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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. -
The Giant Magellan Telescope. Status
The Giant Magellan Telescope. Status By Dr. Mauricio Pilleux Head of Administration (Chile) GMTO Corporation [email protected] April 17, 2019 Observatories in Chile: The beginnings … a successful experiment Cerro Tololo Interamerican Observatory AURA, 1962 Magellan telescopes, 2000 Las Campanas Carnegie Institution of Washington, 1968 La Silla ESO, 1969 2 Observatories in Chile: “Second stage” Very Large Telescope (VLT) Cerro Paranal, ESO, 1999 Gemini South Cerro Pachón, 2002 (AURA) ALMA NRAO-ESO-NAOJ, 2013 3 Observatories in Chile: “Stage 3.0” – big, big, big Giant Magellan Telescope (GMT) Cerro Las Campanas, 2023 (GMTO Corporation) European- Extremely Large Telescope (EELT) Cerro Armazones, 2026 (ESO) Large Synoptic Survey Telescope (LSST) Cerro Pachón, 2022 (NSF/AURA-DOE/SLAC) 4 What next? Size (physical) GMT TMT EELT LSST Main Author – Presentation Title Observatories in Chile: Where? ALMA CCAT* Nanten 2 ASTE Paranal Vista ACT 2 3 E-ELT* TAO* Apex CTA* Las Campanas GMT* Polar Bear Simons Obs. La Silla 1 Tololo SOAR Gemini LSST* 6 Giant Magellan Telescope (GMT): Will be the largest in the world in 2022 25 meters in diameter “Price”: US$1340 million First light: 2023 Enclosure is 62 m high Groundbreaking research in: . Exoplanets and their atmospheres . Dark matter . Distant objects . Unknown unknowns 7 Just how tall is the GMT? 46 meters 8 Giant Magellan Telescope (GMT): The world’s largest optical telescope Korea Sao Paulo, Brazil Texas A&M Arizona New partners are welcome! Main Author – Presentation Title 9 Central mirror casting -
THE GAMMA RAY EXPERIMENT for the SMALL ASTRONOMY SATELLITE B (SAS-B) C. E. Fichtel, C. H..~Hrmann, R. C. Hartman, D. A. Kniffen
THE GAMMA RAY EXPERIMENT FOR THE SMALL ASTRONOMY SATELLITE B (SAS-B) C. E. Fichtel, C. H.. ~hrmann, R. C. Hartman, D. A. Kniffen, H. B. Ogelman*, and R. W. Ross Goddard Space Flight Center, Greenbelt, Md. 20771 Abstract A magnetic core digitized spark chamber gamma ray telescope has been developed for satellite use and will be flown on SAS-B in less than one year. The SAS-B detector will have the following characteristics: Effective area ~ 500 cm2 , solid angle = ~ SR; Efficiency (high energy) ~ 0.29; and time resolution of better than two milliseconds. A detailed picture of the galactic plane in gamma rays should be obtained with this experiment, and a study of point sources, including short bursts of gamma rays from supernovae explosions, will also be possible. 1. Introduction The SAS-B gamma ray telescope represents the first satellite version of a planned evolution of a gamma ray digitized spark chamber telescope which began with the development of a balloon borne instrument. The telescope is aimed at the study of gamma rays whose energy exceeds about 20 MeV. In the early 1960's, it was realized that the celestial gamma ray intensity was very low compared to the high background of cosmic ray particles and earth albedo. For this reason, a picture type detector seemed to be needed to identify unambiguously the electron pair produced by the gamma ray and to study its properties - particularly to obtain a measure of the energy and arrival direction of the gamma ray. In addition, the secondary gamma ray flux produced by cosmic rays in the atmosphere, even at the altitudes of the present large balloons, severely limits the gamma ray astronomy which can be accomplished with balloons and dictates that gamma ray ~stronomy must ultimately be accomplished with detector systems on satellites. -
Exoplanet Community Report
JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probeclass missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2 -
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. -
Effective Aperture 3.6–4.9 M) 4.7 M 186″ Segmented, MMT (6×1.8 M) F
Effective Effective Mirror type Name Site Built aperture aperture (m) (in) 10.4 m 409″ Segmented, Gran Telescopio Roque de los Muchachos 2006/9 36 Canarias (GTC) Obs., Canary Islands, Spain 10 m 394″ Segmented, Keck 1 Mauna Kea Observatories, 1993 36 Hawaii, USA 10 m 394″ Segmented, Keck 2 Mauna Kea Observatories, 1996 36 Hawaii, USA 9.8 m 386″ Segmented, Southern African South African Astronomical 2005 91 Large Telescope Obs., Northern Cape, South (SALT) Africa 9.2 m 362″ Segmented, Hobby-Eberly McDonald Observatory, 1997 91 Telescope (HET) Texas, USA (11 m × 9.8 m mirror) 8.4 m×2 330″×2 Multiple Large Binocular Mount Graham 2004 (can use mirror, 2 Telescope (LBT) Internationals Obs., Phased- Arizona array optics for combined 11.9 m[2]) 8.2 m 323″ Single Subaru (JNLT) Mauna Kea Observatories, 1999 Hawaii, USA 8.2 m 323″ Single VLT UT1 (Antu) Paranal Observatory, 1998 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT2 (Kueyen) Paranal Observatory, 1999 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT3 (Melipal) Paranal Observatory, 2000 Antofagasta Region, Chile 8.2 m 323″ Single VLT UT4 (Yepun) Paranal Observatory, 2001 Antofagasta Region, Chile 8.1 m 318″ Single Gemini North Mauna Kea Observatories, 1999 (Gillett) Hawaii, USA 8.1 m 318″ Single Gemini South Cerro Pachón (CTIO), 2001 Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 1 Las Campanas Obs., 2000 (Walter Baade) Coquimbo Region, Chile 6.5 m 256″ Honeycomb Magellan 2 Las Campanas Obs., 2002 (Landon Clay) Coquimbo Region, Chile 6.5 m 256″ Single MMT (1 x 6.5 M1) F. -
Memo 67 SKA Demonstrators, 2005 Assessment by the Engineering Working Group
Memo 67 SKA Demonstrators, 2005 Assessment by the Engineering Working Group P. J. Hall (EWG Chair), On Behalf of the Group 01/12/05 www.skatelescope.org/pages/page_memos.htm 2 Table of Contents Section Page Summary Remarks 3 Appendix 1 – Reviews of 2005 SKA Demonstrator Updates Chinese Demonstrator (FAST) 10 Canadian Demonstrator (CLAR) 13 US Demonstrators (ATA, DSAN) 16 European Demonstrator (EMBRACE) 19 South African Demonstrator (KAT) 22 Appendix 2 – Guidelines for Reviewers 29 Appendix 3 – SKA Demonstrator Updates for 2005 33 (PDF documents Appended as Submitted) 3 SKA Demonstrators – Summary Remarks Peter Hall, 1 December 2005 1. Introduction The EWG has considered the five SKA demonstrator submissions received. In four cases these submissions were brief updates of previous (2004) detailed expositions. However, an initial outline of the Karoo Array Telescope (KAT) was received from the South African SKA Consortium and the EWG devoted extra effort to a more thorough assessment of this project. No demonstrator updates were received from Australia or India although the Australian SKA Consortium submitted a background report in the form of the statutory annual report for their Major National Research Facility program (available at http://www.atnf.csiro.au/projects/mnrf2001/Astronomy_MNRF_0405.pdf). While this report does not contain detailed schedule information for the proposed Extended New Technology Demonstrator (xNTD) project, it does indicate that the SKA Molonglo Prototype (SKAMP) program is still largely on track. However, additional enquiries indicate that SKAMP development beyond mid-2007 still depends on as yet uncertain funding. It should also be mentioned that KAT and xNTD are very similar instruments and much of the EWG commentary is likely to apply to both projects. -
Biography of Horace Welcome Babcock
NATIONAL ACADEMY OF SCIENCES H O R ACE W ELCOME B A B COC K 1 9 1 2 — 2 0 0 3 A Biographical Memoir by GEO R G E W . P R ESTON Any opinions expressed in this memoir are those of the author and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 2007 NATIONAL ACADEMY OF SCIENCES WASHINGTON, D.C. Photograph by Mount Wilson and Los Campanas Observatories HORACE WELCOME BABCOCK September 13, 1912−August 29, 2003 BY GEORGE W . P RESTON ORACE BABCOCK’S CAREER at the Mount Wilson and Palomar H(later, Hale) Observatories spanned more than three decades. During the first 18 years, from 1946 to 1964, he pioneered the measurement of magnetic fields in stars more massive than the sun, produced a famously successful model of the 22-year cycle of solar activity, and invented important instruments and techniques that are employed throughout the world to this day. Upon assuming the directorship of the observatories, he devoted his last 14 years to creating one of the world’s premier astronomical observatories at Las Campanas in the foothills of the Chilean Andes. CHILDHOOD AND EDUCATION Horace Babcock was born in Pasadena, California, the only child of Harold and Mary Babcock. Harold met Horace’s mother, Mary Henderson, in Berkeley during his student days at the College of Electrical Engineering, University of California. After brief appointments as a laboratory assis- tant at the National Bureau of Standards in 1906 and as a physics teacher at the University of California, Berkeley, in 1907, Horace’s father was invited by George Ellery Hale in 1908 to join the staff of the Mount Wilson Observatory (MWO), where he remained for the rest of his career. -
Support for Site Testing of the European Extremely Large Telescope: Precipitable Water Vapour Over La Silla†
Support for site testing of the European Extremely Large Telescope: precipitable water vapour over La Silla† Richard R. Querel*a, Florian Kerberb, Gaspare Lo Curtob, Joanna E. Thomas-Osipc, Gabriel Prietoc, Arlette Chac´ond, Omar Cuevasd, Diana Pozod, Julio Mar´ınd, David A. Naylora, Michel Cur´ed, Marc S. Sarazinb, Carlos Guiraob and Gerardo Avilab aInstitute for Space Imaging Science, University of Lethbridge, Canada; bEuropean Southern Observatory, Garching, Germany; cLas Campanas Observatory, La Serena, Chile; dGrupo Astrometeorolog´ıa, Universidad de Valparaiso, Chile ABSTRACT The European Southern Observatory (ESO), the Institute for Space Imaging Science (ISIS) and the AstroMete- orology group at the Universidad de Valparaiso collaborated on a project to understand the precipitable water vapour (PWV) over the La Silla Paranal Observatory. Both La Silla and Paranal were studied with the goal of using them as reference sites to evaluate potential E-ELT sites. As ground-based infrared astronomy matures, our understanding of the atmospheric conditions over the observatories becomes paramount, specifically water vapour since it is the principle source of atmospheric opacity at infrared wavelengths. Several years of archival optical spectra (FEROS) have been analysed to reconstruct the PWV history above La Silla using an atmospheric radiative transfer model (BTRAM) developed by ISIS. In order to better understand the systematics involved, a dedicated atmospheric water vapour measurement campaign was conducted in May 2009 in close collaboration with Las Campanas observatory and the GMT site testing team. Several methods of determining the water col- umn were employed, including radiosonde launches, continuous measurements by infrared radiometers (IRMA), a compact echelle spectrograph (BACHES) and several high-resolution optical echelle spectrographs (FEROS, HARPS and MIKE). -
HATS-7B: a HOT SUPER NEPTUNE TRANSITING a QUIET K DWARF STAR* G
The Astrophysical Journal, 813:111 (10pp), 2015 November 10 doi:10.1088/0004-637X/813/2/111 © 2015. The American Astronomical Society. All rights reserved. HATS-7b: A HOT SUPER NEPTUNE TRANSITING A QUIET K DWARF STAR* G. Á. Bakos1,12,13, K. Penev1, D. Bayliss2,3, J. D. Hartman1, G. Zhou1,2, R. Brahm4,5, L. Mancini6, M. de Val-Borro1, W. Bhatti1, A. Jordán4,5, M. Rabus4,6, N. Espinoza4,5, Z. Csubry1,A.W.Howard7, B. J. Fulton7,14, L. A. Buchhave8,9, S. Ciceri6, T. Henning6, B. Schmidt2, H. Isaacson10, R. W. Noyes8, G. W. Marcy10,V.Suc4,A.R.Howe1, A. S. Burrows1, J. Lázár11, I. Papp11, and P. Sári11 1 Department of Astrophysical Sciences, Princeton University, NJ 08544, USA 2 Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia 3 Observatoire Astronomique de l’Université de Genève, 51 ch. des Maillettes, 1290 Versoix, Switzerland 4 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 5 Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 6 Max Planck Institute for Astronomy, Heidelberg, Germany 7 Institute for Astronomy, University of Hawaii at Manoa, Honolulu, HI, USA 8 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA 9 Centre for Star and Planet Formation, Natural History Museum, University of Copenhagen, Denmark 10 Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 11 Hungarian Astronomical Association, Budapest, Hungary Received 2015 July 3; accepted 2015 September 14; published 2015 November 4 ABSTRACT We report the discovery by the HATSouth network of HATS-7b, a transiting Super-Neptune with a mass of 0.120 ± +0.046 0.012 MJ, a radius of 0.563-0.034 RJ, and an orbital period of 3.1853 days. -
NRAO Enews: Vol. 10, Issue 7
NRAO eNews Volume 10, Issue 7 • 10 August 2017 Upcoming Events ALMA Long Baseline Workshop (http://alma intweb.mtk.nao.ac.jp/~diono/meetings/longBL2017/) Oct 3 5, 2017 | Mielparque Kyoto, Japan 6th VLA Data Reduction Workshop (http://go.nrao.edu/vladrw) Oct 23 27, 2017 | Socorro, NM 2017 Jansky Lecture (https://science.nrao.edu/science/janskylecture/speakers/2017jansky lecturerdrbernardfanaroff) Oct 24, 2017 | Charlottesville, VA 2017 Jansky Lecture (https://science.nrao.edu/science/janskylecture/speakers/2017jansky lecturerdrbernardfanaroff) Oct 27, 2017 | Green Bank Observatory, WV 2017 Jansky Lecture (https://science.nrao.edu/science/janskylecture/speakers/2017jansky lecturerdrbernardfanaroff) Nov 3, 2017 | Socorro, NM NRAO Town Hall at the Jan 2018 AAS Meeting (https://science.nrao.edu/science/meetings/2018/aas231/townhall) Jan 11, 2018 | National Harbor, MD The Very Large Array Today and Tomorrow: First Molecules to Life on Exoplanets (https://science.nrao.edu/science/meetings/2018/aas231/vla) Jan 11, 2018 | National Harbor, MD The Very Large Array Today and Tomorrow: First Molecules to Life on Exoplanets Eric Murphy The NRAO will convene a Special Session entitled The Very Large Array Today and Tomorrow: First Molecules to Life on Exoplanets on 11 January 2018 in National Harbor, Maryland, near Washington, D.C. during the 231st Meeting of the American Astronomical Society (AAS). The Very Large Array (VLA) has had a major impact on nearly every branch of astronomy, and the results of its research are abundant in the pages of scientific journals and textbooks. -
Arxiv:2007.07969V3 [Astro-Ph.CO] 22 Mar 2021
INR-TH-2020-032 Towards Testing Sterile Neutrino Dark Matter with Spectrum-Roentgen-Gamma Mission V. V. Barinov,1, 2, ∗ R. A. Burenin,3, 4, y D. S. Gorbunov,2, 5, z and R. A. Krivonos3, x 1Physics Department, M. V. Lomonosov Moscow State University, Leninskie Gory, Moscow 119991, Russia 2Institute for Nuclear Research of the Russian Academy of Sciences, Moscow 117312, Russia 3Space Research Institute of the Russian Academy of Sciences, Moscow 117997, Russia 4National Research University Higher School of Economics, Moscow 101000, Russia 5Moscow Institute of Physics and Technology, Dolgoprudny 141700, Russia We investigate the prospects of the SRG mission in searches for the keV-scale mass sterile neutrino dark matter radiatively decaying into active neutrino and photon. The ongoing all-sky X-ray survey of the SRG space observatory with data acquired by the ART-XC and eROSITA telescopes can provide a possibility to fully explore the resonant production mechanism of the dark matter sterile neutrino, which exploits the lepton asymmetry in the primordial plasma consistent with cosmological limits from the Big Bang Nucleosynthesis. In particular, it is shown that at the end of the four year all-sky survey, the sensitivity of the eROSITA telescope near the 3.5 keV line signal reported earlier can be comparable to that of the XMM -Newton with all collected data, which will allow one to carry out another independent study of the possible sterile neutrino decay signal in this area. In the energy range below ≈ 2:4 keV, the expected constraints on the model parameters can be significantly stronger than those obtained with XMM -Newton.