Dr. Nithyanandan Thyagarajan
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Santa Cruz Summer Workshops in Astronomy and Astrophysics S.M
Santa Cruz Summer Workshops in Astronomy and Astrophysics S.M. Faber Editor Nearly Nonnal Galaxies From the Planck Time to the Present The Eighth Santa Cruz Summer Workshop in Astronomy and Astrophysies July 21-August 1, 1986, Liek Observatory With 133 Illustrations Springer-Verlag New York Berlin Heidelberg London Paris Tokyo S. M. Faber Department of Astronomy University of California Santa Cruz, CA 95064, USA Library of Congress Cataloging-in-Publication Data Santa Cruz Summer Workshop in Astronomy and Astrophysics (8th: 1986) Nearly normal galaxies. (Santa Cruz summer workshops in astrophysics) I. Galaxies-Congresses. 2. Astrophysics- Congresses. I. Faber, Sandra M. 11. Title. 111. Series. Q8856.S26 1986 523.1' 12 87-9559 © 1987 by Springer-Verlag New York Inc. Softcover reprint ofthe hardcover 1st edition 1987 All rights reserved. This work may not be translated or copied in whole or in part without the written permission ofthe publisher (Springer-Verlag, 175 Fifth Avenue, New York, New York 10010, USA), except for bI1ef excerpts in connection with reviews or scholarly analysis. U se in connection with any form of information storage and retrieval. electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed is forbidden. The use of general descriptive names, trade names, trademarks, etc. in this publication, even if the former are not especially identified, is not to be taken as a sign that such names, as understood by the Trade Marks and Merchandise Marks Act, may accordingly be used freely by anyone. Permission to photocopy for internal or personal use, or the internal or personal use of specific c1ients, is granted by Springer-Verlag New York Inc. -
Observing Summary 1991 Statistics
NATIONAL RADIO S U M M A R Y ASTRONOMY OBSERVATORY 1991 STATISTICS Cover: The peculiar galaxy NGC 7252. This galaxy is a result of a recent merger, or collision, of two galaxies. The starlight from the merged galaxy is shown as red in this image, light from stars scattered by the force of the collision, or stars unrelated to the galaxy, is shown as green and the radio emission from neutral atomic hydrogen gas is indicated by blue shading. This image demonstrates that when galaxies collide their gas is removed; the final merged system is nearly devoid of gas. The radio image was made with the NRAO Very Large Array radio telescope. The optical image was obtained at the CTIO 4m telescope. VLA Observers: John Hibbard Jacqueline van Gorkom Linda Schweizer NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary 1991 Statistics February 1992 SOME HIGHLIGHTS OF THE 1991 RESEARCH PROGRAM The 12 m telescope has been used to detect CO in by far the most distant object to date-the diffuse galaxy IRAS10214+4724, whose optical redshift is 2.29. At so high a redshift, the infrared emission corresponds to a luminosity as great as that of the most luminous QSOs, about 1014 solar luminosities, which if thermal dust emission, correspond to 1010 solar masses of dust. Such a large amount of dust is expected to be accompanied by a still larger mass of (molecular) gas. The CO J=3-2 transition which was detected at the 12 m is shifted from its usual frequency of 345 GHz to 105 GHz, and its 4 mK intensity and 400 km/s width correspond to nearly 1012 solar masses of molecular gas. -
Report and Recommendation of the SKA Site Advisory Committee (SSAC)
Report and Recommendation of the SKA Site Advisory Committee (SSAC) 16 February 2012 James M. Moran, Chair Subramaniam Ananthakrishnan Jacob W.M. Baars Jocelyn Bell Burnell Willem N. Brouw Ian Corbett James Crocker Thomas Garvin Stefan Michalowski Ernest R. Seaquist Peter Tindemans Jacqueline van Gorkom Roger J. Brissenden, Executive Secretary Table of Contents 1. Executive Summary ............................................................................................................. 3 2. Introduction ........................................................................................................................... 5 3. SSAC Processes, Time Line, and Materials .................................................................. 7 3.1 Evaluation Process ...................................................................................................................... 7 3.2 Decision-Making Process .......................................................................................................... 9 3.3 Scoring Process ............................................................................................................................ 9 3.4 Time Line of All Discussions and Meetings ..................................................................... 11 3.5 Information Received and Considered ............................................................................. 13 4. Findings and Conclusions ............................................................................................... 14 4.1 Science and -
Imaging SKA-Scale Data in Three Different Computing Environments
Imaging SKA-Scale data in three different computing environments Richard Dodsona,∗, Kevin Vinsena, Chen Wua, Attila Poppingb, Martin Meyera, Andreas Wiceneca, Peter Quinna, Jacqueline van Gorkomc, Emmanuel Momjiand aInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, M468, 35 Stirling Highway, Crawley, Perth, WA 6009, Australia bAustralian Research Council, Centre of Excellence for All-sky Astrophysics (CAASTRO) cDepartment of Astronomy, Columbia University, Mail Code 5246, 550 West 120th Street, New York, New York 10027, USA dNational Radio Astronomy Observatory, 1003 Lopezville Rd., P. O. Box O, Socorro, NM 87801, USA Abstract We present the results of our investigations into options for the computing platform for the imaging pipeline in the chiles project, an ultra-deep HI pathfinder for the era of the Square Kilometre Array. chiles pushes the current computing infrastructure to its limits and understanding how to deliver the images from this project is clarifying the Science Data Processing requirements for the SKA. We have tested three platforms: a moderately sized cluster, a massive High Performance Computing (HPC) system, and the Amazon Web Services (AWS) cloud computing platform. We have used well-established tools for data reduction and performance measurement to investigate the behaviour of these platforms for the complicated access patterns of real-life Radio Astronomy data reduction. All of these platforms have strengths and weaknesses and the system tools allow us to identify and evaluate them in a quantitative manner. With the insights from these tests we are able to complete the imaging pipeline processing on both the HPC platform and also on the cloud computing platform, which paves the way for meeting big data challenges in the era of SKA in the field of Radio Astronomy.