board INTEGRAL) • Diego Götz - High Energy Alerts from Space — TS2020 - 25/09/2019 SWIFT RESULTS Localization of SGRBs The light curve zoo Ultra-long GRBs • Many, many other results, e.g. high-z GRBs, long GRBs without SN, low-z with SN • Swift has observed over 1000 GRBs and is still finding exceptional objects Diego Götz - High Energy Alerts from Space — TS2020 - 25/09/2019 SWIFT EVOLUTION (COURTESY P. O’BRIEN) Early on: all GRBs followed until too faint Ever increasing no. of TOO requests Now: GRBs followed usually for only for 1-3 days (NuStar coordinated in green) Much more time now spent on GI/TOOs Diego Götz - High Energy Alerts from Space — TS2020 - 25/09/2019 SWIFT & MULTI-MESSENGER ALERTS (COURTESY P. -
X-Ray Broad-Band Study of the Symbiotic X-Ray Binary 4U 1954+ 31
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) X–ray broad-band study of the symbiotic X–ray binary 4U 1954+31 N. Masetti1, E. Rigon2, E. Maiorano1,3, G. Cusumano4, E. Palazzi1, M. Orlandini1, L. Amati1 and F. Frontera1,3 1 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Via Gobetti 101, I-40129 Bologna, Italy (formerly IASF/CNR, Bologna) 2 Dipartimento di Fisica, Universit`adi Bologna, Via Irnerio 48, I-40126 Bologna, Italy 3 Dipartimento di Fisica, Universit`adi Ferrara, via Saragat 1, I-44100 Ferrara, Italy 4 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy (formerly IASF/CNR, Palermo) Received 6 October 2006; Accepted 14 November 2006 Abstract. We present results of several pointed X–ray broad band observations of the ‘symbiotic X–ray binary’ 4U 1954+31 performed with the satellites BeppoSAX, EXOSAT, ROSAT, RXTE and Swift between October 1983 and April 2006. We also studied the RXTE ASM data over a period of more than 10 years, from January 1996 to October 2006. Light curves of all pointed observations show an erratic behaviour with sudden increases in the source emission on timescales variable from hundreds to thousands of seconds. There are no indications of changes in the source spectral hardness, with the possible exception of the RXTE pointed observation. Timing analysis does not reveal the presence of coherent pulsations or periodicities either in the pointed observations in the range from 2 ms to 2000 s or in the long-term RXTE ASM light curve on timescales from days to years. -
Particle Background for Equatorial Low Earth Orbit (ELEO)
Particle background for Equatorial Low Earth Orbit (ELEO) Yashvi Sharma August 11, 2020 1 Introduction An important consideration for X-ray and Gamma ray missions is the particle background environ- ment. Focusing telescopes with lower effective area are only background limited at the fainter end of sensitivity. On the other hand, collimators and concentrators have larger effective area hence there primary concern is to both limit and model the background to get better sensitivity. It can be achieved through employing shielding systems and careful modeling of radiation environment (see figure ?? for state of the art simulation efforts) and choosing the orbit in accordance with science objectives and background limitations. Low Earth Orbit (LEO) is the most commonly used orbit for imaging satellites, communication satellites (network) and many different space telescopes (Hubble, AGILE, ASTROSAT, etc.) and space stations (ISS, Tiangong-2). It is defined to be less than 2000 km in altitude or with less than 128 minutes period and with eccentricity within 0.25. Thus, it requires less energy for satellite placement (although does require frequent orbital corrections due to orbital decay), provides good bandwidth and low latency for communication (although the window for communication is short due to smaller orbits) and is more easily accessible for servicing of space stations and satellites. Moreover, it is between the Earth's upper atmosphere and inner Van Allen radiation belt to keep the high energy particle background to the minimum. Figure 1: Simulated background environment using MGGPOD 1 2 Particle Background for ELEO missions The particle background for an unshielded detector in LEO is primarily made up of cosmic diffuse radiation (below 150 keV) and albedo glow of Earth from interaction of cosmic rays with atmosphere (above 150 keV).