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GRB 180418A: a Possibly Short Gamma-Ray Burst with a Wide-Angle Outflow in a Faint Host Galaxy
GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy Item Type Article; text Authors Rouco Escorial, A.; Fong, W.; Veres, P.; Laskar, T.; Lien, A.; Paterson, K.; Lally, M.; Blanchard, P.K.; Nugent, A.E.; Tanvir, N.R.; Cornish, D.; Berger, E.; Burns, E.; Cenko, S.B.; Cobb, B.E.; Cucchiara, A.; Goldstein, A.; Margutti, R.; Metzger, B.D.; Milne, P.; Levan, A.; Nicholl, M.; Smith, N. Citation Rouco Escorial, A., Fong, W., Veres, P., Laskar, T., Lien, A., Paterson, K., Lally, M., Blanchard, P. K., Nugent, A. E., Tanvir, N. R., Cornish, D., Berger, E., Burns, E., Cenko, S. B., Cobb, B. E., Cucchiara, A., Goldstein, A., Margutti, R., Metzger, B. D., … Smith, N. (2021). GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy. Astrophysical Journal, 912(2). DOI 10.3847/1538-4357/abee85 Publisher IOP Publishing Ltd Journal Astrophysical Journal Rights © 2021. The American Astronomical Society. All rights reserved. Download date 28/09/2021 16:20:20 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/660724 The Astrophysical Journal, 912:95 (19pp), 2021 May 10 https://doi.org/10.3847/1538-4357/abee85 © 2021. The American Astronomical Society. All rights reserved. GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy A. Rouco Escorial1, W. Fong1 , P. Veres2 , T. Laskar3 , A. Lien4,5, K. Paterson1 , M. Lally1 , P. K. -
GRIPS-Gamma-Ray Imaging, Polarimetry and Spectroscopy
Experimental Astronomy manuscript No. (will be inserted by the editor) GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy www.grips-mission.eu? Jochen Greiner · Karl Mannheim · Felix Aharonian · Marco Ajello · Lajos G. Balasz · Guido Barbiellini · Ronaldo Bellazzini · Shawn Bishop · Gennady S. Bisnovatij-Kogan · Steven Boggs · Andrej Bykov · Guido DiCocco · Roland Diehl · Dominik Els¨asser · Suzanne Foley · Claes Fransson · Neil Gehrels · Lorraine Hanlon · Dieter Hartmann · Wim Hermsen · Wolfgang Hillebrandt · Rene Hudec · Anatoli Iyudin · Jordi Jose · Matthias Kadler · Gottfried Kanbach · Wlodek Klamra · J¨urgenKiener · Sylvio Klose · Ingo Kreykenbohm · Lucien M. Kuiper · Nikos Kylafis · Claudio Labanti · Karlheinz Langanke · Norbert Langer · Stefan Larsson · Bruno Leibundgut · Uwe Laux · Francesco Longo · Kei'ichi Maeda · Radoslaw Marcinkowski · Martino Marisaldi · Brian McBreen · Sheila McBreen · Attila Meszaros · Ken'ichi Nomoto · Mark Pearce · Asaf Peer · Elena Pian · Nikolas Prantzos · Georg Raffelt · Olaf Reimer · Wolfgang Rhode · Felix Ryde · Christian Schmidt · Joe Silk · Boris M. Shustov · Andrew Strong · Nial Tanvir · Friedrich-Karl Thielemann · Omar Tibolla · David Tierney · Joachim Tr¨umper · Dmitry A. Varshalovich · J¨orn Wilms · Grzegorz Wrochna · Andrzej Zdziarski · Andreas Zoglauer Received: 21 April 2011 / Accepted: 2011 ? See this Web-site for the author's affiliations. Jochen Greiner Karl Mannheim MPI f¨urextraterrestrische Physik Inst. f. Theor. Physik & Astrophysik, Univ. W¨urzburg arXiv:1105.1265v1 [astro-ph.HE] 6 May 2011 85740 Garching, Germany 97074 W¨urzburg,Germany Tel.: +49-89-30000-3847 Tel.: +49-931-318-500 E-mail: [email protected] E-mail: [email protected] 2 Abstract We propose to perform a continuously scanning all-sky survey from 200 keV to 80 MeV achieving a sensitivity which is better by a factor of 40 or more compared to the previous missions in this energy range (COMPTEL, INTEGRAL; see Fig. -
REVIEW ARTICLE the NASA Spitzer Space Telescope
REVIEW OF SCIENTIFIC INSTRUMENTS 78, 011302 ͑2007͒ REVIEW ARTICLE The NASA Spitzer Space Telescope ͒ R. D. Gehrza Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S.E., University of Minnesota, Minneapolis, Minnesota 55455 ͒ T. L. Roelligb NASA Ames Research Center, MS 245-6, Moffett Field, California 94035-1000 ͒ M. W. Wernerc Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͒ G. G. Faziod Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 ͒ J. R. Houcke Astronomy Department, Cornell University, Ithaca, New York 14853-6801 ͒ F. J. Lowf Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ G. H. Riekeg Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ ͒ B. T. Soiferh and D. A. Levinei Spitzer Science Center, MC 220-6, California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125 ͒ E. A. Romanaj Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͑Received 2 June 2006; accepted 17 September 2006; published online 30 January 2007͒ The National Aeronautics and Space Administration’s Spitzer Space Telescope ͑formerly the Space Infrared Telescope Facility͒ is the fourth and final facility in the Great Observatories Program, joining Hubble Space Telescope ͑1990͒, the Compton Gamma-Ray Observatory ͑1991–2000͒, and the Chandra X-Ray Observatory ͑1999͒. Spitzer, with a sensitivity that is almost three orders of magnitude greater than that of any previous ground-based and space-based infrared observatory, is expected to revolutionize our understanding of the creation of the universe, the formation and evolution of primitive galaxies, the origin of stars and planets, and the chemical evolution of the universe. -
Wide-Field Infrared Survey Explorer Launch Press
PRess KIT/DECEMBER 2009 Wide-field Infrared Survey Explorer Launch Contents Media Services Information ................................................................................................................. 3 Quick Facts ............................................................................................................................................. 4 Mission Overview .................................................................................................................................. 5 Why Infrared? ....................................................................................................................................... 10 Science Goals and Objectives ......................................................................................................... 12 Spacecraft ............................................................................................................................................. 16 Science Instrument ............................................................................................................................. 19 Infrared Missions: Past and Present ............................................................................................... 23 NASA’s Explorer Program ................................................................................................................. 25 Program/Project Management .......................................................................................................... 27 Media Contacts J.D. Harrington -
NASA's Goddard Space Flight Center Laboratory for High Energy
1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U. -
Page 1 of 5 Second Stand Alone Missions of Opportunity
Second Stand Alone Missions Of Opportunity Notice (SALMON-2) Program Element Appendix (PEA) Q Heliophysics Explorers Mission of Opportunity Program Library Step-2 Change Log The current version of this document may be found in the Program Library, at https://explorers.larc.nasa.gov/HPSMEX/MO/programlibrary.html, by selecting the “View Step-2 Change Log” link. Updates to the Program Library are represented in reverse-chronological order. Latest revisions are indicated via highlighting. May 4, 2018: CFR-2014-title2-vol1-sec200-466.pdf posted to NASA and Federal Documents item “2 CFR 200.466, “Scholarships and Student Aid Costs” (NOTE: Step-2 addition.)” April 11, 2018: 2017_LSP_Advisory_Services_Overview_for_2016_Heliophysics_Explorer.pdf reposted as an update to Program Specific Documents item “29. 2017 LSP Advisory Services Overview (NOTE: Step-2 addition.)”. Typo corrected on title slide. March 9, 2018: tailored-Class-D-guidance-for-AOs-updated-redact.pdf (dated 12 February 2018) posted as an update to Program Specific Documents item “34. Guidance on the Application of NASA Science Mission Directorate (SMD) Class-D Tailoring/Streamlining Decision Memorandum (signed 07 December 2017) to Currently Active Explorers Program AO Competitions (NOTE: Step-2 addition.)” March 5, 2018: Explorers-Program-Plan-Signed-2014.09.09_Redacted.pdf posted to Program Specific Documents item “32. Explorers Program Plan (NOTE: Step-2 addition.)” March 5, 2018: tailored-Class-D-guidance-for-AOs-redact.pdf (dated 12 February 2018) posted as Program Specific Documents item “31. Guidance on the Application of NASA Science Mission Directorate (SMD) Class-D Tailoring/Streamlining Decision Memorandum (signed [7] December 2017) to Currently Active Explorers Program AO Competitions (NOTE: Step-2 addition.)” March 5, 2018: SMD-Class-D-Policy-redact.pdf (dated 17 December 2017) posted as Program Specific Documents item “30. -
The High Energy Astrophysics Division Newsletter
SPRING 2017 The High Energy Astrophysics Division Newsletter In this Issue: View from the Chair — special advertising section — hidden black holes revealed, and others — second running — finding a path through spacetime — announcing mysteries under the ice — performance enhancements for Chandra — milestones for XMM — the hunt continues for Swift — ULXNS — on the trail of the wild neutrino with INTEGRAL — searching at home with Fermi — energetic electrons seen at the ISS — news from the cosmos — of scientific interest — a Universe of learning — NICER launch prep — SRG progress — the wisdom of Athena — the slant on IXPE — the XARM — building CTA — all-seeing Lynx — in memoriam From the Chair for the discovery of merging black hole binaries, and for beginning the new era of gravitational-wave astronomy. CHRIS REYNOLDS (U. MD) Prof. González will give the Rossi Prize Lecture at the All systems are go for our 16th Divisional meeting to 231st AAS meeting to be held at National Harbor, MD be held in Sun Valley, Idaho, 20-24 August 2017! Regis- in January 2018. Please join me in congratulating all of tration and abstract submission is now open and we’re this year’s HEAD prize winners. looking forward to an exciting scientific program cover- ing all aspects of high-energy astrophysics, kicked off by The past few months has been eventful in the world a total solar eclipse! of high-energy astrophysics missions. NICER and ISS- CREAM are at the Kennedy Space Center and ready for One of the most important aspects of these meet- launch to the International Space Station. Further in the ings is the chance to honor a new batch of HEAD future, NASA has formally selected the Imaging X-ray Po- prize winners. -
ASTR 2310: Chapter 6
ASTR 2310: Chapter 6 Astronomical Detection of Light The Telescope as a Camera Refraction and Reflection Telescopes Quality of Images Astronomical Instruments and Detectors Observations and Photon Counting Other Wavelengths Modern Telescopes Refracting / Reflecting Telescopes 0 Refracting Telescope: Lens focuses light onto the focal plane Focal length Reflecting Telescope: Concave Mirror focuses light onto the focal Focal length plane Almost all modern telescopes are reflecting telescopes. Secondary Optics 0 In reflecting telescopes: Secondary mirror, to re- direct light path towards back or side of incoming light path. Eyepiece: To view and enlarge the small image produced in the focal plane of the primary optics. Disadvantages of 0 Refracting Telescopes • Chromatic aberration: Different wavelengths are focused at different focal lengths (prism effect). Can be corrected, but not eliminated by second lens out of different material. • Difficult and expensive to produce: All surfaces must be perfectly shaped; glass must be flawless; lens can only be supported at the edges. The Best Location for a Telescope0 Far away from civilization – to avoid light pollution The Best Location for a Telescope (II)0 Paranal Observatory (ESO), Chile http://en.wikipedia.org/wiki/Paranal_Observatory On high mountain-tops – to avoid atmospheric turbulence ( seeing) and other weather effects The Powers of a Telescope: 0 Size does matter! 1. Light-gathering power: Depends on the surface area A of the primary lens / D mirror, proportional to diameter squared: A = pi (D/2)2 The Powers of a Telescope (II) 0 2. Resolving power: Wave nature of light => The telescope aperture produces fringe rings that set a limit to the resolution of the telescope. -
Astrophysics
National Aeronautics and Space Administration Astrophysics Committee on NASA Science Paul Hertz Mission Extensions Director, Astrophysics Division NRC Keck Center Science Mission Directorate Washington DC @PHertzNASA February 1-2, 2016 Why Astrophysics? Astrophysics is humankind’s scientific endeavor to understand the universe and our place in it. 1. How did our universe 2. How did galaxies, stars, 3. Are We Alone? begin and evolve? and planets come to be? These national strategic drivers are enduring 1972 1982 1991 2001 2010 2 Astrophysics Driving Documents http://science.nasa.gov/astrophysics/documents 3 Astrophysics Programs Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program 1. How did our universe 2. How did galaxies, stars, 3. Are We Alone? begin and evolve? and planets come to be? Astrophysics Explorers Program Astrophysics Research Program James Webb Space Telescope Program (managed outside of Astrophysics Division until commissioning) 4 Astrophysics Programs and Missions Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program Chandra Hubble Spitzer Kepler/K2 XMM-Newton (ESA) Herschel (ESA) WFIRST Fermi SOFIA Planck (ESA) LISA Pathfinder (ESA) Astrophysics Explorers Program Euclid (ESA) NuSTAR Swift Suzaku (JAXA) Athena (ESA) ASTRO-H (JAXA) NICER TESS L3 GW Obs (ESA) 3 SMEX and 2 MO in Phase A James Webb Space Telescope Program: Webb 5 Astrophysics Programs and Missions Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program Missions in extended phase Chandra Hubble Spitzer Kepler/K2 XMM-Newton (ESA) Herschel (ESA) WFIRST Fermi SOFIA Planck (ESA) LISA Pathfinder (ESA) Astrophysics Explorers Program Euclid (ESA) NuSTAR Swift Suzaku (JAXA) Athena (ESA) ASTRO-H (JAXA) NICER TESS L3 GW Obs (ESA) 3 SMEX and 2 MO in Phase A James Webb Space Telescope Program: Webb 6 Astrophysics Mission Portfolio • NASA Astrophysics seeks to advance NASA’s strategic objectives in astrophysics as well as the science priorities of the Decadal Survey in Astronomy and Astrophysics. -
Gehresl WFIRST AAS V2.Pptx
WFIRST Mission Status Neil Gehrels WFIRST Project Scientist NASA/GSFC AAS WFIRST Session January 5, 2016 Discovery Science • WFIRST was highest ranked large space mission in 2010 Decadal Survey • Use of 2.4m telescope enables - Hubble quality imaging over 100x more sky - Imaging of exoplanets with 10-9 contrast with a coronagraph Dark Energy Exoplanets Astrophysics microlensing M63 HST WFIRST coronagraph 2 WFIRST Surveys • Multiple surveys: – High-Latitude Survey • Imaging, spectroscopy, supernova monitoring – Repeated galactic bulge observations for microlensing – 25% Guest Observer Program – Coronagraph observations • Flexibility to choose optimal approach Near Infrared Surveys 3 WFIRST Instruments Wide-Field Instrument • Imaging & spectroscopy over 1000s of sq. deg. • Monitoring of SN and microlensing fields • 0.7-2.0 mm (imaging), 1.35-1.89 mm (spec.) • 0.28 deg2 FoV (100x JWST FoV) • 18 H4RG detectors (288 Mpixels) • 6 filter imaging, grism + IFU spectroscopy Coronagraph • Image and spectra of exoplanets from super-Earths to giants • Images of debris disks • 430 – 970 nm (imaging) & 600 – 970 nm (IFS spec.) • Final contrast of 10-9 or better • Exoplanet images from 0.1 to 1.0 arcsec 4 Wide Field Instrument Layout M3$Assembly$ Radiator' IFU$ Cryocooler' M3' Outer'Enclosure' Op#cal' F1$Assembly$ Bench' IFU' FPA$ F2$Assembly$ Element$Wheel$Assembly$(EWA)$ Latches'(3)' Radia#on'Shield' FPA' Fold'Flats'(2)' Element'Wheel' 5 Coronagraph Instrument Layout • Primary Architecture: Occulting Mask + Shaped Pupil • SP and HL masks share very -
UV and Infrared Astronomy
Why Put a Telescope In Space? • Access to light that does not penetrate the atmosphere • No seeing. A telescope can reach the diffraction limit: 1.22 l/D radians Astronomy in Space. I. UV Astronomy Ultraviolet Astronomy 912-3650 Å (Lyman Limit to Balmer jump) • Continuua of hot stars (spectral types O,B,A) • H I Lyman lines (1-n transitions) • Resonance lines of Li-like ions C IV, N V, O VI • H2 Lyman and Werner bands Normal incidence optics • Special UV-reflective coatings The Far Ultraviolet 912 to 1150 Å • Defined by Lyman limit, MgF cutoff at 1150 Å • LiF + Al reflects longward of 1050 Å • SiC reflects at shorter wavelengths The Astronomy Quarterly, Vol. 7, pp. 131-142, 1990 0364-9229f90 $3.00+.00 Printed in the USA. All rights reserved. Copyright (c) 1990 Pergamon Press plc ASTRONOMICAL ADVANTAGES History OFAN • 9/1/1946: Lyman Spitzer EXTRA-TERRESTRIAL OBSERVATORY proposed a Space Telescope in LYMAN SPITZER, Jr. ’ a Report to project Rand This study points out, in a very preliminary way, the results that might be expected from astronomical measurements made with a satellite • 1966: Spitzer (Princeton) vehicle. The discussion is divided into three parts, corresponding to three different assumptions concerning the amount of instrumentation provided. chairs NASA Ad Hoc In the first section it is assumed that no telescope is provided; in the second a 10-&h reflector is assumed; in the third section some of the results Committee on the "Scientific obtainable with a large reflecting telescope, many feet in diameter, and revolving about the earth above the terrestrial atmosphere, are briefly Uses of the Large Space sketched. -
The Spitzer Space Telescope and the IR Astronomy Imaging Chain
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different from optical astronomy sources) 2) Object (usually the same as the source in astronomy) 3) Collector (Spitzer Space Telescope) 4) Sensor (IR detector) 5) Processing 6) Display 7) Analysis 8) Storage ... but steps 3) and 4) are a bit more difficult! Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 2/38 The infrared imaging chain Longer wavelength – need a bigger telescope to get the same resolution or put up with lower resolution Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 3/38 Emission of IR radiation Warm objects emit lots of thermal infrared as well as reflecting it Including telescopes, people, and the Earth – so collection of IR radiation with a telescope is more complicated than an optical telescope Optical image of Spitzer Space Telescope launch: brighter regions are those which reflect more light IR image of Spitzer launch: brighter regions are those which emit more heat Infrared wavelength depends on temperature of object Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 4/38 Atmospheric absorption The atmosphere blocks most infrared radiation Need a telescope in space to view the IR properly Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 5/38