DOCSLIB.ORG

Illll]Llllll]Llllllllh]Lll,,.M

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Illll]llllll]llllllllH]lll,,.m PB97-167001 InfOrmatiod Is Our busk_is. RECOMMENDEDPRIORITIES FOR NASA'S GAMMARAY ASTRONOMYPROGRAM1996-2010 (U.S.) NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON, DC APR 97 U.$. bEPAR'I_MENT oF COMMERCi_ National Technical Information Service • 111_ I# • 41 °" _1 _ 4 J . • RECOMMENDEDPRIORITIESFORNASKS GAMMARAYASTRONOMYPROGRAM 1996-2010 ReporloftheGammaRayAstronomyProgramWorkingGroup April,1997 RECOMMENDEDPRIORITIESFORNASA'S GAMMARAYASTRONOMYPROGRAM 1996-2010 ReportoftheGammaRayAstronomyProgramWorkingGroup April,_997 PROTECTED UND_:R INTf:RNATiONAL COPYRIGHT ALL RIQHT_ RESERVED° NATIONAL TECHNICAL INFORMATION SERVICE U.$, DEPARTMENT OF COMMERCE BIBLIOGRAPHIC INFORMATION PB97-167001 Report Nos: Title: Recommended Priorities for NASA'S GammaRay Astronomy Program 1996-2010. Date: Apr 97 Performin 9 Organization: National Aeronautics and Space Administration, Washington, UC. Supplemental Notes: Color illustrations reproduced in black and white. TIS Field/Group Codes: 54C (Astrophysics). 70E (Research Program Administration & ecnnology Iranster) Price: PC AO5/MF AOI Availability: This product may be ordered from NTIS by phone at (703)487-4650" by fax at (/u3)Jz1-8547: and by email at 'orders@ntis,fedworld.gov'. NTIS is located at 5285 Port Royal Road, Springfield, VA, 22161, USA. Number of Pages: 56p Ke_lwords" *NASA programs. *Gamma ray astronomy, *Program management. *Long range pjannlng Research programs, Research management, Pmorities, Recommendatlons, Mission planning Abstract: It has assessed the state of the field including current missions and approvea future missions, the critical scientific problems o_en today, the promising technologies for the future, the mission priorities for the Tu_ure. and _ne neeas Tot data analysis and theory. This report presents a summary of the GRAPWGfindings and gives detailed recommendations. n 1995, NASA formed the Gamma-Ray Astronomy Program Working Group (GRAPWG) to formulate recommendations for future direc- tions in NAS_s gamma-ray astronomy program. The energy range consid- ered in this study extends from hard x-rays (>_ 15 keV) through TeV gamma rays. The mandate of the working group is to recommend a road map to the future for use as an input to th_ next NASA strategic plan, cur- rently slated for 1997. The working group, whose membership is given belom; has met four times over the past 2 years. It has assessed tke state of the field including current missions and approved future missions, the crit- ical scientific problems open today the promising technologies for the future, the mission priorities for the future, and the needs for data analysis and theor): This report presents a summaD' of the GRAPWG findings and gives detailed recommendations. The acronyms used in the report are defined in Appendix A. GAMMA-RAYASTRONOMYPROGRAMWORKINGGROUPMEMBERS: Elena Aprile (Columbia) Alan Bunner (NASA) [Ex-Officio (NASA Headquarters)] Neil Gehrels (GSFC) [Co-Chair] Jonathan Grindlay (Harvard) Gerald Fishman (MSFC) W. Neil Johnson (NRL) Kevin Hurley (UCB/SSL) Steve Kahn (Columbia) Richard Lingenfeher (UCSD) Peter Michelson (Stanford) Thomas Prince (Caltech) [Co-Chair] Roger Romani (Stanford) James Ryan (UNH) Bonnard Teegarden (GSFC) David Thompson (GSFC) Trevor Weekes (Harvard/Smithsonian) Stanford Woosley (UCSC) Precedingpageblank Recommended Ptioritfc._for NASA's Gal,ma.Ra._ Astro_om._ PIog_am iiJ Iv _:_+,* ..'.. _.. _ ..4_-i - ..,. -;_.,; -.. ; .:.,_.._+ . , _'_ ..+ .. -. : _._.. • :...:._- ,.. • ._ _,', . ... ii:."@ i newresu,,fro,,,the ComptonGammaRayObse a,o " j" i_JJlJi'"! J ''"/i_"_i_=J: W ¥ (CGRO), the Rossi X-ray Timing Explorer (RXTE), and GRANAT, hard X-ray and gamma-ray astronomy are in a period of discov- er" and vigor unparalleled in their history- Tr,_ CGRO mission in particular has made fundamental contributions to und_$tanfling many classes of galactic and extragalactic objects. The CGRO discoveries of gamma-ray blazars, an isotropic distribution of gamma-ray bursts, bright black hole and neutron star transients, sites of galactic nucleosymhesis, and a large class of unidentified high energy sources have inlrigaed astronomers and the public alike. These discoveries ha_e prompted a wide range of correlat- ed observations by X-ray satellites and ground-based radio, IR, and optical observatories, adding to our rapidly expanding knowledge of the nature of high-energy emission. We now have the beginnings of a better understand- ing of the astrophysics of gamma-ray sources, and this i;n turn has raised . fundamental new questions about the origin and evolution of high-energy objects and about the nonthermal astrophysical processes that occur in them. Looking ahead to the next decade, further discoveries in hard X-ray and ._-.. gamma-ray astronomy are anticipated with further CGRO and RXTE obser- ¢. vations and with the ESA INTEGRAL mission (launch +2001). However, there are currently no major missions being planned beyond INTEGRAL and none being planned at all by NASA. Of particular concern is the high- energy regime (100 Me\: - 100 GeV), where obseta-ations will soon come to a virtual halt in the next 2 years as the EGRET instrument on CGRO runs out of spark-chamber gas. Also of concern is the present lack of plans for missions that would l) significantly improve on the BATSE capabilities to study gamma-ray bursts as well as conduct a full-sky survey and monitor transient source 2) follow-on the first exploration of the MeV band by COMPTEL with much better sensitivity, and 3) continue the important studies of nucleosynthesis begun by balloon instruments, OSSE, and COMPTEL. From a scientific standpoint, there is an urgent need for new observational missions. From a technical standpoint, the timing is excellent since powerful new detector and imaging technologies are in hand that promise major steps in observational capabilities. With this in mind, the GRAPWG recommends the following program in hard X-ray and gamma-ray astronomy: Precedingpageblank Rccc,,,,,,tc,,dcdP,io,llIes fo, X.-_,S..'t_Ga,nn,c,.Ra3. Astro,,o,,,) P,og,a,,, v INTERMEDIATEMISSIONS($75M- _00M) expected two orders of magnitude improve- The HIGHEST PRIORITY recommendation of merit in sensitivity compare to RXTE would the GRAPWG is: address questions such as the nature of • A next-generation 10 Mev to I00 GeV accretion onto compact objects in galactic sources. A new multilayer mirror technology gamma-ray mission such as GLAST. One to can extend the focusing range to -I00 keg: two orders of magnitude improvement in The HTXS concept includes a focusing hard sensitivity compared to EGRET are expected X-ray telescope that extends up to 50 keV. resulting in breakthroughs in our under- • A next-generation nuclear line and MeV con- standing of particle acceleration and nonther- tinuum mission. A major step forward com- real processes in AGN and galactic sources. pared to INTEGRAL in both sensiuvity and The GRAPWG identified two other missions as energy range would allow detailed studies of very high priority for initiation within the next sites of nucleosynthesis in the galaxy and of decade. These programs would serve pressing sci- nonthermal sources in the universe. The entific needs and represent areas where prompt GRAPWG views this mission as a follow-on support for technology development and mission to INTEGILhL. study' promises great gains in the capabilities and efficiency of future missions. MIDEXANDSMEXMISSIONS • A focusing hard X-ray telescope. The Future MIDEX and SMEX missions are crucial for NASKs gamma-ray and hard X-ray astronomy program. The two highest priorities for near-term KEYQUESTIONSIN HARDX-RAYAhD SMEX and MIDEX missions are (of equal priority): GAMMA.RAYASTRONOMY • A gamma-ray burst localization mission. • What is the origin and nature of gamma- Such a mission would address the question of ray bursts? the origin of gamma-ray bursts. Missions • What are the physical conditions and with coding apertures or an a, rat of small processes near accreting black holes and telescopes would fill this need. Searches neutron stars? could also be made for a halo population of • How does matter behave in extreme con- burst sources around M31 to test galactic ditions like those in neutron stars, super- halo models. Example mission concepts are BASIS, ETA, and BLAST. nova explosions and active galactic nuclei? • A hard X-ray all-sky survey and monitor mis- sion such as EXIST. More than two orders of . How do astrophysical accretion processes work and what are their instabilities, magnitude improvement over the HEAO-1 periodicities and modes? survey could be obtained in the 10 - 200 keV range. A significant fraction of the entire sky • What is the nature of the jets emanating from galactic black holes and AGN and could be scanned every day ','ortransient sources. how are the particles accelerated? • What is the origin of the diffuse gamma- HETE ray background? The loss of HETE is a maj _r setback to the • What is the nature of the unidentified study of gamma-ray bursts. The objectives of that high energy gamma-ray sources? mission are still compelling: rapidly obtained pre- • Where are the sites of nucleosynthesis? cise positions are invaluable for multiwavelength • How do supernovae work? What are the counterpart searches, The HETE spacecraft can be progenitors and explosion mechanisms? rebuilt and reflown relatively quickly and inexpen- What has been the rate in the last several sively. hundred years? • We endorse this initiative and further recom- • What and where ate
Recommended publications
  • Parallel Sessions

    Parallel Sessions

    Identification of Dark Matter July 23-27, 2012 9th International Conference Chicago, IL http://kicp-workshops.uchicago.edu/IDM2012/ PARALLEL SESSIONS http://kicp.uchicago.edu/ http://www.nsf.gov/ http://www.uchicago.edu/ http://www.fnal.gov/ International Advisory Committee Daniel Akerib Elena Aprile Rita Bernabei Case Western Reserve University, Columbia University, USA Universita degli Studi di Roma, Italy Cleveland, USA Gianfranco Bertone Joakim Edsjo Katherine Freese University of Amsterdam Oskar Klein Centre / Stockholm University of Michigan, USA University Richard Gaitskell Gilles Gerbier Anne Green Brown University, USA IRFU/ CEA Saclay, France University of Nottingham, UK Karsten Jedamzik Xiangdong Ji Lawrence Krauss Universite de Montpellier, France University of Maryland, USA Arizona State University, USA Vitaly Kudryavtsev Reina Maruyama Leszek Roszkowski University of Sheffield University of Wisconsin-Madison University of Sheffield, UK Bernard Sadoulet Pierre Salati Daniel Santos University of California, Berkeley, USA University of California, Berkeley, USA LPSC/UJF/CNRS Pierre Sikivie Daniel Snowden-Ifft Neil Spooner University of Florida, USA Occidental College University of Sheffield, UK Max Tegmark Karl van Bibber Kavli Institute for Astrophysics & Space Naval Postgraduate School Monterey, Research at MIT, USA USA Local Organizing Committee Daniel Bauer Matthew Buckley Juan Collar Fermi National Accelerator Laboratory Fermi National Accelerator Laboratory Kavli Institute for Cosmological Physics Scott Dodelson Aimee
  • AAS Worldwide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data

    AAS Worldwide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data

    AAS WorldWide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Rosenfield, Philip, Jonathan Fay, Ronald K Gilchrist, Chenzhou Cui, A. David Weigel, Thomas Robitaille, Oderah Justin Otor, and Alyssa Goodman. 2018. AAS WorldWide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data. The Astrophysical Journal: Supplement Series 236, no. 1. Published Version https://iopscience-iop-org.ezp-prod1.hul.harvard.edu/ article/10.3847/1538-4365/aab776 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41504669 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP Draft version January 30, 2018 Typeset using LATEX twocolumn style in AASTeX62 AAS WorldWide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data Philip Rosenfield,1 Jonathan Fay,1 Ronald K Gilchrist,1 Chenzhou Cui,2 A. David Weigel,3 Thomas Robitaille,4 Oderah Justin Otor,1 and Alyssa Goodman5 1American Astronomical Society 1667 K St NW Suite 800 Washington, DC 20006, USA 2National Astronomical Observatories, Chinese Academy of Sciences 20A Datun Road, Chaoyang District Beijing, 100012, China 3Christenberry Planetarium, Samford University 800 Lakeshore Drive Birmingham, AL 35229, USA 4Aperio Software Ltd. Headingley Enterprise and Arts Centre, Bennett Road Leeds, LS6 3HN, United Kingdom 5Harvard Smithsonian Center for Astrophysics 60 Garden St.
  • Space Astronomy in the 90S

    Space Astronomy in the 90S

    Space Astronomy in the 90s Jonathan McDowell April 26, 1995 1 Why Space Astronomy? • SHARPER PICTURES (Spatial Resolution) The Earth’s atmosphere messes up the light coming in (stars twinkle, etc). • TECHNICOLOR (X-ray, infrared, etc) The atmosphere also absorbs light of different wavelengths (col- ors) outside the visible range. X-ray astronomy is impossible from the Earth’s surface. 2 What are the differences between satellite instruments? • Focussing optics or bare detectors • Wavelength or energy range - IR, UV, etc. Different technology used for different wavebands. • Spatial Resolution (how sharp a picture?) • Spatial Field of View (how large a piece of sky?) • Spectral Resolution (can it tell photons of different energies apart?) • Spectral Field of View (bandwidth) • Sensitivity • Pointing Accuracy • Lifetime • Orbit (hence operating efficiency, background, etc.) • Scan or Point What are the differences between satellites? • Spinning or 3-axis pointing (older satellites spun around a fixed axis, precession let them eventually see different parts of the sky) • Fixed or movable solar arrays (fixed arrays mean the spacecraft has to point near the plane perpendicular to the solar-satellite vector) 3 • Low or high orbit (low orbit has higher radiation, atmospheric drag, and more Earth occultation; high orbit has slower preces- sion and no refurbishment opportunity) • Propulsion to raise orbit? • Other consumables (proportional counter gas, attitude control gas, liquid helium coolant) 4 What are the differences in operation? • PI mission vs. GO mission PI = Principal Investigator. One of the people responsible for building the satellite. Nowadays often referred to as IPIs (In- strument PIs). GO = Guest Observer. Someone who just want to use the satel- lite.
  • Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search

    Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search

    Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Advisor: Professor Elena Aprile Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved ABSTRACT Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni This thesis describes the research conducted for the XENON dark matter direct detection experiment. The tiny energy and small cross-section, from the interaction of dark matter particle on the target, requires a low threshold and sufficient background rejection capability of the detector. The XENON experiment uses dual phase technology to detect scintillation and ionization simultaneously from an event in liquid xenon (LXe). The distinct ratio, be- tween scintillation and ionization, for nuclear recoil and electron recoil events provides excellent background rejection potential. The XENON detector is designed to have 3D position sensitivity down to mm scale, which provides additional event information for background rejection. Started in 2002, the XENON project made steady progress in the R&D phase during the past few years. Those include developing sensitive photon detectors in LXe, improving the energy resolution and LXe purity for detect- ing very low energy events.
  • Particle Acceleration in Solar Flares What Is the Link Between Heating and Particle Acceleration?

    Particle Acceleration in Solar Flares What Is the Link Between Heating and Particle Acceleration?

    Energetic Particles in the Solar Atmosphere (X- ray diagnostics) Nicole Vilmer LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot The Sun as a Particle Accelerator: First detection of energetic protons from the Sun(1942) (related to a solar flare) First X-ray observations of solar flares (1970) Chupp et al., 1974 First observations of -ray lines from solar flares (OSO7/Prognoz 1972) Since then many more observations With e.g. RHESSI (2002-2018) And also INTEGRAL, FERMI >120000 X-ray flares observed by RHESSI (NASA/SMEX; 2002-2018) But still a limited number of gamma- ray line flares ~30 Solar flare: Sudden release of magnetic energy Heating Particle acceleration X-rays 6-8 keV 25-80 keV 195 Å 304 Å 21 aug 2002 (extreme ultraviolet) 335 Å 15 fev 2011 HXR/GR diagnostics of energetic electrons and ions SXR emission Hot Plasma (7to 8 MK ) HXR emission Bremsstrahlung from non-thermal electrons Prompt -ray lines : Deexcitation lines(C and 0) (60%) Signature of energetic ions (>2 MeV/nuc) Neutron capture line: p –p ; p-α and p-ions interactions Production of neutrons Collisional slowing down of neutrons Radiative capture on ambient H deuterium + 2.2 MeV. line RHESSI Observations X/ spectrum Thermal components T= 2 10 7 K T= 4 10 7 K Electron bremsstrahlung Ultrarelativistic -ray lines Electron (ions > 3 MeV/nuc) Bremsstrahlung (INTEGRAL) SMM/GRS PHEBUS/GRANAT FERMI/LAT observations RHESSI Pion decay radiation(ions > ~300MeV/nuc) Particle acceleration in solar flares What is the link between heating and particle acceleration? Where are the acceleration sites? What is the transport of particles from acceleration sites to X/ γ ray emission sites? What are the characteristic acceleration times? RHESSI How many energetic particles? Energy spectra? Relative abundances of energetic ions? RHESSI Which acceleration mechanisms in solar flares? Shock acceleration? Stochastic acceleration? (wave-particle interaction) Direct Electric field acceleration.
  • Centaurus a at Hard X-Rays and Gamma Rays

    Centaurus a at Hard X-Rays and Gamma Rays

    Centaurus A at Hard X-Rays and Soft Gamma-Rays Chandra 1-10 keV CGRO-COMPTEL 1 ± 30 MeV Fermi 100 MeV ± 100 GeV Helmut Steinle Max-Planck-Institut für extraterrestrische Physik Garching, Germany ----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- The Many Faces of Centaurus A ± Sydney, 28 June ± 3 July 2009; H. Steinle, MPE 1 / 35 Centaurus A at Hard X-Rays and Soft Gamma-Rays Contents · Introduction · The Spectral Energy Distribution · Properties of the existing measurements in the hard X-ray / soft Gamma-ray regime · Important satellites for this energy / frequency range · Variability of the X-ray / Gamma-ray emission · Two examples of models for the Cen A Spectral Energy Distribution · Problems (features) to be considered when using the hard X-ray / soft Gamma-ray data ± the ªsoft X-ray transient problemº ± the ªSED problemº · Outlook ----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- The Many Faces of Centaurus A ± Sydney, 28 June ± 3 July 2009; H. Steinle, MPE 2 / 35 Centaurus A at Hard X-Rays and Soft Gamma-Rays ------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- Introduction In the introductory (ªsetting the stageº) section of the
  • Dark Matter Working Group Executive Summary (Ness '02)

    Dark Matter Working Group Executive Summary (Ness '02)

    Dark Matter Working Group Executive Summary (NeSS ’02) Working Group Leaders: Rick Gaitskell, Brown; and Dick Arnowitt, Texas A&M. (Document Version 020925v21) Working Group Members: Craig Aalseth, PNL; Dan Akerib, CWRU; Elena Aprile, Columbia; Priscilla Cushman, U. Minnesota; John Ellis, CERN; Jonathan Feng, UC Irvine; Gilles Gerbier, Saclay; Alexander Kusenko, UCLA; Kirk McDonald, Princeton; Jeff Martoff, Temple; Richard Schnee, CWRU; and Nigel Smith, RAL. Introduction No currently observed particle is a suitable candidate for cold dark matter. The solution to the non baryonic dark matter problem, both in the universe as a whole, and in our own galaxy, may be resolved by physics found at the intersection of astronomy, high energy particle physics, and cosmology. The main candidates for this dark matter are relic particles generated, in great abundance, shortly after the Big Bang. Currently, there are 20 operating experiments designed to perform the direct detection of these particles being conducted at all the underground physics laboratories worldwide (bar one). One of them is sited at a US underground laboratory, although US sourced funding is made to six experiments. Existing results have put significant constraints on the allowed particle theories of dark matter, with one experiment claiming a positive observation, yet to be confirmed by other experiments. The planned dark matter experiments that were discussed at this workshop would be able to cover most of the parameter space of major theoretical proposals. The new physics required for particle dark matter is also expected to be discovered in the next round of high energy accelerator experiments (LHC, NLC). Theoretically and experimentally there is great complementarity between direct detection and accelerator programs.
  • Testing the Purity Monitor for the XENON Dark Matter Search

    Testing the Purity Monitor for the XENON Dark Matter Search

    Testing the Purity Monitor for the XENON Dark Matter Search Alison Andrews Laboratori Nazionali del Gran Sasso Columbia University REU August 4, 2006 1 Introduction Evidence for dark matter is found in many observed features of the universe. New- q GM(r) tonian gravitation predicts the rotational velocities of galaxies by v(r) = r , where mass is described by M(r) = 4π R ρ(r)r2dr. Actual measurements of the rota- tional velocities of galaxies, however, describe a distribution of mass where M(r) ∝ r. Fritz Zwicky studied this inconsistency in the Coma galaxy cluster in 1933, and he proposed the existence of a non-luminous dark matter. Over thirty years later, Vera Rubin supported Zwickys work with additional observations of galaxy rotational 1 curves. Their studies imply the existence of a halo of dark matter with ρ(r) ∝ r2 . Further evidence of dark matter is gravitational lensing. The General Theory of Relativity predicts the bending of light through areas of gravitational potential. Observations of this phenomenon show that the amount of bending around galaxy clusters corresponds to a greater amount of mass than is visible. Dark matter also helps to explain the formation and temperature distribution of the universe. A favored candidate for cold non-baryonic dark matter is the Weakly Interac- tive Massive Particle (or WIMP). Direct detection of WIMPs in experiments like XENON aim to detect the energy released from the elastic scattering of a WIMP off a terrestrial nucleus. 1 2 The XENON Dark Matter Search The XENON experiment aims to detect dark matter particles by measuring the scintillation and ionization of the nuclear recoils which result from the elastic collision of WIMPs with Xe nuclei using a dual phase (liquid/gas) xenon time projection chamber.
  • Elena Aprile Columbia University

    Elena Aprile Columbia University

    XENON1T: First Results (arXiv:1705.06655) Elena Aprile Columbia University Patras Axion-Wimp 2017 May 15-19 Thessaloniki, Greece 1 XENON World ~130 scientists from 22 institutions Laboratori Nazionali del Gran Sasso (LNGS), Italy XENON1T Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 2 Phases of the XENON program XENON10 XENON100 XENON1T / XENONnT 2005-2007 2008-2016 2013-2018 / 2019-2023 15 cm drift TPC – 25 kg 30 cm drift TPC – 161 kg 100 cm / 144 cm drift TPC - 3200 kg / ~8000 kg Achieved (2007) Achieved (2016) Projected (2018) / Projected (2023) σ -44 2 σ -45 2 σ -47 2 σ -48 2 SI = 8.8 x 10 cm SI = 1.1 x 10 cm SI = 1.6 x 10 cm / SI = 1.6 x 10 cm Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 3 The XENON1T Experiment Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 4 The XENON1T Experiment Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 4 July 2013 Uwe Oberlack LNGS SC Meeting - 29-Oct-2013 17 Aug. 2014 XENON1T Cryostat 7 XENON1T Cryostat 7 XENON1T Cryostat 7 XENON1T Cryostat 7 XENON1T Cryostat 7 Time Projection Chamber Eur. Phys. J. C 75, no. 11, 546 (2015) Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 8 Cryostat in the Water Tank Elena Aprile (Columbia) XENON1T: First Results @ Patras Axion-WIMP 2017 9 Cherenkov Muon Veto • Active shield against muons • 84 high-QE 8'' Hamamatsu R5912 PMTs • Trigger efficiency > 99.5% for neutrons with muons in water tank • Can suppress cosmogenic background to < 0.01 events/ton/year
  • Astronomy and Astrophysics

    Astronomy and Astrophysics

    THE DECADE OF DISCOVERY IN ASTRONOMY AND ASTROPHYSICS Astronomy and Astrophysics Survey Committee Board on Physics and Astronomy Commission on Physical Sciences, Mathematics, and Applications National Research Council NATIONAL ACADEMY PRESS Washington, D.C. 1991 NATIONAL ACADEMY PRESS • 2101 Constitution Avenue, NW • Washington, DC 20418 NOTICE: The project that is the subject of this report was approved by the Governing Board of the National Research Council, whose members are drawn from the councils of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. The members of the committee responsible for the report were chosen for their special compe_nces and with regard for appropriate balance. This report has been reviewed by a group other than the authors according to procedures approved by a Report Review Committee consisting of members of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. This project was supported by the Department of Energy under Grant No. DE-FGO5- 89ER40421, the National Aeronautics and Space Administration and the National Science Foundation under Grant No. AST-8901685, the Naval Research Laboratory under Contract No. N00173-90-M-9744, and the Smithsonian Institution under Purchase Order No. SF0022430000. Additional support was provided by the Maurice Ewing Earth and Planetary Sciences Fund of the National Academy of Sciences created through a gift from the Palisades Geophysical Institute, Inc., and an anonymous donor. Library of Congress Cataloging-in-Publication Data National Research Council (U.S.). Astronomy and Astrophysics Survey Committee. The decade of discovery in astronomy and astrophysics / Astronomy and Astrophysics Survey Committee, Board on Physics and Astronomy, Commission on Physical Sciences, Mathematics, and Applications, National Research Council.
  • Experiments on the Differential Vlbi Measurements with the Former Russian Deep Space Network

    Experiments on the Differential Vlbi Measurements with the Former Russian Deep Space Network

    EXPERIMENTS ON THE DIFFERENTIAL VLBI MEASUREMENTS WITH THE FORMER RUSSIAN DEEP SPACE NETWORK Igor E. Molotov(1,2,3) (1)Bear Lakes Radio Astronomy Station of Central (Pulkovo) Astronomical Observatory, Pulkovskoye chosse 65/1, Saint-Petersburg, 196140, Russia , E-mail: [email protected] (2)Keldysh Institute of Applied Mathematics, Miusskaja sq. 4, 125047 Moscow, Russia (3)Central Research Institute for Machine Building, 4 Pionerskaya Street, Korolev, 141070, Russia ABSTRACT The differential VLBI technique (delta-VLBI) is applied transforms the signals into video frequencies, which for measuring spacecraft position with accuracy up to 1 then are sampled with 1- or 2-bit quantization, formatted in any standard VLBI format (Mk-4, S2, K-4, mas. This procedure allows to link the sky position of object with the position of close ICRF quasar on the Mk-2) and recorded on magnetic tapes or PC-disks celestial sphere. Few delta-VLBI measurements can together with precise clock using VLBI terminal. All frequency transformations are connected with atomic urgently improve the knowledge of object trajectory in the times of critical maneuvers. frequency standard. The tapes/disks from all radio telescopes of VLBI array are collected at data The Russian Deep Space Network that was based on processing center, where the data are cross-correlated. three large antennas: 70 m in Evpatoria (Ukraine) and The processing is aimed to measure the time delay of Ussuriysk (Far East), and 64 m in Bear Lakes (near emitted wavefront arrival to receiving antennas, and Moscow) arranged the trial delta-VLBI experiments frequency of interference (fringe rate), that contain the with help of four scientific institutions.
  • GRANAT/WATCH Catalogue of Cosmic Gamma-Ray Bursts: December 1989 to September 1994? S.Y

    GRANAT/WATCH Catalogue of Cosmic Gamma-Ray Bursts: December 1989 to September 1994? S.Y

    ASTRONOMY & ASTROPHYSICS APRIL I 1998,PAGE1 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 129, 1-8 (1998) GRANAT/WATCH catalogue of cosmic gamma-ray bursts: December 1989 to September 1994? S.Y. Sazonov1,2, R.A. Sunyaev1,2, O.V. Terekhov1,N.Lund3, S. Brandt4, and A.J. Castro-Tirado5 1 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117810 Moscow, Russia 2 Max-Planck-Institut f¨ur Astrophysik, Karl-Schwarzschildstr 1, 85740 Garching, Germany 3 Danish Space Research Institute, Juliane Maries Vej 30, DK 2100 Copenhagen Ø, Denmark 4 Los Alamos National Laboratory, MS D436, Los Alamos, NM 87545, U.S.A. 5 Laboratorio de astrof´ısica Espacial y F´ısica Fundamental (LAEFF), INTA, P.O. Box 50727, 28080 Madrid, Spain Received May 23; accepted August 8, 1997 Abstract. We present the catalogue of gamma-ray bursts celestial positions (the radius of the localization region is (GRB) observed with the WATCH all-sky monitor on generally smaller than 1 deg at the 3σ confidence level) board the GRANAT satellite during the period December of short-lived hard X-ray sources, which include GRBs. 1989 to September 1994. The cosmic origin of 95 bursts Another feature of the instrument relevant to observa- comprising the catalogue is confirmed either by their lo- tions of GRBs is that its detectors are sensitive over an calization with WATCH or by their detection with other X-ray energy range that reaches down to ∼ 8 keV, the do- GRB experiments. For each burst its time history and main where the properties of GRBs are known less than information on its intensity in the two energy ranges at higher energies.