Herschel Space Observatory: Opening New Windows on the Universe
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Exhibits and Financial Statement Schedules 149
Table of Contents UNITED STATES SECURITIES AND EXCHANGE COMMISSION Washington, D.C. 20549 FORM 10-K [ X] ANNUAL REPORT PURSUANT TO SECTION 13 OR 15(d) OF THE SECURITIES EXCHANGE ACT OF 1934 For the fiscal year ended December 31, 2011 OR [ ] TRANSITION REPORT PURSUANT TO SECTION 13 OR 15(d) OF THE SECURITIES EXCHANGE ACT OF 1934 For the transition period from to Commission File Number 1-16417 NUSTAR ENERGY L.P. (Exact name of registrant as specified in its charter) Delaware 74-2956831 (State or other jurisdiction of (I.R.S. Employer incorporation or organization) Identification No.) 2330 North Loop 1604 West 78248 San Antonio, Texas (Zip Code) (Address of principal executive offices) Registrant’s telephone number, including area code (210) 918-2000 Securities registered pursuant to Section 12(b) of the Act: Common units representing partnership interests listed on the New York Stock Exchange. Securities registered pursuant to 12(g) of the Act: None. Indicate by check mark if the registrant is a well-known seasoned issuer, as defined in Rule 405 of the Securities Act. Yes [X] No [ ] Indicate by check mark if the registrant is not required to file reports pursuant to Section 13 or Section 15(d) of the Act. Yes [ ] No [X] Indicate by check mark whether the registrant (1) has filed all reports required to be filed by Section 13 or 15(d) of the Securities Exchange Act of 1934 during the preceding 12 months (or for such shorter period that the registrant was required to file such reports), and (2) has been subject to such filing requirements for the past 90 days. -
Rfi Issue and Spectrum Sharing Paradigm for Future Satellite
RFI ISSUE AND SPECTRUM SHARING PARADIGM FOR FUTURE SATELLITE COMMUNICATION AND RADIO ASTRONOMY SYSTEMS by Yucheng Dai APPROVED BY SUPERVISORY COMMITTEE: Dr. Hlaing Minn, Chair Dr. John P. Fonseka Dr. Andrea Fumagalli Dr. Murat Torlak Copyright © 2020 Yucheng Dai All rights reserved Dedicated to my family, I received no more powerful and effective support than the support from my beloved family. RFI ISSUE AND SPECTRUM SHARING PARADIGM FOR FUTURE SATELLITE COMMUNICATION AND RADIO ASTRONOMY SYSTEMS by YUCHENG DAI, BS, MS DISSERTATION Presented to the Faculty of The University of Texas at Dallas in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY IN ELECTRICAL ENGINEERING THE UNIVERSITY OF TEXAS AT DALLAS August 2020 ACKNOWLEDGMENTS I would like to thank my PhD adviser, Dr. Hlaing Minn, for his valuable advice, dedicated guidance, and unparalleled support that made this work possible. I would like to express my deepest appreciation to my committee members, Drs. Andrea Fumagalli, John P. Fonseka, and Murat Torlak. I would like to thank my parents, for their guidance to the way to PhD, and for their support both spiritually and financially. I also want to thank my friend and lab-mate, Dong Han, who shows an example of dedicated and helpful PhD student to me. June 2020 v RFI ISSUE AND SPECTRUM SHARING PARADIGM FOR FUTURE SATELLITE COMMUNICATION AND RADIO ASTRONOMY SYSTEMS Yucheng Dai, PhD The University of Texas at Dallas, 2020 Supervising Professor: Dr. Hlaing Minn, Chair Wireless services, which utilize radio spectrum resources, can be classified into two types: passive wireless services and active wireless services. -
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. -
Abundance Study of the Two Solar-Analogue Corot Targets HD 42618 and HD 43587 from HARPS Spectroscopy ,
A&A 552, A42 (2013) Astronomy DOI: 10.1051/0004-6361/201220883 & c ESO 2013 Astrophysics Abundance study of the two solar-analogue CoRoT targets HD 42618 and HD 43587 from HARPS spectroscopy, T. Morel1,M.Rainer2, E. Poretti2,C.Barban3, and P. Boumier4 1 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, Bât. B5c, 4000 Liège, Belgium e-mail: [email protected] 2 INAF – Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy 3 LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195 Meudon Cedex, France 4 Institut d’Astrophysique Spatiale, UMR 8617, Université Paris XI, Bâtiment 121, 91405 Orsay Cedex, France Received 11 December 2012 / Accepted 11 February 2013 ABSTRACT We present a detailed abundance study based on spectroscopic data obtained with HARPS of two solar-analogue main targets for the asteroseismology programme of the CoRoT satellite: HD 42618 and HD 43587. The atmospheric parameters and chemical com- position are accurately determined through a fully differential analysis with respect to the Sun observed with the same instrumental set-up. Several sources of systematic errors largely cancel out with this approach, which allows us to narrow down the 1-σ error bars to typically 20 K in effective temperature, 0.04 dex in surface gravity, and less than 0.05 dex in the elemental abundances. Although HD 42618 fulfils many requirements for being classified as a solar twin, its slight deficiency in metals and its possibly younger age indicate that, strictly speaking, it does not belong to this class of objects. -
EUCLID Mission Assessment Study
EUCLID Mission Assessment Study Executive Summary ESA Contract. No. 5856/08/F/VS September 2009 EUCLID– Mapping the Dark Universe EUCLID is a mission to study geometry and nature of the dark universe. It is a medium-class mission candidate within ESA's Cosmic Vision 2015– 2025 Plan for launch around 2017. EUCLID has been derived by ESA from DUNE and SPACE, two complementary Cosmic Vision proposals addressing questions on the origin and the constitution of the Universe. 70% Dark Energy The observational methods applied by EUCLID are shape and redshift measure- ments of galaxies and clusters of galaxies. To 4% Baryonic Matter this end EUCLID is equipped with 3 scientific instruments: 26% Dark Matter • Visible Imager (VIS) • Near-Infrared Photometer (NIP) • Near-Infrared Spectrograph (NIS) The EUCLID Mission Assessment Study is the industrial part of the EUCLID assessment phase. The study has been performed by Astrium from September 2008 to September 2009 and is intended for space segment definition and programmatic evaluation. The prime responsibility is with Astrium GmbH (Friedrichshafen, Germany) with support from Astrium SAS (Toulouse, France) and Astrium Ltd (Stevenage, UK). EUCLID Mission EUCLID shall observe 20.000 deg2 of the extragalactic sky at galactic latitudes |b|>30 deg. The sky is sampled in step & b>30° stare mode with instantaneous fields of about 0.5 deg2 . Nominally a strip of about 20 deg in latitude is scanned per day (corresponding to about 1 deg in longitude). galactic plane step 1 b<30° step 2 step 3 The sky is nominally observed along great circles in planes perpendicular to the Sun- spacecraft axis (SAA=0). -
Planetary Defence Activities Beyond NASA and ESA
Planetary Defence Activities Beyond NASA and ESA Brent W. Barbee 1. Introduction The collision of a significant asteroid or comet with Earth represents a singular natural disaster for a myriad of reasons, including: its extraterrestrial origin; the fact that it is perhaps the only natural disaster that is preventable in many cases, given sufficient preparation and warning; its scope, which ranges from damaging a city to an extinction-level event; and the duality of asteroids and comets themselves---they are grave potential threats, but are also tantalising scientific clues to our ancient past and resources with which we may one day build a prosperous spacefaring future. Accordingly, the problems of developing the means to interact with asteroids and comets for purposes of defence, scientific study, exploration, and resource utilisation have grown in importance over the past several decades. Since the 1980s, more and more asteroids and comets (especially the former) have been discovered, radically changing our picture of the solar system. At the beginning of the year 1980, approximately 9,000 asteroids were known to exist. By the beginning of 2001, that number had risen to approximately 125,000 thanks to the Earth-based telescopic survey efforts of the era, particularly the emergence of modern automated telescopic search systems, pioneered by the Massachusetts Institute of Technology’s (MIT’s) LINEAR system in the mid-to-late 1990s.1 Today, in late 2019, about 840,000 asteroids have been discovered,2 with more and more being found every week, month, and year. Of those, approximately 21,400 are categorised as near-Earth asteroids (NEAs), 2,000 of which are categorised as Potentially Hazardous Asteroids (PHAs)3 and 2,749 of which are categorised as potentially accessible.4 The hazards posed to us by asteroids affect people everywhere around the world. -
Observations from Orbiting Platforms 219
Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey. -
Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/Luminous Infrared Galaxies Observed with Nustar And/Or Swift/BAT
Draft version July 26, 2021 Typeset using LATEX twocolumn style in AASTeX631 Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada ,1 Yoshihiro Ueda ,1 Atsushi Tanimoto ,2 Masatoshi Imanishi ,3, 4 Yoshiki Toba ,1, 5 Claudio Ricci ,6, 7, 8 and George C. Privon 9 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan 2Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan 3National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 5Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan 6N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 7Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China 8George Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Drive, Fairfax, VA 22030, USA 9National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903, USA (Received April 13, 2021; Revised June 11, 2021; Accepted Jul, 2021) ABSTRACT We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard (>10 keV) X-ray detected active galactic nuclei (AGNs) and con- strain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al. -
Orbital Debris: a Chronology
NASA/TP-1999-208856 January 1999 Orbital Debris: A Chronology David S. F. Portree Houston, Texas Joseph P. Loftus, Jr Lwldon B. Johnson Space Center Houston, Texas David S. F. Portree is a freelance writer working in Houston_ Texas Contents List of Figures ................................................................................................................ iv Preface ........................................................................................................................... v Acknowledgments ......................................................................................................... vii Acronyms and Abbreviations ........................................................................................ ix The Chronology ............................................................................................................. 1 1961 ......................................................................................................................... 4 1962 ......................................................................................................................... 5 963 ......................................................................................................................... 5 964 ......................................................................................................................... 6 965 ......................................................................................................................... 6 966 ........................................................................................................................ -
Variable and Broad Iron Lines Around Black Holes
Variable and Broad Iron Lines around Black Holes ESAC/ XMM-Newton Science Operations Center Workshop 26 – 28 June, 2006 “Broad” Iron Line ～20 years ago Cyg X-1 EXOSAT Barr et al. Tenma Kitamoto et al. broad narrow Gas Scintillation prop. Counter: best energy resolution at that time Rest frame @6.4 keV Iron K-line profile Newtonian near a black hole Special Relativity: Beaming and Fabian et al. 1989 Transverse Doppler General Relativity: Gravitational Redshift Disk Emissivity νobs/νem Fe K emission • Most prominent feature in X-ray spectrum of reprocessed (reflected) emission • Important diagnostics of illuminating source & illuminated matter • Sensitive probe of central region under extreme physical conditions • Potential of determining BH Mass & Spin [Fabian] [Matt] [Miniutti] ~10 yrs ago with ASCA K. Nandra Era of XMM-Newton, Chandra & Suzaku higher sensitivity and/or higher energy resolution • Presence of broad Fe lines confirmed and more are found • Also from Galactic BHBs • More complex spectral & time-variability features / properties discovered • Interpretations developed Relativistic Lines in Galactic BHs little affected by continuum model [Miller] Cyg X-1 (XMM) (JMM 02, 06) GRS 1915+105 (CXO) XTE J1550-564 (ASCA) (JMM 04) (JMM 04) GX 339-4 (CXO) (JMM 04) XTE J1650-500 (XMM) GRO J1655-40 (ASCA) (JMM 02) Broad Fe line in ~20 systems: [J.Miller] Is the relativistic broad Fe line robust? POTENTIAL COMPLICATIONS • Narrow components • Blueshifted & redshifted lines [Cappi] • Compton reflection • High ionization / high column absorbers -
Infrared Astronomical Satellite IRAS
Infrared Astronomical Satellite IRAS Dr. Dusan Petrac 1 2 IRAS satellite 3 Collaboration IRAS mission was a collaboration between United States - NASA, Netherlands - Netherlands Agency for Aerospace Programmes (NIVR), and United Kingdom Science and Engineering Research Council - SERC. By ownership of satellite subsystems: NASA - optics, amplifying electronics, cryogenics, testing and launch. NIVR - satellite bus and processing electronics. SERC - mission operations and data acquisition. 4 General Major contractors: Ball Aerospace, Fokker Space and Hollandse Signaal. Launch date – 25 January, 1983 Launch site – SLC-2 West, Vandenberg AFB, CA Launch system – Delta 3910 Mass – 1083 kg Mission duration – 10 months 5 General cont. Type of orbit – sun-synchronous polar Orbit height – ~900 km Orbit period – ~100 minutes Current location – in orbit, deactivated Telescope style – Ritchey-Chretien Wavelength – infrared Mirror diameter – 0.57m Focal length – 5.5m 6 Following in IRAS footsteps Following spectacular successes of the IRAS mission, last few decades have seen several additional surveyors of our universe in infrared: Infrared Space Observatory - 1995 Spitzer Space Telescope - 2003 AKARI Space Telescope - 2006 Herschel Space Observatory (ESA) - April 2009 7 Mission design All-sky survey in four infrared bands 8 Mission design cont. IRAS mission design and survey strategy were optimized for maximally reliable detection of point sources. An all-sky survey was done at wavelengths ranging from 8 to 120 microns in four broadband photometric channels Channels were centered at 12, 25, 60 and 100 microns. Searches of rejected sources for moving objects led to discovery of three asteroids, six comets and a huge dust trail of comet Tempel 2. 9 Mission design cont. -
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