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Astronomie in Theorie Und Praxis 8. Auflage in Zwei Bänden Erik Wischnewski
Astronomie in Theorie und Praxis 8. Auflage in zwei Bänden Erik Wischnewski Inhaltsverzeichnis 1 Beobachtungen mit bloßem Auge 37 Motivation 37 Hilfsmittel 38 Drehbare Sternkarte Bücher und Atlanten Kataloge Planetariumssoftware Elektronischer Almanach Sternkarten 39 2 Atmosphäre der Erde 49 Aufbau 49 Atmosphärische Fenster 51 Warum der Himmel blau ist? 52 Extinktion 52 Extinktionsgleichung Photometrie Refraktion 55 Szintillationsrauschen 56 Angaben zur Beobachtung 57 Durchsicht Himmelshelligkeit Luftunruhe Beispiel einer Notiz Taupunkt 59 Solar-terrestrische Beziehungen 60 Klassifizierung der Flares Korrelation zur Fleckenrelativzahl Luftleuchten 62 Polarlichter 63 Nachtleuchtende Wolken 64 Haloerscheinungen 67 Formen Häufigkeit Beobachtung Photographie Grüner Strahl 69 Zodiakallicht 71 Dämmerung 72 Definition Purpurlicht Gegendämmerung Venusgürtel Erdschattenbogen 3 Optische Teleskope 75 Fernrohrtypen 76 Refraktoren Reflektoren Fokus Optische Fehler 82 Farbfehler Kugelgestaltsfehler Bildfeldwölbung Koma Astigmatismus Verzeichnung Bildverzerrungen Helligkeitsinhomogenität Objektive 86 Linsenobjektive Spiegelobjektive Vergütung Optische Qualitätsprüfung RC-Wert RGB-Chromasietest Okulare 97 Zusatzoptiken 100 Barlow-Linse Shapley-Linse Flattener Spezialokulare Spektroskopie Herschel-Prisma Fabry-Pérot-Interferometer Vergrößerung 103 Welche Vergrößerung ist die Beste? Blickfeld 105 Lichtstärke 106 Kontrast Dämmerungszahl Auflösungsvermögen 108 Strehl-Zahl Luftunruhe (Seeing) 112 Tubusseeing Kuppelseeing Gebäudeseeing Montierungen 113 Nachführfehler -
Marcia Rieke Programs Subcommittee Chair Astro2010
Decadal Surveys: What Are They and Why Do They Matter? Marcia Rieke Programs Subcommittee Chair Astro2010 What Are Decadal Surveys? • In the 1960s, astronomers realized 1st Survey that their aspirations required so in 1964 much federal funding that some type of assessment and recommendations were needed • Initially only astronomers did this 1982 and now all of the disciplines in space science conduct surveys with some participation from other agencies 1991 • Surveys and “CATE” are congressionally mandated 1972 2001 2010 2 U.S. Decadal Surveys -1 • 1964: Ground-based Astronomy: A Ten Year Program (Whitford) QSOs had just been discovered -- resulted in construction of CTIO 4-meter • 1972: Astronomy and Astrophysics for the 1970s (Greenstein) Astronomy satellites used to discover X-ray emission from stars -- resulted in construction of the VLA, HEAOs, and development work for HST • 1982: Astronomy and Astrophysics for the 1980s (Field) Many galaxies observed to produce large amounts of IR emission -- resulted in construction of Chandra and VLBI -- for future study: “Long-duration space flights of IR telescopes cooled to cryogenic temperatures” 3 U.S. Decadal Surveys -2 • 1991: The Decade of Discovery in Astronomy and Astrophysics (Bahcall) Existence of dark matter demonstrated -- resulted in construction of Spitzer, SOFIA, Gemini • 2001: Astronomy and Astrophysics in the New Millennium (McKee-Taylor) First exo-planets discovered, first evidence of dark energy seen -- resulted in development of JWST (and reassessment of how to execute decadal surveys) • 2010: New Worlds, New Horizons [“Astro2010”] (Blandford) First direct images of exo-planets, GRB afterglows observed, SMBHs in nuclei of virtually all galaxiex -- resulted in construction start for LSST, work on WFIRST Astro2010 Executive Committee Why There Are Decadal Surveys Astronomers want to do more than the federal budget can support: Once this fact is acknowledged, then the discussion turns to who should decide what is to be done, what are the rules and criteria. -
LIGO SCIENTIFIC COLLABORATION VIRGO COLLABORATION the LSC
LIGO SCIENTIFIC COLLABORATION VIRGO COLLABORATION Document Type LIGO–T1100322 VIR-0353A-11 The LSC-Virgo white paper on gravitational wave data analysis Science goals, status and plans, priorities (2011–2012 edition) The LSC-Virgo Data Analysis Working Groups, the Data Analysis Software Working Group, the Detector Characterization Working Group and the Computing Committee WWW: http://www.ligo.org/ and http://www.virgo.infn.it Processed with LATEX on 2011/10/13 LSC-Virgo data analysis white paper Contents 1 Introduction 6 2 The characterization of the data 8 2.1 LSC-Virgo-wide detector characterization priorities . .8 2.2 LIGO Detector Characterization . .9 2.2.1 Introduction . .9 2.2.2 Preparing for the Advanced Detector Era . 10 2.2.3 Priorities for LIGO Detector Characterization . 11 2.2.4 Data Run Support . 11 2.2.5 Software Infrastructure . 12 2.2.6 Noise Transients . 14 2.2.7 Spectral Features . 15 2.2.8 Calibration . 16 2.2.9 Timing . 17 2.3 GEO Detector Characterization . 18 2.3.1 Introduction . 18 2.3.2 Transient Studies . 19 2.3.3 Stationary Studies . 20 2.3.4 Stability Studies . 21 2.3.5 Calibration . 21 2.3.6 Resources . 22 2.4 Virgo Detector Characterization . 22 2.4.1 Introduction . 22 2.4.2 Calibration and h-reconstruction . 23 2.4.3 Environmental noise . 24 2.4.4 Virgo Data Quality and vetoes . 26 2.4.5 Monitoring Tools . 28 2.4.6 Noise monitoring tools . 29 2.4.7 The Virgo Data Base . 31 2.4.8 Virgo detector characterization next steps . -
Reach Your Ideal Chemistry Candidate in Print, Online and on Social Media
Reach your ideal chemistry candidate in print, online and on social media. Visit newscientistjobs.com and connect with thousands of chemistry professionals the easy way Contact us on 617-283-3213 or [email protected] STUPID ECONOMICS Why we’re hardwired to misunderstand finance PEA MILK, ANYONE? The non-dairy dairy explosion DITCHING DNA A brand new molecule for life WEEKLY September 22 – 28, 2018 THE MYSTERY OF THE UNIVERSE IN 10 OBJECTS Understand them, and we’ll understand everything Supermassive black holes Polystyrene planets Big bang afterglow Exploding dwarfs Superfast flashes Naked galaxies Monster stars No3196 US$6.99 CAN$6.99 38 and more... Science and technology news www.newscientist.com 0 72440 30690 5 US jobs in science THE WEIRDEST DINOSAUR Almost a bird, almost a whale – meet Spinosaurus PLUS NEW SCIENTIST ASKS THE PUBLIC: Our exclusive survey of attitudes to science Headlines grab attention, but only details inform. For over 28 years, that’s how Orbis has invested. By digging deep into a company’s fundamentals, we find value others miss. And by ignoring short-term market distractions, we’ve remained focused on long-term performance. For more details, ask your financial adviser or visit Orbis.com As with all investing, your capital is at risk. Past performance is not a reliable indicator of future results. Avoid distracting headlines Orbis Investments (U.K.) Limited is authorised and regulated by the Financial Conduct Authority SUBSCRIPTION OFFER More ideas... more discoveries... and now even more value SAVE 77% AND GET A FREE BOOK WORTH $35 “A beautifully produced book which gives an excellent overview of just what makes us tick” Subscribe today PRINT + APP + WEB HOW TO BE HUMAN Weekly magazine delivered to your door + Take a tour around the human body and brain + full digital access to the app and web in the ultimate guide to your amazing existence. -
A COMPREHENSIVE STUDY of SUPERNOVAE MODELING By
A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING by Chengdong Li BS, University of Science and Technology of China, 2006 MS, University of Pittsburgh, 2007 Submitted to the Graduate Faculty of the Dietrich School of Arts and Sciences in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Pittsburgh 2013 UNIVERSITY OF PITTSBURGH PHYSICS AND ASTRONOMY DEPARTMENT This dissertation was presented by Chengdong Li It was defended on January 22nd 2013 and approved by John Hillier, Professor, Department of Physics and Astronomy Rupert Croft, Associate Professor, Department of Physics Steven Dytman, Professor, Department of Physics and Astronomy Michael Wood-Vasey, Assistant Professor, Department of Physics and Astronomy Andrew Zentner, Associate Professor, Department of Physics and Astronomy Dissertation Director: John Hillier, Professor, Department of Physics and Astronomy ii Copyright ⃝c by Chengdong Li 2013 iii A COMPREHENSIVE STUDY OF SUPERNOVAE MODELING Chengdong Li, PhD University of Pittsburgh, 2013 The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important both in astrophysics and cosmology. While tremendous progress towards an understanding of SNe has been made, there are still many unanswered questions. The goal of this thesis is to study the evolution of massive stars, both before and after explosion. In the case of SNe, we synthesize supernova light curves and spectra by relaxing two assumptions made in previous investigations with the the radiative transfer code cmfgen, and explore the effects of these two assumptions. Previous studies with cmfgen assumed γ-rays from radioactive decay deposit all energy into heating. However, some of the energy excites and ionizes the medium. -
Supernova 2007Bi As a Pair-Instability Explosion
doi: 10.1038/nature08579 SUPPLEMENTARY INFORMATION Supplementary Information (1) Technical observational details Photometry: Discovery and follow-up observations of SN 2007bi were obtained using the Palomar- QUEST camera mounted on the 48-inch Oschin Schmidt telescope at Palomar Observa- tory (P48) as part of the SN Factory (SNF) program[31]. These R-band observations were pipeline-reduced by the SNF software, including bias removal, flatfield corrections, and an astrometric solution. Observations using the robotic 60-inch telescope at Palomar Observatory (P60) were pipeline-processed[32], including trimming, bias removal, flatfield corrections, and an as- trometric solution. Observations using the 200-inch Hale telescope at Palomar Observatory (P200) were obtained using the Large Format Camera (LFC) in SDSS r-band and were cross-calibrated onto the standard R band as detailed below. Observations by the Catalina Sky Survey (CSS[15]) were obtained using the CCD cam- era mounted on the 0.7 m Catalina telescope. These unfiltered data were cross-calibrated onto the R-band grid as detailed below. Synthetic photometry was derived from the late-time Keck spectrum using the meth- ods of ref. [33]. Table 3 provides the full list of photometric data. Spectroscopy: Early-time spectroscopy presented in Fig. 1[34] was obtained with the Low Resolution Imaging Spectrometer (LRIS[26]) mounted on the 10 m Keck I telescope on Mauna Kea, Hawaii. The presented spectrum was obtained on Apr. 16, 2007 in long-slit mode. The exposure time was 600 s at airmass 1.08 under clear sky conditions with variable seeing around 2��. The D560 dichroic was used with the 600 line mm−1 grism on the blue side, and the 400 line mm−1 grating blazed at 8500 A˚ on the red side, with the 1.5�� slit oriented at the parallactic angle[35]. -
January 2021 Newsletter
APS Division of In this issue Astrophysics • April Meeting Online • Upcoming DAP election alert Electronic Newsletter January 2021 • APS Fellows • Bethe Prize Winner • Student/Postdoc Travel Grants • April Meeting: DAP and Plenary Programs & Abstract Categories • Snowmass Update APS DAP Officers 2020–2021: Finalize your plans now to attend the April 2021 meeting held virtually this year. A • Chair: Glennys Farrar number of plenary and invited sessions will • Past Chair: Joshua Frieman feature presentations by DAP members. Here are the key details: • Chair Elect: Chris Fryer • Vice Chair: Daniel Holz What: April 2021 APS Meeting • Secretary/Treasurer: Judith Racusin When: April 17 - 20, 2021 • Deputy Sec./Treasurer: Amy Furniss Where: Online Abstract Deadline: Jan 8, 2021, 5 pm EST • Division Councilor: Cole Miller Travel Grant Deadline: Jan 31, 2021 • Member-at-Large: Stefano Profumo Early Registration Deadline: Feb 26, 2021 • Member-at-Large: Ignacio Taboada Late Registration Deadline: Mar 26, 2021 • Member-at-Large: Erin Kara • Member-at-Large: Laura Blecha The 2021 April Meeting will be virtual. Questions? Comments? Detailed information for the meeting, including details on registration and the scientific Newsletter editors: program can be found online at https://april.aps.org/ Amy Furniss [email protected] HEADS-UP: The ELECTION for next year’s DAP Executive Committee and chairline will Judith Racusin be held soon. Be on the lookout for the [email protected] announcement from APS, and please vote! 1 Dear DAP, Please see the January 2021 DAP newsletter below. It will be archived on the DAP website (https://www.aps.org/units/dap/newsletters/index.cfm). -
The Next Generation of Hydrodynamical Simulations of Galaxy Formation
HLRS Golden Spike Award 2016 The Next Generation of Hydrodynamical Simulations of Galaxy Formation Scientific background galaxies in clusters and the characteristics of Galaxies are comprised of up to several hundred hydrogen on large scales, and at the same time billion stars and display a variety of shapes and matched the metal and hydrogen content of sizes. Their formation involves a complicated galaxies on small scales. Indeed, the virtual uni- blend of astrophysics, including gravitational, verse created by Illustris resembles the real one hydrodynamical and radiative processes, as well so closely that it can be adopted as a powerful as dynamics in the enigmatic „dark sector“ of laboratory to further explore and characterize the Universe, which is composed of dark mat- galaxy formation physics. This is underscored ter and dark energy. Dark matter is thought to by the nearly 100 publications that have been consist of a yet unidentified elementary parti- written using the simulation thus far. cle, making up about 85% of all matter, whereas dark energy opposes gravity and has induced However, the Illustris simulation also showed an accelerated expansion of the Universe in the some tensions between its predictions and recent past. Because the governing equations observations of the real Universe, calling for both, are too complicated to be solved analytically, improvements in the physical model as well as numerical simulations have become a primary in the numerical accuracy and size of the simu- tool in theoretical astrophysics to study cosmic lations used to represent the cosmos. For exam- structure formation. Such calculations connect ple, one important physical ingredient that was the comparatively simple initial state left behind missing are magnetic fields. -
Bruce Winstein 1943–2011
Bruce Winstein 1943–2011 A Biographical Memoir by Melvyn J. Shochet and Michael S. Turner ©2016 National Academy of Sciences. Any opinions expressed in this memoir are those of the authors and do not necessarily reflect the views of the National Academy of Sciences. BRUCE daRRELL WINSTEIN September 25, 1943–February 28, 2011 Elected to the NAS, 1995 Bruce D. Winstein began his career as an experimental high-energy physicist and became renowned for making the most precise measurements of CP (“charge parity”) violation in the neutral K meson system. His results illu- minated the tiny asymmetry between matter and anti- matter that is essential for the existence of matter in the universe. He was associated with the University of Chicago from 1972 until his death in 2011, first as a senior research associate and finally as the Samuel K. Allison Distinguished Service Professor. Late in his career Winstein became a cosmologist, focusing on the polar- ization of the cosmic microwave background (CMB) radiation. Bringing to cosmology the techniques from By Melvyn J. Shochet high-energy physics, he made highly accurate measure- and Michael S. Turner ments of CMB polarization. Winstein was also instru- mental in establishing the Kavli Institute for Cosmo- logical Physics at the University of Chicago. Outside of physics, he was an avid fan of avant-garde film, twice teaching a course on the films of Michelangelo Antonioni. Early years Bruce was born in Los Angeles, CA, to Saul and Sylvia Winstein. His father was a distinguished physical organic chemist, elected to the National Academy of Sciences in 1955 and a faculty member at UCLA from 1941 until his death in 1969. -
Astro2010 Progress Report
Astro2010 Progress Report Roger Blandford KIPAC Stanford Chair, Astro2010 (http://sites.nationalacademies.org/bpa/BPA_049810) Overview The three pillars of the survey Astro2010: Science Frontiers Astro2010: State of the Profession / Infrastructure Astro2010: Activities / Program Prioritization Some features of Astro2010 Unprecedented community buy in to process Include unstarted projects from AANM Improved cost, readiness, risk assessment Increased international and private collaboration Changing economic political background HEPAP 22 v 2009 2 Executive Committee, NRC Staff . Roger Blandford Chair, Astro 2010 . Martha Haynes Chair, Science . John Huchra . Marcia Rieke . Lynne Hillenbrand . NRC: Staff Michael Moloney. BPA/SSB Liaison Responsibility for managing process, communicating with community 7 bulletins HEPAP 22 v 2009 Committee on Astro2010 Roger Blandford, Chair, Stanford University Lynne Hillenbrand, Executive Officer, California Institute of Technology Subcommittee on Science Martha P. Haynes, Vice Chair – Science Frontiers, Cornell University Lars Bildsten, University of California, Santa Barbara John E. Carlstrom, The University of Chicago Fiona A. Harrison, California Institute of Technology Timothy M. Heckman, Johns Hopkins University Jonathan I. Lunine, University of Arizona Juri Toomre, University of Colorado at Boulder BPA, SSB Liaisons Scott D. Tremaine, Institute for Advanced Study DOE, NASA, NSF Subcommittee on State of the Profession John P. Huchra, Vice Chair – State of the Profession, Harvard-University Debra M. Elmegreen, Vassar College Joshua Frieman, Fermi National Accelerator Laboratory Robert C. Kennicutt, Jr., University of Cambridge Dan McCammon, University of Wisconsin-Madison Neil de Grasse Tyson, American Museum of Natural History Subcommittee on Programs Marcia J. Rieke, Vice Chair – Program Prioritization, University of Arizona Steven J. Battel, Battel Engineering Claire E. Max, University of California, Santa Cruz Steven M. -
David Stevenson the Complex Lives of Star Clusters Astronomers’ Universe
David Stevenson The Complex Lives of Star Clusters Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 David Stevenson The Complex Lives of Star Clusters David Stevenson Sherwood , UK ISSN 1614-659X ISSN 2197-6651 (electronic) Astronomers’ Universe ISBN 978-3-319-14233-3 ISBN 978-3-319-14234-0 (eBook) DOI 10.1007/978-3-319-14234-0 Library of Congress Control Number: 2015936043 Springer Cham Heidelberg New York Dordrecht London © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specifi c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made. Cover photo of the Orion Nebula M42 courtesy of NASA Spitzer Printed on acid-free paper Springer International Publishing AG Switzerland is part of Springer Science+Business Media (www.springer.com) For my late mother, Margaret Weir Smith Stevenson Pref ace Stars are fairly social beasts. -
The University of Chicago Astronomy and Cosmology
THE UNIVERSITY OF CHICAGO ASTRONOMY AND COSMOLOGY WITH GRAVITATIONAL WAVES A DISSERTATION SUBMITTED TO THE FACULTY OF THE DIVISION OF THE PHYSICAL SCIENCES IN CANDIDACY FOR THE DEGREE OF DOCTOR OF PHILOSOPHY DEPARTMENT OF ASTRONOMY & ASTROPHYSICS BY MAYA FISHBACH CHICAGO, ILLINOIS AUGUST 2020 Copyright c 2020 by Maya Fishbach All Rights Reserved לאמא ואבא To my parents TABLE OF CONTENTS LIST OF FIGURES . vii ACKNOWLEDGMENTS . xv ABSTRACT . xvi 1 INTRODUCTION . 1 2 ARE LIGO'S BLACK HOLES MADE FROM SMALLER BLACK HOLES? . 5 2.1 Abstract . .6 2.2 Introduction . .7 2.3 Methods . 10 2.3.1 Hierarchical Merger Spin Distribution . 10 2.3.2 Mixture Model Analysis . 14 2.4 Results . 20 2.5 Conclusion . 24 3 WHERE ARE LIGO'S BIG BLACK HOLES? . 25 3.1 Abstract . 26 3.2 Introduction . 27 3.3 Sensitive volume . 31 3.4 Fitting the Mass Distribution . 34 3.5 Results . 38 3.5.1 Non-detection of heavy BBHs . 38 3.5.2 Bayesian evidence in favor of mass gap . 40 3.5.3 Joint power law{maximum mass fit . 43 3.6 Discussion . 47 3.6.1 Effect of Redshift Evolution . 47 3.6.2 Distribution of mass ratios . 48 3.6.3 Extending to non-power-law mass distributions . 49 3.6.4 Are there BBHs beyond the gap? . 49 3.7 Conclusion . 50 4 DOES THE BLACK HOLE MERGER RATE EVOLVE WITH REDSHIFT? . 52 4.1 Abstract . 53 4.2 Introduction . 54 4.3 Detected redshift distribution . 55 4.4 Joint Mass-redshift Model . 58 4.4.1 Redshift Model A .