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Grant Proposals, 1991-1999
Grant Proposals, 1991-1999 Finding aid prepared by Smithsonian Institution Archives Smithsonian Institution Archives Washington, D.C. Contact us at [email protected] Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Descriptive Entry.............................................................................................................. 1 Names and Subjects ...................................................................................................... 1 Container Listing ............................................................................................................. 2 Grant Proposals https://siarchives.si.edu/collections/siris_arc_251859 Collection Overview Repository: Smithsonian Institution Archives, Washington, D.C., [email protected] Title: Grant Proposals Identifier: Accession 99-171 Date: 1991-1999 Extent: 17 cu. ft. (17 record storage boxes) Creator:: Smithsonian Astrophysical Observatory. Contracts and Procurement Office Language: English Administrative Information Prefered Citation Smithsonian Institution Archives, Accession 99-171, Smithsonian Astrophysical Observatory, Contracts and Procurement Office, Grant Proposals Descriptive Entry This accession consists of records documenting Smithsonian Astrophysical Observatory projects and activities. Materials include proposals, correspondence, progress -
Formation of the Active Star Forming Region LHA 120-N 44 Triggered By
Draft version December 24, 2018 Typeset using LATEX twocolumn style in AASTeX61 FORMATION OF THE ACTIVE STAR FORMING REGION LHA 120-N 44 TRIGGERED BY TIDALLY-DRIVEN COLLIDING HI FLOWS Kisetsu Tsuge,1 Hidetoshi Sano,1,2 Kengo Tachihara,1 Cameron Yozin,3 Kenji Bekki,3 Tsuyoshi Inoue,1 Norikazu Mizuno,4 Akiko Kawamura,4 Toshikazu Onishi,5 and Yasuo Fukui1,2 1Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; [email protected] 2Institute for Advanced Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan 3ICRAR, M468, The University of Western Australia, 35 Stirling Highway, Crawley Western Australia 6009, Australia 4National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan 5Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan (Accepted November 30, 2018) ABSTRACT N44 is the second active site of high mass star formation next to R136 in the Large Magellanic Cloud (LMC). We carried out a detailed analysis of Hi at 60 arcsec resolution by using the ATCA & Parkes data. We presented decomposition of the Hi emission into two velocity components (the L- and D-components) with the velocity separation of ∼60 km s−1. In addition, we newly defined the I-component whose velocity is intermediate between the L- and D-components. The D-component was used to derive the rotation curve of the LMC disk, which is consistent with the stellar rotation curve (Alves & Nelson 2000). Toward the active cluster forming region of LHA 120-N 44, the three velocity components of Hi gas show signatures of dynamical interaction including bridges and complementary spatial distributions. -
Photons That Travel in Free Space Slower Than the Speed of Light Authors
Title: Photons that travel in free space slower than the speed of light Authors: Daniel Giovannini1†, Jacquiline Romero1†, Václav Potoček1, Gergely Ferenczi1, Fiona Speirits1, Stephen M. Barnett1, Daniele Faccio2, Miles J. Padgett1* Affiliations: 1 School of Physics and Astronomy, SUPA, University of Glasgow, Glasgow G12 8QQ, UK 2 School of Engineering and Physical Sciences, SUPA, Heriot-Watt University, Edinburgh EH14 4AS, UK † These authors contributed equally to this work. * Correspondence to: [email protected] Abstract: That the speed of light in free space is constant is a cornerstone of modern physics. However, light beams have finite transverse size, which leads to a modification of their wavevectors resulting in a change to their phase and group velocities. We study the group velocity of single photons by measuring a change in their arrival time that results from changing the beam’s transverse spatial structure. Using time-correlated photon pairs we show a reduction of the group velocity of photons in both a Bessel beam and photons in a focused Gaussian beam. In both cases, the delay is several microns over a propagation distance of the order of 1 m. Our work highlights that, even in free space, the invariance of the speed of light only applies to plane waves. Introducing spatial structure to an optical beam, even for a single photon, reduces the group velocity of the light by a readily measurable amount. One sentence summary: The group velocity of light in free space is reduced by controlling the transverse spatial structure of the light beam. Main text The speed of light is trivially given as �/�, where � is the speed of light in free space and � is the refractive index of the medium. -
Arxiv:1603.00726V1 [Physics.Optics] 2 Mar 2016
Single-pixel 3D imaging with time-based depth resolution Ming-Jie Sun,1, 2, ∗ Matthew. P. Edgar,2 Graham M. Gibson,2 Baoqing Sun,2 Neal Radwell,2 Robert Lamb,3 and Miles J. Padgett2, y 1Department of Opto-electronic Engineering, Beihang University, Beijing, 100191, China 2SUPA, School of Physics and Astronomy, University of Glasgow, Glasgow, G12 8QQ, UK 3Selex ES, Edinburgh, UK Time-of-flight three dimensional imaging is an important tool for many applications, such as object recognition and remote sensing. Unlike conventional imaging approach using pixelated detector array, single-pixel imaging based on projected patterns, such as Hadamard patterns, utilises an alternative strategy to acquire information with sampling basis. Here we show a modified single-pixel camera using a pulsed illumi- nation source and a high-speed photodiode, capable of reconstructing 128×128 pixel resolution 3D scenes to an accuracy of ∼ 3 mm at a range of ∼ 5 m. Furthermore, we demonstrate continuous real-time 3D video with a frame-rate up to 12 Hz. The sim- plicity of the system hardware could enable low-cost 3D imaging devices for precision ranging at wavelengths beyond the visible spectrum. Introduction Whilst a variety of 3D imaging technologies are suited for different applications, time-of-flight (TOF) systems have set the benchmark for performance with regards to a combination of accuracy and operating range. Time-of-flight imaging is performed by illuminating a scene with a pulsed light source and observing the back-scattered light. Correlating the detection time of the back-scattered light with the time of the illumination pulse allows the distance, d, to objects within the scene to be estimated by d = tc=2, where t is the TOF and c is the propagation speed of light. -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
The Cataclysmic Variable AE Aquarii: Orbital Variability in V Band
The cataclysmic variable AE Aquarii: orbital variability in V band R. Zamanov & G. Latev Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Shose 72, BG-1784 Sofia, Bulgaria [email protected] [email protected] (Submitted on 28.11.2016. Accepted on 31.01.2017) Abstract. We present 62.7 hours observations of the cataclysmic variable AE Aqr in Johnson V band. These are non-published archive electro-photometric data obtained during the time period 1993 to 1999. We construct the orbital variability in V band and obtain a Fourier fit to the double-wave quiescent light curve. The strongest flares in our data set are in phase interval 0.6 - 0.8. The data can be downloaded from http://www.astro.bas.bg/∼rz/DATA/AEAqr.elphot.dat. Key words: Stars: novae, cataclysmic variables – Accretion, accretion disks – white dwarfs – Stars: individual: AE Aqr 1 Introduction AE Aqr is a bright intermediate polar cataclysmic variable (V ≈ 11−12.3). In this semi-detached binary system a spotted K type dwarf (K0-K4 IV/V star) transfers material through the inner Lagrangian point L1 toward a magnetic white dwarf (Skidmore et al. 2003, Hill et al. 2016). It has a relatively long orbital period of 9.88 hours (Robinson et al. 1991; Echevarr´ıa et al. 2008) and an extremely short rotational period of the white dwarf of only 33 s (Patterson et al. 1980). To appear in such a state, AE Aqr should be a former supersoft X-ray binary, in which the mass transfer rate in the recent past (≈ 107 yr) has been much higher than its current value (Schenker et al. -
Msc-Whipple Analysis 2010
TWO DIMENSIONAL ANALYSIS OF INCOMPLETE PARAMETERISED ARCHIVAL DATA FROM THE WHIPPLE 10 METRE IMAGING ATMOSPHERIC CHERENKOV TELESCOPE CENTERED ON AE AQUARII by Michael Connolly H.Dip., B.D., B.Ph., B.Sc. A dissertation submitted to the Centre for Astronomy, School of Physics, National University of Ireland, Galway in fulfilment of the requirements for the degree of Master of Science Supervisor Dr Mark Lang February 2010 Galway, Ireland MSc-Whipple Analysis 2010 Dedicated to the memory of Martin Connolly (1940-1985) Hard work and belief can accomplish, With God’s help 1. Michael Connolly Page 2 MSc-Whipple Analysis 2010 1. Michael Connolly Page 3 MSc-Whipple Analysis 2010 Contents List of Figures. 8 List of Tables. 12 Acknowledgements. 12 Abstract. 14 Chapter 1: Introduction to Thesis 1.1 Introduction. 16 1.2 Thesis Overview. 17 1.3 Personal Contribution. 18 Chapter 2: Very High Energy Gamma-Ray Astronomy 2.1 Introduction. 20 2.2 Gamma ray production in the Earth’s atmosphere. 23 2.3 Extensive Air Showers. 23 2.3.1 Pair Production. 24 2.3.2 Electron-photon cascades or electromagnetic showers. 25 2.4 Extensive air showers from two different progenitors. 26 2.4.1 Properties of gamma ray induced showers. 26 2.4.2 Properties of cosmic ray induced showers. 27 2.5 What is Cherenkov light? . 28 1. Michael Connolly Page 4 MSc-Whipple Analysis 2010 2.6 Relative incidence of high energy electromagnetic photons . 31 2.7 History. 33 2.8 VHE gamma ray sources and production. 38 2.8.1 Physical processes involved in gamma ray production. -
29 Jan 2020 11Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-Ku, Sapporo, Hokkaido 060-0810, Japan
Publ. Astron. Soc. Japan (2014) 00(0), 1–42 1 doi: 10.1093/pasj/xxx000 FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant molecular cloud complex Mikito KOHNO1∗, Kengo TACHIHARA1∗, Kazufumi TORII2∗, Shinji FUJITA1∗, Atsushi NISHIMURA1,3, Nario KUNO4,5, Tomofumi UMEMOTO2,6, Tetsuhiro MINAMIDANI2,6,7, Mitsuhiro MATSUO2, Ryosuke KIRIDOSHI3, Kazuki TOKUDA3,7, Misaki HANAOKA1, Yuya TSUDA8, Mika KURIKI4, Akio OHAMA1, Hidetoshi SANO1,9, Tetsuo HASEGAWA7, Yoshiaki SOFUE10, Asao HABE11, Toshikazu ONISHI3 and Yasuo FUKUI1,9 1Department of Physics, Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan 2Nobeyama Radio Observatory, National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences (NINS), 462-2, Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan 3Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan 4Department of Physics, Graduate School of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Ten-nodai, Tsukuba, Ibaraki 305-8577, Japan 5Tomonaga Center for the History of the Universe, University of Tsukuba, Ten-nodai 1-1-1, Tsukuba, Ibaraki 305-8571, Japan 6Department of Astronomical Science, School of Physical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan 7National Astronomical Observatory of Japan (NAOJ), National -
Astrophysical Studies of Extrasolar Planetary Systems Using Infrared Interferometric Techniques Olivier Absil
Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques Olivier Absil To cite this version: Olivier Absil. Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques. Astrophysics [astro-ph]. Université de Liège, 2006. English. tel-00124720 HAL Id: tel-00124720 https://tel.archives-ouvertes.fr/tel-00124720 Submitted on 15 Jan 2007 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Facult´edes Sciences D´epartement d’Astrophysique, G´eophysique et Oc´eanographie Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques THESE` pr´esent´eepour l’obtention du diplˆomede Docteur en Sciences par Olivier Absil Soutenue publiquement le 17 mars 2006 devant le Jury compos´ede : Pr´esident: Pr. Jean-Pierre Swings Directeur de th`ese: Pr. Jean Surdej Examinateurs : Dr. Vincent Coude´ du Foresto Dr. Philippe Gondoin Pr. Jacques Henrard Pr. Claude Jamar Dr. Fabien Malbet Institut d’Astrophysique et de G´eophysique de Li`ege Mis en page avec la classe thloria. i Acknowledgments First and foremost, I want to express my deepest gratitude to my advisor, Professor Jean Surdej. I am forever indebted to him for striking my interest in interferometry back in my undergraduate student years; for introducing me to the world of scientific research and fostering so many international collaborations; for helping me put this work in perspective when I needed it most; and for guiding my steps, from the supervision of diploma thesis to the conclusion of my PhD studies. -
New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope&amp;#39;s view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way. -
Search for Gamma-Ray Emission from AE Aquarii with Seven Years of FERMI-LAT Observations
Search for gamma-ray emission from AE Aquarii with seven years of FERMI-LAT observations Jian Li1, Diego F. Torres1,2, Nanda Rea1,3, Emma de O˜na Wilhelmi1, Alessandro Papitto4, Xian Hou5, & Christopher W. Mauche6 ABSTRACT AE Aquarii (AE Aqr) is a cataclysmic binary hosting one of the fastest rotating (Pspin = 33.08 s) white dwarfs known. Based on seven years of Fermi Large Area Tele- scope (LAT) Pass 8 data, we report on a deep search for gamma-ray emission from æ. Using X-ray observations from ASCA, XMM-Newton, Chandra, Swift, Suzaku, and NuSTAR, spanning 20 years, we substantially extend and improve the spin ephemeris of æ. Using this ephemeris, we searched for gamma-ray pulsations at the spin period of the white dwarf. No gamma-ray pulsations were detected above 3 σ significance. Neither phase-averaged gamma-ray emission nor gamma-ray variability of æ is de- tected by Fermi-LAT. We impose the most restrictive upper limit to the gamma-ray flux from æ to date: 1.3 × 10−12 erg cm−2 s−1 in the 100 MeV–300 GeV energy range, providing constraints on models. Subject headings: gamma rays: stars — cataclysmic binary: individual: æ 1. Introduction Cataclysmic variables (CVs) are semi-detached binaries consisting of a white dwarf (WD) and a companion star, usually a red dwarf. æ is a bright (V≈11, Welsh et al. 1999) CV hosting one of the fastest rotating WDs known (Pspin = 33.08 s, Patterson 1979) and a K 4-5 V secondary; it is arXiv:1608.06662v1 [astro-ph.HE] 23 Aug 2016 1Institute of Space Sciences (IEEC-CSIC), Campus UAB, Carrer de Magrans s/n, 08193 Barcelona, Spain 2Instituci´oCatalana de Recerca i Estudis Avanc¸ats (ICREA), E-08010 Barcelona, Spain 3Anton Pannekoek Institute, University of Amsterdam, Postbus 94249, NL-1090-GE Amsterdam, The Netherlands 4INAF-Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monte Porzio Catone, Roma, Italy 5Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China.