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Packet Switched, General Purpose FPGA-Based Modules For
Peta-Flop Radio Astronomy Signal Processing and the CASPER Collaboration (and correlators too !) Dan Werthimer and 800 CASPER Collaborators http://casper.berkeley.edu Two Types of Signal Processing 1. Embarrassingly Parallel – Low Data Rates (record the data and process it later) (high computation per bit) 2. Real Time in-situ Processing Petabits per second (can not record data) TYPE 1 Embarrassingly Parallel – Low Data Rates (record the data and process it later) (high computation per bit) VOLUNTEER COMPUTING BOINC - Berkeley Open Infrastructure for Network Computing From Download Work Server Generator Arecibo Feeder Transitioner Shared Database Memory Purger MySQL Volunteers Scheduler Database File Deleter To Nobel Upload Validator Assimilator Server Prize Committee BERKELEY SETI RESEARCH CENTER BERKELEY ASTRONOMY CollaboratorsDEPARTMENT Berkeley SETI and Volunteer Computing Group David Anderson, Hong Chen, Jeff Cobb, Matt Dexter, Walt Fitelson, Eric Korpela, Matt Lebofsky, Geoff Marcy, David MacMahon, Eric Petigura, Andrew Siemion, Charlie Townes, Mark Wagner, Ed Wishnow, Dan Werthimer NSF , NASA, Individual Donors Agilent, Fujitsu, HP, Intel, Xilinx Arecibo Observatory High performance data storage silo UC Berkeley Space Sciences Lab Public Volunteers SETI@Home ✴ Polyphase Channelization ✴ Coherent Doppler Drift Search ✴ Narrowband Pulse Search ✴ Gaussian Drift Search ✴ Autocorrelation ✴ <insert your algorithm here> SETI@home Statistics TOTAL RATE 8,464,550 2,000 per day participants (in 226 countries) 3 million years 1,000 years -
Variable Stars Observer Bulletin
Amateurs' Guide to Variable Stars September-October 2013 | Issue #2 Variable Stars Observer Bulletin ISSN 2309-5539 Twenty new W Ursae Majoris-type eclipsing binaries from the Catalina Sky Survey Details for 20 new WUMa systems are presented, along with a preliminary The FU Orionis phenomenon model of the FU Orionis stars are pre-main-sequence totally eclipsing eruptive variables which appear to be a system GSC stage in the development of T Tauri 03090-00153. stars. Image: FU Orionis. Credit: ESO NSVS 5860878 = Dauban V 171 Carbon in the sky: A new Mira variable in Cygnus a few remarkable carbon stars The list of the most interesting and bright carbon stars for northern observers is presented. Right: TT Cygni. A carbon star. Credit & Copyright: H.Olofsson (Stockholm Nova Observatory) et al. Delphini 2013 Nova has reached magnitude 4.3 visual The "Heavenly Owl" on August 16 observatory: seeing above the Black Sea waterfront VS-COMPAS Project: variable stars research and data mining. More at http://vs-compas.belastro.net Variable Stars Observer Bulletin Amateurs' Guide to Variable Stars September-October 2013 | Issue #2 C O N T E N T S 04 NSVS 5860878 = Dauban V 171: a new Mira variable in Cygnus by Ivan Adamin, Siarhey Hadon A new Mira variable in the constellation of Cygnus is presented. The variability of the NSVS 5860878 source was detected in January of 2012. Lately, the object was identified as the Dauban V171. A revision is submitted to the VSX. 06 Twenty new W Ursae Majoris-type eclipsing binaries Credit: Justin Ng from the Catalina Sky Survey by Stefan Hümmerich, Klaus Bernhard, Gregor Srdoc 16 Nova Delphini 2013: a naked-eye visible flare in A short overview of eclipsing binary northern skies stars and their traditional by Andrey Prokopovich classification scheme is given, which concentrates on W Ursae Majoris On August 14, 2013 a new bright star (WUMa)-type systems. -
Supervisor R
Optical and Near-In&ared Photometry of Old Galactic Clusters by Joanne Mcirie Rosvick B.Sc., University of Alberta, 1987 M.Sc., University of Victoria, 1990 A Dissertation Submitted in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY in the Department of Physics and Astronomy We accept this dissertation as conforming to the required standaird Dr. C. D. , Supervisor r. T. J. Davidge, Supervisor Dr. F. D. A. Héirtwick, Dr. D. A. VandMBerg, Departmental Member Departmental Member Dr. A. C. Gower, Departmental Member Dr. P. Wan, Outside Member Dr. E. D. Friel, External Examiner ©Joaime Marie Rosvick, 1996 University of Victoria All rights reserved. This dissertation may not be reproduced in whole or in part, by photocopying or other means, without the permission of the author. u Abstract Supervisors: Dr. C. D. Scarfe, Dr. T. J. Davidge The open clusters NGC 2141, NGC 6791, NGC 6819 and NGC 7142, all suspected of having ages greater than 2 billion years (Gyr), were ob served at optical and near-in&ared wavelengths. The images were reduced using standard IRAF routines, and magnitudes for the stars were determined using DAOPHOT (Stetson, 1987). These data were used to construct colour- magnitude diagrams (CMDs) for each cluster, as well as two-colour diagreims {J - K , V - K), {J -H ,H -K ) of the giants. Colour excesses were redetermined by comparing the optical CMD main sequences to semi-empirical ZAMS calibrations (VeindenBerg and PoU, 1989; this work) and are as follows: E{B — V) = 0.32 ± 0.04, 0.23 ± 0.03, 0.11 ± 0.03 and 0.29 ± 0.04, for NGC 2141, NGC 6791, NGC 6819 and NGC 7142, respectively. -
Tesi Di Laurea La Solidarietà Digitale
Tesi di Laurea La Solidarietà Digitale Da Seti@home a Boinc. Ipotesi di una società dell’elaborazione. di Francesco Morello 1 INDICE Introduzione............................................................... 4 Capitolo I Calcolo Vontario....................................... 5 1.1 Dai media di massa al calcolo distribuito......... 5 1.2 Calcolo Distribuito............................................... 6 1.3 Calcolo Volontario............................................... 8 1.3.1 Come funziona il calcolo volontario ?.......... 10 1.3.2 Applicazioni del Calcolo Volontario.............. 11 Capitolo II Analisi di BOINC.................................... 23 2.1 Piattaforma per il calcolo volontario............... 23 2.2 Architettura di BOINC........................................ 25 2.2.1 L'interfaccia di BOINC.................................... 25 2.2.2 Progetti e Volontari......................................... 31 2.2.3 Checkpointing e Work unit............................ 32 2.2.4 Crediti e ridondanza....................................... 32 2.2.5 Gli scopi di BOINC.......................................... 33 Capitolo III Aspetti tecnici del calcolo distribuito 36 3.1 Grid Computing vs Volunteer Computing....... 36 3.2 Hardware e Software per il Distributed Computing38 3.2.1 La Playstation 3 per raggiungere il Petaflop.41 Capitolo IV Aspetti sociali del calcolo volontario 45 4.1 Riavvicinarci alla scienza.................................. 45 2 4.2 Volontari oltre la CPU........................................ 47 4.2.1 Forum, Blog -
Ira Sprague Bowen Papers, 1940-1973
http://oac.cdlib.org/findaid/ark:/13030/tf2p300278 No online items Inventory of the Ira Sprague Bowen Papers, 1940-1973 Processed by Ronald S. Brashear; machine-readable finding aid created by Gabriela A. Montoya Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 © 1998 The Huntington Library. All rights reserved. Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague 1 Bowen Papers, 1940-1973 Observatories of the Carnegie Institution of Washington Collection Inventory of the Ira Sprague Bowen Paper, 1940-1973 The Huntington Library San Marino, California Contact Information Manuscripts Department The Huntington Library 1151 Oxford Road San Marino, California 91108 Phone: (626) 405-2203 Fax: (626) 449-5720 Email: [email protected] URL: http://www.huntington.org/huntingtonlibrary.aspx?id=554 Processed by: Ronald S. Brashear Encoded by: Gabriela A. Montoya © 1998 The Huntington Library. All rights reserved. Descriptive Summary Title: Ira Sprague Bowen Papers, Date (inclusive): 1940-1973 Creator: Bowen, Ira Sprague Extent: Approximately 29,000 pieces in 88 boxes Repository: The Huntington Library San Marino, California 91108 Language: English. Provenance Placed on permanent deposit in the Huntington Library by the Observatories of the Carnegie Institution of Washington Collection. This was done in 1989 as part of a letter of agreement (dated November 5, 1987) between the Huntington and the Carnegie Observatories. The papers have yet to be officially accessioned. Cataloging of the papers was completed in 1989 prior to their transfer to the Huntington. -
Cygnus OB2 – a Young Globular Cluster in the Milky Way Jürgen Knödlseder
Cygnus OB2 – a young globular cluster in the Milky Way Jürgen Knödlseder To cite this version: Jürgen Knödlseder. Cygnus OB2 – a young globular cluster in the Milky Way. Astronomy and Astrophysics - A&A, EDP Sciences, 2000, 360, pp.539 - 548. hal-01381935 HAL Id: hal-01381935 https://hal.archives-ouvertes.fr/hal-01381935 Submitted on 14 Oct 2016 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. Astron. Astrophys. 360, 539–548 (2000) ASTRONOMY AND ASTROPHYSICS Cygnus OB2–ayoung globular cluster in the Milky Way J. Knodlseder¨ INTEGRAL Science Data Centre, Chemin d’Ecogia 16, 1290 Versoix, Switzerland Centre d’Etude Spatiale des Rayonnements, CNRS/UPS, B.P. 4346, 31028 Toulouse Cedex 4, France ([email protected]) Received 31 May 2000 / Accepted 23 June 2000 Abstract. The morphology and stellar content of the Cygnus particularly good region to address such questions, since it is OB2 association has been determined using 2MASS infrared extremely rich (e.g. Reddish et al. 1966, hereafter RLP), and observations in the J, H, and K bands. The analysis reveals contains some of the most luminous stars known in our Galaxy a spherically symmetric association of ∼ 2◦ in diameter with (e.g. -
Astronomy and Astrophysics Report for 2016
Astronomy and Astrophysics Report for 2016 Submitted to the Governing Board at its meeting on 1st March 2017 1.Research output and activities The primary research output of the section consists of peer-reviewed publications in the leading astronomical and astrophysical journals. The section has a green open-access publishing policy whereby all publications are placed as preprints on the freely accessible arXiv server. To this end DIAS supports arXiv with a modest financial contribution. During the calendar year seventy three papers were published, or posted as preprints on arXiv, and with at least one co-author from the section as well as six non-refereed papers. Full details can be found in the detailed bibliography at the end of this report (which replaces the former summary text). In some ways what is more interesting than the raw number of papers is the trend over time which shows considerable year on year fluctuations, but no major change over the last decade. Refereed Preprints Non-refereed 160 120 80 40 0 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 Note that pre 2010 preprints were classified as non-refereed and not treated as a separate category. In addition to research papers, talks and conference presentations are an important means of communicating our research to our peers and a useful measure of the esteem in which we are held. During the year the following were delivered. Felix Aharonian: 1. Rome, Italy, workshop “Towards a large field-of-view TeV experiment” (14.01-15.01.2016) Evidence for a PeVatron in the Galactic Center: is it Sgr A*? 2. -
POSTERS SESSION I: Atmospheres of Massive Stars
Abstracts of Posters 25 POSTERS (Grouped by sessions in alphabetical order by first author) SESSION I: Atmospheres of Massive Stars I-1. Pulsational Seeding of Structure in a Line-Driven Stellar Wind Nurdan Anilmis & Stan Owocki, University of Delaware Massive stars often exhibit signatures of radial or non-radial pulsation, and in principal these can play a key role in seeding structure in their radiatively driven stellar wind. We have been carrying out time-dependent hydrodynamical simulations of such winds with time-variable surface brightness and lower boundary condi- tions that are intended to mimic the forms expected from stellar pulsation. We present sample results for a strong radial pulsation, using also an SEI (Sobolev with Exact Integration) line-transfer code to derive characteristic line-profile signatures of the resulting wind structure. Future work will compare these with observed signatures in a variety of specific stars known to be radial and non-radial pulsators. I-2. Wind and Photospheric Variability in Late-B Supergiants Matt Austin, University College London (UCL); Nevyana Markova, National Astronomical Observatory, Bulgaria; Raman Prinja, UCL There is currently a growing realisation that the time-variable properties of massive stars can have a funda- mental influence in the determination of key parameters. Specifically, the fact that the winds may be highly clumped and structured can lead to significant downward revision in the mass-loss rates of OB stars. While wind clumping is generally well studied in O-type stars, it is by contrast poorly understood in B stars. In this study we present the analysis of optical data of the B8 Iae star HD 199478. -
Collisional Modelling of the AU Microscopii Debris Disc
A&A 581, A97 (2015) Astronomy DOI: 10.1051/0004-6361/201525664 & c ESO 2015 Astrophysics Collisional modelling of the AU Microscopii debris disc Ch. Schüppler1, T. Löhne1, A. V. Krivov1, S. Ertel2, J. P. Marshall3;4, S. Wolf5, M. C. Wyatt6, J.-C. Augereau7;8, and S. A. Metchev9 1 Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany e-mail: [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 3 School of Physics, University of New South Wales, NSW 2052 Sydney, Australia 4 Australian Centre for Astrobiology, University of New South Wales, NSW 2052 Sydney, Australia 5 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24098 Kiel, Germany 6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 7 Université Grenoble Alpes, IPAG, 38000 Grenoble, France 8 CNRS, IPAG, 38000 Grenoble, France 9 University of Western Ontario, Department of Physics and Astronomy, 1151 Richmond Avenue, London, ON N6A 3K7, Canada Received 14 January 2015 / Accepted 12 June 2015 ABSTRACT AU Microscopii’s debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. -
The Constellation Microscopium, the Microscope Microscopium Is A
The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'. -
Modeling and Interpretation of the Ultraviolet Spectral Energy Distributions of Primeval Galaxies
Ecole´ Doctorale d'Astronomie et Astrophysique d'^Ile-de-France UNIVERSITE´ PARIS VI - PIERRE & MARIE CURIE DOCTORATE THESIS to obtain the title of Doctor of the University of Pierre & Marie Curie in Astrophysics Presented by Alba Vidal Garc´ıa Modeling and interpretation of the ultraviolet spectral energy distributions of primeval galaxies Thesis Advisor: St´ephane Charlot prepared at Institut d'Astrophysique de Paris, CNRS (UMR 7095), Universit´ePierre & Marie Curie (Paris VI) with financial support from the European Research Council grant `ERC NEOGAL' Composition of the jury Reviewers: Alessandro Bressan - SISSA, Trieste, Italy Rosa Gonzalez´ Delgado - IAA (CSIC), Granada, Spain Advisor: St´ephane Charlot - IAP, Paris, France President: Patrick Boisse´ - IAP, Paris, France Examinators: Jeremy Blaizot - CRAL, Observatoire de Lyon, France Vianney Lebouteiller - CEA, Saclay, France Dedicatoria v Contents Abstract vii R´esum´e ix 1 Introduction 3 1.1 Historical context . .4 1.2 Early epochs of the Universe . .5 1.3 Galaxytypes ......................................6 1.4 Components of a Galaxy . .8 1.4.1 Classification of stars . .9 1.4.2 The ISM: components and phases . .9 1.4.3 Physical processes in the ISM . 12 1.5 Chemical content of a galaxy . 17 1.6 Galaxy spectral energy distributions . 17 1.7 Future observing facilities . 19 1.8 Outline ......................................... 20 2 Modeling spectral energy distributions of galaxies 23 2.1 Stellar emission . 24 2.1.1 Stellar population synthesis codes . 24 2.1.2 Evolutionary tracks . 25 2.1.3 IMF . 29 2.1.4 Stellar spectral libraries . 30 2.2 Absorption and emission in the ISM . 31 2.2.1 Photoionization code: CLOUDY ....................... -
Arxiv:1704.01678V2 [Astro-Ph.GA] 28 Jul 2017 Been Notoriously Difficult, Resulting Mostly in Upper Lim- Highest Escape Fractions Measured to Date Among Low- Its (E.G
Submitted: 3 March 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 MRK 71 / NGC 2366: THE NEAREST GREEN PEA ANALOG Genoveva Micheva1, M. S. Oey1, Anne E. Jaskot2, and Bethan L. James3 (Accepted 24 July 2017) 1University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109-1107, USA 2Department of Astronomy, Smith College, Northampton, MA 01063, USA 3STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA ABSTRACT We present the remarkable discovery that the dwarf irregular galaxy NGC 2366 is an excellent analog of the Green Pea (GP) galaxies, which are characterized by extremely high ionization parameters. The similarities are driven predominantly by the giant H II region Markarian 71 (Mrk 71). We compare the system with GPs in terms of morphology, excitation properties, specific star-formation rate, kinematics, absorption of low-ionization species, reddening, and chemical abundance, and find consistencies throughout. Since extreme GPs are associated with both candidate and confirmed Lyman continuum (LyC) emitters, Mrk 71/NGC 2366 is thus also a good candidate for LyC escape. The spatially resolved data for this object show a superbubble blowout generated by mechanical feedback from one of its two super star clusters (SSCs), Knot B, while the extreme ionization properties are driven by the . 1 Myr-old, enshrouded SSC Knot A, which has ∼ 10 times higher ionizing luminosity. Very massive stars (> 100 M ) may be present in this remarkable object. Ionization-parameter mapping indicates the blowout region is optically thin in the LyC, and the general properties also suggest LyC escape in the line of sight.