Creating Updated, Scientifically-Calibrated Mosaic Images for the Rc3 Catalogue
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Guide Avancé D'écriture Des Scripts Bash
Guide avancé d'écriture des scripts Bash Une exploration en profondeur de l'art de la pro- grammation shell Mendel Cooper Guide avancé d'écriture des scripts Bash: Une exploration en profondeur de l'art de la programmation shell Mendel Cooper 5.3 Publié le 11 mai 2008 Résumé Ce tutoriel ne suppose aucune connaissance de la programmation de scripts, mais permet une progression rapide vers un niveau in- termédiaire/avancé d'instructions tout en se plongeant dans de petites astuces du royaume d'UNIX®. Il est utile comme livre, comme manuel permettant d'étudier seul, et comme référence et source de connaissance sur les techniques de programmation de scripts. Les exercices et les exemples grandement commentés invitent à une participation active du lecteur avec en tête l'idée que la seule façon pour vraiment apprendre la programmation de scripts est d'écrire des scripts. Ce livre est adapté à une utilisation en classe en tant qu'introduction générale aux concepts de la programmation. La dernière mise à jour de ce document, comme une « archive tar » compressée avec bzip2 incluant à la fois le source SGML et le HTML généré, peut être téléchargée à partir du site personnel de l'auteur. Une version PDF est aussi disponible (site miroir du PDF). Voir le journal des modifications pour un historique des révisions. Dédicace Pour Anita, la source de toute magie i Part 1. Introduction .......................................................................................................................................... 1 1. Pourquoi la programmation -
Sustaining the Montage Image Mosaic Engine Since 2002
PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie 6XVWDLQLQJWKH0RQWDJHLPDJH PRVDLFHQJLQHVLQFH *%UXFH%HUULPDQ-RKQ&*RRG *%UXFH%HUULPDQ-RKQ&*RRG6XVWDLQLQJWKH0RQWDJHLPDJHPRVDLF HQJLQHVLQFH3URF63,(6RIWZDUHDQG&\EHULQIUDVWUXFWXUHIRU $VWURQRP\9 -XO\ GRL (YHQW63,($VWURQRPLFDO7HOHVFRSHV,QVWUXPHQWDWLRQ$XVWLQ7H[DV 8QLWHG6WDWHV 'RZQORDGHG)URPKWWSVZZZVSLHGLJLWDOOLEUDU\RUJFRQIHUHQFHSURFHHGLQJVRIVSLHRQ7HUPVRI8VHKWWSVZZZVSLHGLJLWDOOLEUDU\RUJWHUPVRIXVH Sustaining the Montage Image Mosaic Engine Since 2002 G. Bruce Berriman*a, John C. Gooda a Caltech/IPAC-NExScI, 1201 East California Blvd., Pasadena, CA 91125, USA ABSTRACT This paper describes how we have sustained the Montage image mosaic engine (http://montage.ipac.caltech.edu) first released in 2002, to support the ever-growing scale and complexity of modern data sets. The key to its longevity has been its design as a toolkit written in ANSI-C, with each tool performing one distinct task, for easy integration into scripts, pipelines and workflows. The same code base now supports Windows, JavaScript and Python by taking advantage of recent advances in compilers. The design has led to applicability of Montage far beyond what was anticipated when Montage was first built, such as supporting observation planning for the JWST. Moreover, Montage is highly scalable and is in wide use within the IT community to develop advanced, fault-tolerant cyber-infrastructure, such as job schedulers for grids, workflow orchestration, and restructuring techniques for processing complex workflows and pipelines. Keywords: image processing, software toolkits, software engineering, software sustainability, image mosaics, astronomy imaging. 1. INTRODUCTION The Montage image mosaic engine is entering its sixteenth year of support to the astrophysics and IT communities. The mosaics created by Montage are intended for scientific analysis: they preserve the calibration and astrometric fidelity of the original images, and rectify the highly variable sky background to a common level across all the original images1. -
Galaxies with Rows A
Astronomy Reports, Vol. 45, No. 11, 2001, pp. 841–853. Translated from Astronomicheski˘ı Zhurnal, Vol. 78, No. 11, 2001, pp. 963–976. Original Russian Text Copyright c 2001 by Chernin, Kravtsova, Zasov, Arkhipova. Galaxies with Rows A. D. Chernin, A. S. Kravtsova, A. V. Zasov, and V. P. Arkhipova Sternberg Astronomical Institute, Universitetskii˘ pr. 13, Moscow, 119899 Russia Received March 16, 2001 Abstract—The results of a search for galaxies with straight structural elements, usually spiral-arm rows (“rows” in the terminology of Vorontsov-Vel’yaminov), are reported. The list of galaxies that possess (or probably possess) such rows includes about 200 objects, of which about 70% are brighter than 14m.On the whole, galaxies with rows make up 6–8% of all spiral galaxies with well-developed spiral patterns. Most galaxies with rows are gas-rich Sbc–Scd spirals. The fraction of interacting galaxies among them is appreciably higher than among galaxies without rows. Earlier conclusions that, as a rule, the lengths of rows are similar to their galactocentric distances and that the angles between adjacent rows are concentrated near 120◦ are confirmed. It is concluded that the rows must be transient hydrodynamic structures that develop in normal galaxies. c 2001 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION images were reproduced by Vorontsov-Vel’yaminov and analyze the general properties of these objects. The long, straight features found in some galaxies, which usually appear as straight spiral-arm rows and persist in spite of differential rotation of the galaxy 2. THE SAMPLE OF GALAXIES disks, pose an intriguing problem. These features, WITH STRAIGHT ROWS first described by Vorontsov-Vel’yaminov (to whom we owe the term “rows”) have long escaped the To identify galaxies with rows, we inspected about attention of researchers. -
HPSEC-05.Pdf
A COMPARISON OF TWO METHODS FOR BUILDING ASTRONOMICAL IMAGE MOSAICS ON A GRID∗ DANIEL S. KATZ,† G. BRUCE BERRIMAN,‡ EWA DEELMAN,§ JOHN GOOD,‡ JOSEPH C. JACOB,† CARL KESSELMAN,§ ANASTASIA C. LAITY,‡ THOMAS A. PRINCE,¶ GURMEET SINGH,§ MEI-HUI SU§ Abstract. This paper compares two methods for running an application composed of a set of modules on a grid. The set of modules generates large astronomical image mosaics by composing multiple small images. This software suite is called Montage (http://montage.ipac.caltech.edu/). The workflow that describes a particular run of Montage can be expressed as a directed acyclic graph (DAG), or as a short sequence of parallel (MPI) and sequential programs. In the first case, Pegasus can be used to run the workflow. In the second case, a short shell script that calls each program can be run. In this paper, we discuss the Montage modules, the workflow run for a sample job, and the two methods of actually running the workflow. We examine the run time for each method and compare the portions that differ between the two methods. Key words. grid applications, performance, astronomy, mosaics Technical Areas. Network-Based/Grid Computing, Cluster Computing, Algorithms & Applications 1. Introduction. Many science data processing applications can be expressed as a sequence of tasks to be performed. In astronomy, one such application is building science-grade mosaics from multiple image data sets as if they were single images with a common coordinate system, map projection, etc. Here, the software must preserve the astrometric and photometric integrity of the original data, and rectify background emission from the sky or from the instrument using physically based models. -
Astronomical Image Mosaicking on a Grid: Initial Experiences∗ Daniel S
ASTRONOMICAL IMAGE MOSAICKING ON A GRID: INITIAL EXPERIENCES∗ DANIEL S. KATZ,† NATHANIEL ANAGNOSTOU,‡ G. BRUCE BERRIMAN,‡ EWA DEELMAN,§ JOHN GOOD,‡ JOSEPH C. JACOB,† CARL KESSELMAN,§ ANASTASIA LAITY,‡ THOMAS A. PRINCE,¶ GURMEET SINGH,§ MEI-HUI SU,§ ROY WILLIAMSk Abstract. This chapter discusses some grid experiences in solving the problem of generat- ing large astronomical image mosaics by composing multiple small images, from the team that has developed Montage (http://montage.ipac.caltech.edu/). The problem of generating these mosaics is complex in that individual images must be projected into a common coordinate space, overlaps between images calculated, the images processed so that the backgrounds match, and images com- posed while using a variety of techniques to handle the presence of multiple pixels in the same output space. To accomplish these tasks, a suite of software tools called Montage has been developed. The modules in this suite can be run on a single processor computer using a simple shell script, and can additionally be run using a combination of parallel approaches. These include running MPI versions of some modules, and using standard grid tools. In the latter case, processing workflows are automatically generated, and appropriate data sources are located and transferred to a variety of parallel processing environments for execution. As a result, it is now possible to generate large-scale mosaics on-demand in timescales that support iterative, scientific exploration. In this chapter, we describe Montage, how it was modified to execute in the grid environment, the tools that were used to support its execution, as well as performance results. Key words. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Morphology and Large-Scale Structure Within the Horologium-Reticulum Supercluster of Galaxies
Morphology and Large-Scale Structure within the Horologium-Reticulum Supercluster of Galaxies Matthew Clay Fleenor A dissertation submitted to the faculty of the University of North Carolina at Chapel Hill in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physics & Astronomy. Chapel Hill 2006 Approved by Advisor: James A. Rose Reader: Gerald Cecil Reader: Wayne A. Christiansen Reader: Dan Reichart Reader: Paul Tiesinga c 2006 Matthew Clay Fleenor ii ABSTRACT Matthew Clay Fleenor: Morphology and Large-Scale Structure within the Horologium-Reticulum Supercluster of Galaxies (Under the Direction of James A. Rose) We have undertaken a comprehensive spectroscopic survey of the Horologium-Reticulum supercluster (HRS) of galaxies. With a concentration on the intercluster regions, our goal is to resolve the “cosmic web” of filaments, voids, and sheets within the HRS and to examine the interrelationship between them. What are the constituents of the HRS? What can be understood about the formation of such a behemoth from these current constituents? More locally, are there small-scale imprints of the larger, surrounding environment, and can we relate the two with any confidence? What is the relationship between the HRS and the other superclusters in the nearby universe? These are the questions driving our inquiry. To answer them, we have obtained over 2500 galaxy redshifts in the direction of the intercluster regions in the HRS. Specifically, we have developed a sample of galaxies with a limiting brightness of bJ < 17.5, which samples the galaxy luminosity function down to one magnitude below M⋆ at the mean redshift of the HRS,z ¯ ≈ 0.06. -
Statistics of Images of Galaxies with Particular Reference to Clustering
STATISTICS OF IMAGES OF GALAXIES WITH PARTICULAR REFERENCE TO CLUSTERING JERZY NEYMAN AND ELIZABETH L. SCOTT STATISTICAL LABORATORY AND C. D. SHANE LICK OBSERVATORY UNIVERSITY OF CALIFORNIA CONTENTS PAGE General Introduction . 75 I. OBSERVATIONAL STUDIES OF THE DISTRIBUTION OF IMAGES OF GALAXIES 1. Introductory remarks . 77 2. Existing surveys of galaxies . 77 3. Suggested program of surveys . 79 II. PROBABILISTIC STUDIES OF THE DISTRIBUTION OF IMAGES OF GALAXIES 4. General remarks . 80 5. Postulates underlying the stochastic model of clustering . 81 6. Generalization to a possibly expanding universe . 83 7. Postulate regarding the "visibility" of a galaxy on a photographic plate . 84 8. Basic formulas of the theory of simple clustering of galaxies . 86 9. Some numerical results . 88 10. Expected number of images of galaxies per square degree . 92 11. Generalization of the original model: model of multiple clustering . 96 12. Probability distribution of certain characteristics of images of clusters . 100 13. Problem of interlocking of clusters . 101 14. Model of fluctuating density of galaxies . 104 15. Test for expansion of clusters of galaxies . 106 16. Concluding section: some important outstanding problems . 106 GENERAL INTRODUCTION The paper summarizes the results obtained by the authors in a cooperative study extending over several years and outlines a program of future work. Theoretical results which are not yet published include (i) extension of the model of simple clustering of galaxies, originally developed for a static universe, to cover the possi- bility that the universe is expanding (sections 6 and 8), (ii) a model of multiple clustering (section 11), and (iii) formulas relating to the distributions of certain characteristics of images of clusters on the photographic plate (section 12). -
The Seyfert Galaxy Population
FIELD GALAXIES MARKARIAN GALAXIES OPTICALLY SELECTED^ QUASARS (LOCAL! KVKRT MF.rRS A/1 INI S-mf—8648 THE SEYFERT GALAXY POPULATION a radio survey; luminosity functions; related objects THE SEYFERT GALAXY POPULATION a radio survey; luminosity functions; related objects proefschrift ter verkrijging van de graad van Doctor in de Wiskunde en Natuurwetenschappen aan de Rijksuniversiteit te Leiden, op gezag van de Rector Magnificus Dr. AAH. Kassenaar, hoogleraar in de Faculteit der Geneeskunde, volgens besluit van het College van Dekanen te verdedigen op maandag 14 juni 1982 te klokke 14.15 uur door Evert Johan Alexander Meurs geboren te Amsterdam in 1950 Sterrewacht Leiden 1982 Beugelsdijk Leiden B.V. r Promotor: Prof. Dr. H. van der Laan Referenten: Prof. Dr. H.C. van de Hulst Dr. A.G. de Bruyn Voor mijn noeder, in herinnering, en voor Wouter TABLE OF CONTENTS CHAPTER I INTRODUCTION AND SYNOPSIS page 1. Seyfert galaxies 2. Contents of this thesis CHAPTER II OPTICAL POSITIONS OF SEYFERT GALAXIES 15 1. Introduction 2. Accurate Optical Positions of Seyfert Galaxies A.S.Wilson and E.J.A. Meurs, 1978, As iron.As trophys. Suppl.Ser. 33_,407 3. Further measurements CHAPTER III A RADIO SURVEY OF SEYFERT GALAXIES 25 1. A 1415 MHz Survey of Seyfert and Related Galaxies-II E.J.A. Meurs and A.S. Wilson, 1981, Astron.Astrophys. Suppl.Ser. 45,99 2. A 14)5 MHz Survey of Seyfert and Related Galaxies-III (In collaboration with A.S. Wilson.) CHAPTER IV LUMINOSITY FUNCTIONS OF SEYFERT GALAXIES 57 1. Introduction 2. Observational data 3. The optical luminosity function of Seyfert galaxies 4. -
Administration D'oracle Solaris : Systèmes De Fichiers ZFS • Février 2012 Table Des Matières
Administration d'Oracle® Solaris : Systèmes de fichiers ZFS Référence : E25822–03 Février 2012 Copyright © 2006, 2012, Oracle et/ou ses affiliés. Tous droits réservés. Ce logiciel et la documentation qui l'accompagne sont protégés par les lois sur la propriété intellectuelle. Ils sont concédés sous licence et soumis à des restrictions d'utilisation et de divulgation. Sauf disposition de votre contrat de licence ou de la loi, vous ne pouvez pas copier, reproduire, traduire, diffuser, modifier, breveter, transmettre, distribuer, exposer, exécuter, publier ou afficher le logiciel, même partiellement, sous quelque forme et par quelque procédé quecesoit. Par ailleurs, il est interdit de procéder à toute ingénierie inverse du logiciel, de le désassembler ou de le décompiler, excepté à des fins d'interopérabilité avec des logiciels tiers ou tel que prescrit par la loi. Les informations fournies dans ce document sont susceptibles de modification sans préavis. Par ailleurs, Oracle Corporation ne garantit pas qu'elles soient exemptes d'erreurs et vous invite, le cas échéant, à lui en faire part par écrit. Si ce logiciel, ou la documentation qui l'accompagne, est concédé sous licence au Gouvernement des Etats-Unis, ou à toute entité qui délivre la licence de ce logiciel ou l'utilise pour le compte du Gouvernement des Etats-Unis, la notice suivante s'applique : U.S. GOVERNMENT END USERS: Oracle programs, including any operating system, integrated software, any programs installed on the hardware, and/or documentation, delivered to U.S. Government end users are "commercial computer software" pursuant to the applicable Federal Acquisition Regulation and agency-specific supplemental regulations. -
RADIAL STAR FORMATION HISTORIES in FIFTEEN NEARBY GALAXIES Daniel A
RADIAL STAR FORMATION HISTORIES IN FIFTEEN NEARBY GALAXIES Daniel A. Dale1, Gillian D. Beltz-Mohrmann2, Arika A. Egan3 Alan J. Hatlestad1, Laura J. Herzog4, Andrew S. Leung5, Jacob N. McLane6 Christopher Phenicie7, Jareth S. Roberts1, Kate L. Barnes8, M´ed´eric Boquien9, Daniela Calzetti10, David O. Cook1, and Henry A. Kobulnicky1, Shawn M. Staudaher1, and Liese van Zee8 ABSTRACT New deep optical imaging is combined with archival ultraviolet and infrared data for fifteen nearby galaxies mapped in the Spitzer Extended Disk Galaxy Ex- ploration Science survey. These images are particularly deep and thus excellent for studying the low surface brightness outskirts of these disk dominated galaxies 8 11 with stellar masses ranging between 10 and 10 M⊙. The spectral energy distri- butions derived from this dataset are modeled to investigate the radial variations in the galaxy colors and star formation histories. Though there is substantial variation from galaxy to galaxy, taken as a whole the sample shows bluer and younger stars for larger radii until reversing near the optical radius, whereafter the trend is for redder and older stars for larger galacto-centric distances. These results are consistent with an inside-out disk formation scenario coupled with an old stellar outer disk population formed through radial migration and/or the cumulative history of minor mergers and accretions of satellite dwarf galaxies. Subject headings: galaxies: star formation — galaxies: halos — galaxies: forma- tion — galaxies: photometry 1Department of Physics -
Arxiv:1303.5328V2
Updated Nearby Galaxy Catalog. Igor D. Karachentsev, Dmitry I. Makarov and Elena I. Kaisina Special Astrophysical Observatory RAS, Nizhnij Arkhyz, Karachai-Cherkessian Republic, Russia 369167 [email protected] Received ; accepted arXiv:1303.5328v2 [astro-ph.CO] 22 Mar 2013 –2– ABSTRACT We present an all-sky catalog of 869 nearby galaxies, having individual dis- −1 tance estimates within 11 Mpc or corrected radial velocities VLG < 600 km s . The catalog is a renewed and expanded version of the “Catalog of Neighboring Galaxies” by Karachentsev et al. (2004). It collects data on the following ob- servables for the galaxies: angular diameters, apparent magnitudes in FUV -, B-, and Ks- bands, Hα and HI fluxes, morphological types, HI-line widths, radial velocities and distance estimates. In this Local Volume (LV) sample 108 dwarf galaxies remain to be still without measured radial velocities. The catalog yields also calculated global galaxy parameters: linear Holm- berg diameter, absolute B-magnitude, surface brightness, HI-mass, stellar mass estimated via K-band luminosity, HI rotational velocity corrected for galaxy in- clination, indicative mass within the Holmberg radius, and three kinds of “tidal index”, which quantify the local density environment. The catalog is supple- mented with the data based on the local galaxies (http://www.sao.ru/lv/lvgdb), which presents their optical and available Hα images, as well as other service. We briefly discuss the Hubble flow within the LV, and different scaling rela- tions that characterize galaxy structure and global star formation in them. We also trace the behavior of the mean stellar mass density, HI-mass density and star formation rate density within the considered volume.