head 1.1; access; symbols; locks http:1.1; strict; comment @# @; expand @b@; 1.1 date 2004.02.03.12.40.52; author AndyLawrence; state Exp; branches; next ; desc @none @ 1.1 log @none @ text @ࡱ>  ! X bjbj +l...DXXXlV8V8V888R9$l2:^L(MMMNQKRhz||||||$- MXRsN"NRRsXXMMksssRXMXMzsRzssyBXXMv: ڲՁl0V8odvf0ssllXXXXPerformance tests for Grid Components in AVO Guy Rixon, 2002-11-01 Summary Tests of components and systems based on grid-computing techniques are necessary to inform and validate AVOs construction of software. Two classes of test are proposed: top-down tests, based on use-cases derived from scientific goals, and bottom-up tests derived from architectural analysis. The top-down tests have greater power for objective validation of systems, while the bottom-up tests have greater predictive power for choosing aspects of system architecture; both types of test are necessary. It is proposed that the top-down tests be based on the representative science-cases identified by AstroGrid since (a) an extensive analysis of these cases is already available; (b) the AstroGrid cases will be implemented in software as a priority; (c) the data-resources for the cases are available inside AVO. These tests are largely independent of system architecture. There is a pre-existing plan to transfer data in bulk from La Palma to Cambridge using GridFTP. This is an opportunity for an extensive test of a crucial piece of data-grid technology. It is proposed that AVO monitors the results of this experiment. The design of bottom-up tests depends on details of the system architecture. The architecture emerging from AstroGrids investigations, which is intended to be suitable for AVO and the global VO, is described in outline. Tests are presented that check for performance problems in specific parts of this architecture. Introduction Motivation for testing The performance tests may help several ways. They warn us of bad software-architecture and unworkable software-components. They set realistic limits on capabilities of the VO. They identify areas of poor performance that can be improved simply by buying better equipment. They validate the investment in AVO by demonstrating that science can be done faster in a gridded environment. The first and last points are the most important, since they measure the overall success or failure of the project. What to test? Two kinds of test are needed: top down and bottom up. The top-down tests are specific, astronomical procedures derived from real, scientific use-cases. These tests measure the overall performance of the VO, including both the times for actual data-processing and the additional costs in doing that processing on the grid. The bottom-up tests investigate specific grid technology. These tests measure the overhead incurred by grid operations for the small-scale operations around which the use-cases are built. Using the data from the bottom-up tests, it is possible to predict, for a given use-case, which combinations of grid architecture have the best performance. These thought experiments are a cheap way of checking the performance of architectures: they show clearly the extreme cases of good and bad performance. We do not have enough resource to test all architectures experimentally, so the thought experiments are essential. Bottom-up tests do not validate a chosen architecture. It is common in IT for a system to under-perform even though all its individual parts work to specification. This may be because the performance prediction misses out some source of overhead; or because the combination degrades the performance of the individual parts. It is not safe to rely on predicted performance, so the top-down tests are needed for validation. In the top-down tests, the metrics are: The overall run-time of the use cases. The fraction of run-time (duty cycle) in which the user must drive the system interactively. The mean time between user interventions during the run (MTBI). In many cases, improving duty cycle and MTBI at the expense of run-time may be a gain for users. Each of the bottom-up tests measures time to achieve some part of a use case. At some level, the use cases break down into individual computations of the kind that can be run on the grid as batch jobs (computational-grid model) or service calls (service-grid model). The time to finish a computation depends on these factors: The time, D, to discover the resources needed to execute the job. The time, S, to install the software on the chosen processor (S is typically non-zero in purely computational grids). The time, I, to move the input data to the processor over the network. The time, L, to load the data into the processing system (typically important for tabular data loading into a DBMS, but negligible for image data). The time, C, to execute a call to the processor, including any access-control checks and parsing of arguments. The queuing time, Q, before the job runs on the chosen processor. The processing time, P. The time, W, to write out the results in a VO-compatible format. The time, O, to retrieve the output data across the network. In any given job, many of these factors will be negligible; e.g. L, C and W are believed to be unimportant compared with P for all image processing. These assumptions and beliefs are grounded in experience with desktop processing and may be unsafe in grid computing. Therefore, all parts of the job should be considered and tested. What kind of grid? There are three distinct kinds of grid, each with a different purpose and natural architecture. A practical grid will almost certainly combine the natural architectures. A computational grid [1] provides access to processors. Programmes and data are sent away to the processor, the job is run and the results are recovered. Between jobs, the users files are not retained at the processor. Computational grids optimise workflows for processing speed at the expense of network bandwidth and the time to prepare and configure software. A service grid [3] provides access to pre-installed software. Typically, the services are installed at the same site as the data that they must process; alternatively data may be passed in to the service with each job executed. Results may be passed back to the client at the end of the job, or they may be cached by the service for later retrieval. An important special case of a service grid is a network of data-selection services. Service grids optimise the use of network bandwidth (in the case where the services are collocated with their data-sets) and the cost of installing and supporting software (by concentrating the work of many users on a few installations) to the detriment of processing power: the services typically cannot be concentrated on the best processors. A special, and crucial, case of a service grid is a network of data-selection services. Each of these services provides a faade for an archives data set of arbitrary size, and generates extracts from the archive according to queries. The extracts are small and portable and can be passed to other, remote services whereas the original archives are too large and complex to transport. A data grid [2] provides access to distributed data. A programme on a given processor can use the data grid to read in data for any part of the grid, and to write out results to storage inside the data grid; that is the results remain accessible to programmes through the data grid. Data-grid products to date have concentrated on sharing files. Data-grid systems that share database tables are also possible and desirable. A system that allows federations between database tables on different sites is a data grid. AstroGrids first-year research into grid technologies [4] strongly suggests that the VO should be based on a service grid with an associated data grid. The service grid should be based on data-selection services, since astronomy abounds with large, non-portable archives. Other services will allow processing of extracts produced by the selection services. Since many research programmes require combination of data from different archives, the services cannot all be collocated. The primary purpose of the data grid is to move data extracts between the data-selection and data-processing services and later from the services to the desktop for visualization. A secondary purpose for the data grid is to allow combined searches of database tables as if they were one table. This feature is effectively a distributed join on database tables and is extremely sensitive to limits in network bandwidth. There is little perceived need for a pure computational grid. Computations on astronomical data do relatively little work per datum compared to, say, theoretical modelling in science and engineering. Consequently, the cost of moving data to the processors is expected to outweigh the gains in processing speed. However, this is folklore; the assumption has not been tested. Top-down tests Tests based on VO use-cases AstroGrid use cases AstroGrids analysis of requirements has identified 10 use-cases that are representative of the general requirements. Four of these are to do with solar astronomy or solar-terrestial physics, and are therefore not relevant to AVO; the remaining six are to do with astronomy outside the solar system and are directly applicable to AVO. These use cases are ideal for testing astronomical grids: they have been worked out in detail by AstroGrid staff; they are chosen to have good coverage of both the science expected from AstroGrid (and, by extension, from the VO) and the technical challenges identified so far; AstroGrid is committed to supporting these particular use-cases as a priority; the use-cases can be executed using data resources already available to AstroGrid and therefore to AVO; the cases will be executed periodically as a qualitative test of the system; this provides a chance to get more performance data with less labour; performance targets, in the form of total, allowable run-times, have been stated for each use-case. The use cases are listed and described in AstroGrids Science Requirements Document (SRD) [5]. Searching for Brown Dwarfs Discovering low-surface-brightness galaxies The galaxy environment of Supernovae at cosmological distances Object identification in deep-field surveys Localizing galaxy clusters Discovering high-redshift quasars. These are the leading characteristics of the the use cases as stated in the SRD.  HYPERLINK "/bin/view/VO/BrownDwarfSelection" Brown Dwarfs A-S y y y y Y y Y y Science CaseScience CatAdvanced Algorithms AQL Compute Intensive Database Access Data Mining IAA  HYPERLINK "/bin/view/Astrogrid/AstroOntology" AstroOntology,  HYPERLINK "/bin/view/Astrogrid/WorkFlow" WorkFlow Resource Location  HYPERLINK "/bin/view/VO/LowSurfaceBrightnessGalaxyDiscovery" LSB Galaxies A-G y y Y   y  y  HYPERLINK "/bin/view/VO/SupernovaGalaxyEnvironment" SN Environment A-G y y Y Y  y  Y  HYPERLINK "/bin/view/VO/DeepFieldSurveys" Deep Fields A-C Y Y y Y  y y y  HYPERLINK "/bin/view/VO/GalaxyClustering" Galaxy Clusters A-C Y y Y Y Y Y    HYPERLINK "/bin/view/VO/HiZQuasars" Hi-z QSO's A-C Y y y y Y Y   Science Cat = Science category: A-S (Astronomy: Stellar), A-G (Astronomy: Galaxy), A-C (Astronomy: Cosmology). A matrix element marked 'Y' indicates that this area will be important, whilst 'y' indicates a lesser degree of importance. AQL = Astronomical Query Language. IAA = Identity, Authentication and Authorization (collectively, control of access to resources). Science Case Science Cat Data Manipulations Problem Completion Time  HYPERLINK "/bin/view/VO/BrownDwarfSelection" Brown Dwarfs A-S Perform complex query on 1000 deg^2 of multi-colour (e.g. 6 band, Sloan &  HYPERLINK "/bin/view/Astrogrid/UKIDSS" UKIDSS) to return 1000+ Brown Dwarf candidate sample, plus postage cutouts of pixel data (~20Mb pixel data per cutout). For each candidate return proper motion estimate via astrometry of multi-temporal data sets. One hour  HYPERLINK "/bin/view/VO/LowSurfaceBrightnessGalaxyDiscovery" LSB Galaxies A-G Select candidates from IR data sets (e.g. 1000 sq deg of  HYPERLINK "/bin/view/Astrogrid/UKIDSS" UKIDSS Large Area Survey data), cross match with Sloan optical, perform background analysis, determine luminosity calculations One hour  HYPERLINK "/bin/view/VO/SupernovaGalaxyEnvironment" SN Environment A-G For search fields, classify galaxies, determine redshifts (literature search, spectral or photmetric methods).30 mins  HYPERLINK "/bin/view/VO/DeepFieldSurveys" Deep Fields A-C Automatic registration and calibration of multicolour data sets (~10 wavebands, few 100 MB/band), object identification, cross identification and association.One hour  HYPERLINK "/bin/view/VO/GalaxyClustering" Galaxy Clusters A-C Generate cluster maps from smoothing functions applied to red early type galaxies identified in catalogue data (e.g.  HYPERLINK "/bin/view/Astrogrid/SRD" \l "JumpToVST" VST,  HYPERLINK "/bin/view/Astrogrid/UKIDSS" UKIDSS). Assign redshifts to clusters via photometric techniques, compare sanple with model outputs as function of redshift.Four hours  HYPERLINK "/bin/view/VO/HiZQuasars" Hi-z QSO's A-C Perform complex query on 2000 deg2 of multi-colour (e.g. 6 band, Sloan &  HYPERLINK "/bin/view/Astrogrid/UKIDSS" UKIDSS) to return 1000+ QSO candidate sample, plus postage-stamp cut-outs of pixel data (~20MB pixel-data per cut-out). Ability to cross reference the sample QSO set against X-ray, Radio, NED, catalogue lists. One hour Note that the total allowed time for each case is low enough that a test of the case can be run manually. That is, the tests can include human intervention and decision points. Because of the richness of features used by these science cases, it will not be possible to run all of any given case until quite late in the project. Therefore, the science cases are broken up into smaller use cases that can be run independently. This approach is fundemental to AstroGrids programme of software construction: each development cycle builds a selection of complete use cases. Accordingly, performance tests based on the use cases are a suitable building block. It is reasonable to expect that AstroGrid software be instrumented for these uses cases as it is produced. The analysis of science use-cases into technical use-cases is presented in appendix A of this document. This analysis is taken from the AstroGrid architecture documents [6]. Details of the technical use-cases are available in the same documents. Assumed architecture These tests are deliberately made as general as possible. The use cases could be executed on many architectures. However, AstroGrid has made some assumptions as follows. The data sources are distributed about the network. There is either a service grid or a compute grid for the basic computations. If a compute grid, then the process of installing temporarily the necessary software for each computation is hidden from the user such that the grid feels like a service grid. There is a data grid. Data, including bulk data such as images, may move from node to node during the use cases. Data moving from service to service need not be routed through the desktop client controlling the use case. Results of steps within the use cases are retained within the data grid and need not be copied to and from the desktop client between processing steps. Grid-style access control is available where it is needed. Transferring INT WFS results from La Palma to Cambridge Motivation One other high-level use-case is advantageous for testing the data grid: the transfer of images in the Isaac Newton Telescope Wide Field Survey (INT WFS) [7] from the Isaac Newton Group of telescopes on La Palma to the archive centre at Cambridge. The INT WFS produces a moderate amount up to ~1 GB of pixel data per night of observation, and the observations are public to the UK and NL communities immediately after observation. The images are reduced in a pipeline and the reduced data are published on a FTP site at Cambridge. Currently, the data are sent to Cambridge on tape and are reduced at Cambridge. The operation could be made more efficient and timely by using GridFTP [8] to move the files across the network. The reduction can best be performed at the observatory on their processor farm Gigawulf [9], whereas the archiving is best done at Cambridge. The link between reduction pipeline and archive needs to be automatic, as reductions occur continuously and the staff costs for manual filing of the reduced data would be too high. GridFTP is ideal for this task, since it allows image files to be pushed from La Palma to Cambridge as they become available. Pre-grid arrangements for pushing files are not appropriate on the public internet; they are either insecure (e.g. ordinary FTP with passwords exchanged in clear text) or extremely inefficient (e.g. scp, which laboriously encrypts every byte sent). GridFTP is ideal for the task as it provides a secure exchange without encrypting the bulk of the data. The tests The transmitting agent must detect images as they become available from the data-reduction pipeline and must push them across the network as soon as possible. If the thoughput of the pipeline temporarily exceeds the throughput of the network, then images must be queued on La Palma until the network is quieter. That is, the transmitting agent must exploit the average network bandwidth over 24 hours of operation and must be capable of recovering from downtime on the network. The receiving agent must copy the images to disc and catalogue them. The system as a whole must be capable of steady-state operation over several weeks of observations at a time. This is an extreme test of the long-term stability of the GridFTP protocol. Arrangements with ING staff to run this test are in hand. Architectural assumptions This test assumes the following features. Nodes of the VO will want, and will be allowed, to exchange regularly large volumes of data as network transfers in preference to exchange on removable media. Security is important. Grid-style access control is available where it is needed. GridFTP is the protocol of choice for moving data in bulk. Bottom-up tests Architectural assumptions These tests are based on details of the architecture emerging from AstroGrids investigations [ref], as follows.  Probable grid architecture. The links in the service grid (lines with arrows) have a tree-like structure expressing a hierarchy of control and delegation. The links in the data grid (broad lines without arrows) have a bus-like structure. The core of the system is a service grid based on web services. Services are fine-grained enough i.e. do a small enough part of each use-case that latency on starting them may be important. Arguments to services are sent in XML form and converted as necessary to local formats at the site of the service. Grid-style access controls [10] are used where access needs to be restricted. Authorization uses central database of authority data. There is a data-grid for moving files between services. The data grid uses mainly server-to-server transfers via GridFTP. The data grid also links certain database services such that federations of database tables are possible. Latency in web-service calls An echo service will be distributed which echoes a single argument back to its caller. This is the minimal programme that exercises both input to and output from a service. The round-trip time for calling this service defines the minimum overhead for calling any web-service. The echo service will be installed on all AstroGrid sites (most have a version already), and can be installed on other AVO sites as needed. The echo package will be made portable to all web-service hosting-environments. Clients will be put in place to poll all known echo services at intervals of order one minute. Over time, this will determine for each connection both the average response time and the distributions of response times under exceptional conditions. It will be possible to monitor how often the VO may under-perform due to failures in the underlying network. The echo services can also be use to test the response of web-service installations to large numbers of simultaneous connections. A special client for this will be developed. Two versions of the echo service should be tested: a pure web-service code, applicable to any hosting environment, and a grid-service version, applicable to OGSA environments. It is important to AVO to measure any additional overhead introduced by OGSA. The echo service will be provided as Java software. Latency due to access controls Two processes are to be measured: authentication of a users identity and checking the users authorization to carry out a task. Both can best be measured using a do-nothing service. Two variants of the echo service, described above, will be used. The OGSA authentication process will be used. Specifically, the process described as SOAP secure in the OGSA technology-preview [11] will be used, since this seems to be the process implied by emerging GGF and industry standards. The SOAP-secure process makes the greatest possible use of industry standards. The authorization look-ups will be delegated to an external authorization-service. Initially, this will be an instance of AstroGrids prototype CoPS [12], since an web service is implied. In later arrangements of the tests, a version of Globus product CAS [13] may replace CoPS. CAS is expected to be available as a grid service in the first quarter of 2003. Two services will be provided and will be tested separately. The authenticating echo-service will work exactly as the basic echo service but with an identity check on each call. The authorizing echo-service will work exactly as the authenticating echo-service but adds a call to the authorization service for each call to the echo service. The echo services are expected to put little load on the host computer. All three variants can be run in parallel, so that calls to each variant execute in the same conditions of processor load. This allows the specific overheads due to authentication and authorization to be measured accurately. Latency due to Parsing parameters from XML The software to explore this will be based on the Sextractor web-service produced for AVOs demonstration in January 2003 [14]. Sextractor is a good example of a service with bulky input-parameters and bulky outputs, both of which need to be translated from grid form to native form. Sextractor can stand as a prototype for this kind of service. The test is as follows. To parse the input parameters from XML. To validate the parameters against their XML schema. To translate the parameters into Sextractors native form (a parameter file plus a few command-line variables). To generate VOTable output from a fixed file of Sextractors output. Note that Sextractor itself is not run in this test because the run-time of the astronomical code could dominate the translations being measured. Instead, a dummy version of the service is used that always produces the same, precalculated output. Furthermore, where the real Sextractor service would read in one or more images, possible from remote sites on the data-grid, the dummy service does not use any image files. The tests can be repeated with different sizes of output catalogue. Based on the object density of the INT WFS images, a catalogue of ~10,000 rows per run is a fair test. File-transfer bandwidth Two protocols are to be tested: HTTP and GridFTP [8]. Each protocol will be tested between both clients and servers and between pairs of servers each under control of one client (third-party transfers). Initially, these tests can be run with generic HTTP and GridFTP servers; this is an easy way to get early tests of the network bandwidth. The normal web-server software from the Apache foundation is a possible server for HTTP. The only GridFTP server currently available is part of the Globus toolkit [15]. When the server programmes for the data-grid proper become available, the tests will be repeated, to look for variations in performance with to the generic servers. To allow this comparison, the tests are deliberately kept simple and free of astronomical content. Special clients will be written for these tests using the Java commodity-grid (CoG) kit [16] that works with the Globus toolkit and with GridFTP. The test is to repeatedly transfer files of the same size, measuring the average time for each transfer and the distribution of times. The test can be tuned in two different ways. If the same file is transferred repeatedly, it will tend to remain in memory on both the sending and receiving nodes and will not need to be repeatedly read from disc on the sending node. The effect of local I/O on the transfer time will be reduced. The measured times will be as close to the minimum defined by the network bandwidth as can be achieved with commodity servers. If a different file is transferred each time, more strain will be put on discs and memory on the sending and receiving nodes. The measured times will be more representative of normal, working conditions but will say less about the underlying network. Both variants should be tested. Several sizes of files should be used for the tests. The smallest-possible file: a single byte. A file matching a small image-extract: an image one arcminute on each side with half-arcsecond pixels. This file would be ~ 60KB in FITS format and is representative of the smallest image extracts likely to be used. A file matching the image from a full CCD or similar detector. This file would be ~17 MB in FITS format. A file matching a mosaic of all the detectors in a VISTA observation. This file would be ~1 GB in FITS format. Clearly, files of other sizes can be used, but these represent the lower limit, two typical sizes and the practical upper-limit. These prescribed sizes should be used to test network links between AVO sites on a regular basis. As a one-off test, a wider range of file-sizes should be tested, filling in the points between the prescribed sizes for the regular tests. The objective is to test for any dependencies of effective bandwidth on file size. Latency in combining database tables Background Federation of databases between sites sometimes requires a distributed join of tables. Consider two databases containing catalogues with measurements of the same object: one contains columns for optical magnitudes B, V and R and another contains columns for infrared magnitudes J, H and K. It is scientifically useful to be able to select objects on the basis of their V-K colour, but this requires tables from the two databases to be joined. This join-between-databases option is not supported in most DBMS; special arrangements are needed to achieve the distributed join. Much of the VO work involves joining catalogues. The feature cannot be excluded from the system. Distributed joins are believed to suffer from very poor performance, since they logically involved copying all rows of one database into its partner before doing the selection [17]. However, this belief has not been tested; the true performance is uncertain by orders of magnitude. If the performance of distributed joins is unacceptable for some or all cases, then the VO may be forced to provide a data-mining centre at which replicas of catalogues can be combined into one master database. It is therefore vital to measure the distributed joins. Proposed tests We need a database system capable of distributed joins. Such as system exists in astronomy: the SkyQuery system [18] developed and released for the Sloan Digital Sky Survey (SDSS). SkyQuery is already installed at some AstroGrid nodes. Notably, a SkyQuery DB exists at Cambridge holding the combined object catalogue from the INT Wide-Field Survey: ~1,000,000 rows. We need to measure the overhead of joining tables. The simplest test is to federate one catalogue with itself in these configurations: One DB table, in one DB, on one computer. Two DB tables, in one DB, on one computer. Two DB tables, in two separate DBs, on one computer. Two DB tables, in two separate DBs, on two computers, on the same LAN. Two DB tables, in two separate DBs, on two computers, connected across the Internet. The test results are to be assessed relative to the baseline measurement, number 1 above. This means that the exact nature of the catalogue used for the test is not critical to the results, since the tests do not have to be compared to a baseline derived from a separate DB system. We also need to know whether the performance of the distributed join varies with the size of the table. I.e. is the extra cost per row roughly constant with the number of rows, or are there regimes of exceptional cost? The unit of testing should be a SQL SELECT command that selects on the combination of two columns and also on some other criteria that can be evaluated entirely inside one table. I.e., apart from the selection criterion that causes the join, there should be some way of limiting the numbers of rows in the join that does not itself require coordination between the two DBs. SkyQuery is known to exploit intelligently these local selections in order to minimized the size of the join. These tests should be repeated at different points on the European academic networks, in order to sample many different levels of bandwidth. The tests should be coordinated with the basic bandwidth tests (see above). This might be achieved in either of two ways: have many sites within AVO set up matching SkyQuery installations; or use one base-station (IoA Cambridge is already equipped) and one portable station that tours the AVO sites for the duration of the test. The SkyQuery installation with the INT-WFS catalogue is small enough to be hosted on a laptop PC if the touring option is approved. Acknowledgments The material used in this document includes input from many members of AVO and particularly of AstroGrid; the discussion of the architecture and performance issues has been public and many people have contributed. The science cases for the top-down tests are taken from the AstroGrid science-requirements document by Nicholas Walton, and the analysis into technical use-cases was lead by Elizabeth Auden, David Giaretta, and Anita Richards. The experiment between La Palma and Cambridge was suggested by Nicholas Walton and Robert Greimel. Potential problems with distributed joins have been investigated by Clive Page. The Sextractor service, with which AVO can test argument-parsing overheads is a contribution by AstroGrid to the AVO demonstration of January 2003 and led by Martin Hill and Kona Andrews. References [1] Computational Grids. I. Foster, C. Kesselman. Chapter 2 of "The Grid: Blueprint for a New Computing Infrastructure", Morgan-Kaufman, 1999. [2] The Data Grid: Towards an Architecture for the Distributed Management and Analysis of Large Scientific Datasets. A. Chervenak, I. Foster, C. Kesselman, C. Salisbury, S. Tuecke. Journal of Network and Computer Applications, 23:187-200, 2001 (based on conference publication from Proceedings of NetStore Conference 1999). [3] The Physiology of the Grid: An Open Grid Services Architecture for Distributed Systems Integration. I. Foster, C. Kesselman, J. Nick, S. Tuecke, Open Grid Service Infrastructure WG, Global Grid Forum, June 22, 2002. (extended version of  HYPERLINK "http://www.globus.org/research/" \l "IEEE-CS-2" Grid Services for Distributed System Integration) [4] The AstroGrid Phase-A report. AstroGrid project, 2002.  HYPERLINK "http://wiki.astrogrid.org/pub/Astrogrid/PhaseAReport/redbook.pdf" http://wiki.astrogrid.org/pub/Astrogrid/PhaseAReport/redbook.pdf [5] AstroGrid Science Requirements Document. AstroGrid project, 2002.  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/SRD" http://wiki.astrogrid.org/bin/view/Astrogrid/SRD [6] Sequence Diagrams for AstroGrid science-cases. AstroGrid project, 2002.  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/SequenceDiagrams" http://wiki.astrogrid.org/bin/view/Astrogrid/SequenceDiagrams [7] Isaac Newton Telescope Wide-Field Survey. Cambridge Astronomical Survey Unit, Institute of Astronomy, University of Cambridge.  HYPERLINK "http://www.ast.cam.ac.uk/~wfcsur/index.php" http://www.ast.cam.ac.uk/~wfcsur/index.php [8] GridFTP Protocol Specification. W. Allcock, J. Bester, J. Bresnahan, A. Chervenak, L. Liming, S. Meder, S. Tuecke. GGF GridFTP Working Group Document, September 2002. [9] Pipeline Data Processing. R. Greimel, J. Lewis and N. Walton, in Isaac Newton Group Newsletter, 4, March 2001. [10] A Security Architecture for Computational Grids. I. Foster, C. Kesselman, G. Tsudik, S. Tuecke. Proc. 5th ACM Conference on Computer and Communications Security Conference, pp. 83-92, 1998. [11] OGSI technology preview release. Globus Project, 2002.  HYPERLINK "http://www.globus.org/ogsa/releases/TechPreview/index.html" http://www.globus.org/ogsa/releases/TechPreview/index.html [12] Community Privilege Service. AstroGrid project, 2002.  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/CASDemo" http://wiki.astrogrid.org/bin/view/Astrogrid/CASDemo [13] A Community Authorization Service for Group Collaboration. L. Pearlman, V. Welch, I. Foster, C. Kesselman, S. Tuecke. Proceedings of the IEEE 3rd International Workshop on Policies for Distributed Systems and Networks, 2002. [14] ACE: AstroGrid Catalogue Extractor. AstroGrid project/AVO project, 2002.  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/AVODemo" http://wiki.astrogrid.org/bin/view/Astrogrid/AVODemo [15] Globus: A Metacomputing Infrastructure Toolkit. I. Foster, C. Kesselman. Intl J. Supercomputer Applications, 11(2):115-128, 1997. Provides an overview of the Globus project and toolkit. [16] A Java Commodity Grid Toolkit. G, von Laszewski, I. Foster, J. Gawor, P. Lane. Concurrency: Practice and Experience, 13, 2001. [17] Data warehouse vs. federating databases. On-line discussion led by C. Page.  HYPERLINK "http://forum.astrogrid.org/read.php?TID=168" http://forum.astrogrid.org/read.php?TID=168 [18] SkyQuery: a Distributed Web-based Query Service for Astronomy. T. Malik, T. Budavari, Alex Szalay and Ani Thakar. The Johns Hopkins University, 2002. http://contest.eraserver.com/SkyQuery/ Appendix A: decompositions of AstroGrid science cases Searching for Brown Dwarfs Introduction An astronomer exploring the lower end of the stellar mass function wants to conduct a census of brown dwarfs. The census population will be determined by colour, proper motion, and location (such as all brown dwarfs within some radius around the sun). New brown dwarf candidates have been successfully identified by conducting a proper motion survey of Galactic clusters (clusters of Stars in the Milky Way). This use case is based on the paper "Brown Dwarfs in the Pleiades and the initial mass function across the stellar/substellar boundary" by Hambley, et al, MNRAS 303, 835. Their calculation for relative proper motion should probably be accessed via user code, a web service, or possibly a library function. Their procedure for calculating proper motion has been summarized: For each 'image' (defined by Hambly, et al as an area of 5 or more connected pixels) in the dataset, the mean position of the image is calculated over all datasets. Then the relative shift of each image from an individual dataset is determined with respect to the mean position. Finally a weighted linear least-squares fit as a function of time is applied to the relative shifts; this determines the image's relative proper motion. A vector-point diagram of the images' proper motion is produced. Flow of Events 1. The astronomer searches the resource catalogue for catalogues containing Galactic clusters via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch. 2. A list of cluster catalogues is returned via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults, and the astronomer selects one or more cluster catalogues via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue. 3. Next, the astronomer searches the selected catalogues for cluster locations via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch. 4. A list of locations, defined by right ascension, declination, radius, and distance, is returned via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults. 5. The astronomer then returns to the resource catalogue and executes a complex query for catalogues with coverage of I, K, or R wavelengths over each cluster location via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ComplexQuery" ComplexQuery. 6. A list of catalogues with I, K, or R coverage of the cluster location is returned via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults. 7. The astronomer selects 1 or more catalogues via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue and searches them for 2 or more datasets covering the cluster location in the same wavelength (either all datasets with I coverage or all with K coverage) via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch. 8. The datasets are stored to  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/MySpace" MySpace via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults. 9. Now the astronomer can prepare the data for the proper motion survey. The datasets are astrometrically aligned using a library function, a web service, or user code via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram. 10. Next, the proper motion can be applied to the datasets by user code, a web service, or a library function via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram. 11. The program calculates a proper motion vector-point diagram of objects in the dataset. The diagram is stored on  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/MySpace" MySpace via  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData and returned to the astronomer. Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\AgWiki _ Astrogrid _ BrownDwarfSelectionSD_files\\browndwarfSD2.gif.gif" \* MERGEFORMATINET   HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ComplexQuery" ComplexQuery  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue Discovering Low Surface Brightness Galaxies Introduction An astronomer wishes to discover new faint galaxies. To locate extended objects with low surface brightness in an image, all bright point sources and extended objects must be removed. Low surface brightness galaxy candidates are compared against background flux to determine existence. Flow of Events First, the astronomer searches the resource catalogue for image catalogues with magnitude and depth metadata. After selecting an appropriate catalogue, the astronomer searches the catalogue for images of point sources and other bright structures. After selecting a suitable image (or images), the astronomer can upload and run three pieces of code on the image: an algorithm to remove bright sources, an algorithm to smooth the image, and an algorithm to identify any extended sources that remain against the sky background. A list of extended source candidates is returned. Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\AgWiki _ Astrogrid _ LowSurfaceBrightnessSD_files\\lowsurf_brightness.gif" \* MERGEFORMATINET   HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob The Galaxy Environment of Supernovae at Cosmological Distances Introduction An astronomer wants to ascertain whether a supernova candidate is Type Ia or Type II. Determining galaxy redshift and morphology of the environment in which the supernova candidate was discovered will aid classification. Flow of Events First, the astronomer searches the resource catalogue for optical or IR image data catalogues covering known supernova positions. The astronomer selects a catalogue from the returned list and requests images from the catalogue, based on position. The astronomer then acquires recent observations of the same location (in the same wavelength) from a telescope resource. The new observation image is uploaded onto Astrogrid; it is subtracted from the old image, creating a new subtracted image. The astronomer then uploads an algorithm to check the new image for objects that have moved between the first and second observation; these objects are eliminated as near Earth objects. Finally, a catalogue is generated of the remaining supernova candidates. Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\AgWiki _ Astrogrid _ SupernovaGalaxyEnvironmentSD_files\\supernova_galaxy.gif" \* MERGEFORMATINET  The flow of event is more like as follows. The above describes how one would support the actual discovery of the SN via facilitating the running of search alogorithms (image subtraction etc). For SN search areas: search literature and published sources for possible spectroscopic redshifts of galaxies in fields. search archives for spectroscopic data of objects in field > determine redshifts of galaxies in fields using perhaps automated techniques such as devloped for the 2dFGRS (see  HYPERLINK "http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2001MNRAS.328.1039C&db_key=AST&high=3c502ee73919240" \t "_top" Colless et al, 2001) Locate multicolour broadband optical data for the search fields Determine  HYPERLINK "http://nedwww.ipac.caltech.edu/level5/Glossary/Essay_photredshifts.html" \t "_top" photometric redshifts to galaxies in the fields using a variety of techniques (e.g.  HYPERLINK "http://webast.ast.obs-mip.fr/hyperz/" \t "_top" hyperz, more recently (2002)  HYPERLINK "http://www.iap.fr/pegase/zpeg/cgi-bin/zpeg.pl" \t "_top" Z-Peg). identify possible galaxy clusters (see e.g.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/OpticalNearIRGalaxyClusterSelection" OpticalNearIRGalaxyClusterSelection) cross reference position of newly discovered SN from search. If located in a galaxy for which the redshift is known from one of the above techniques, return an assigned redshift for that SN (together with estimation of error). return morphological information of the galaxy in which the SN candidate is located (if applicable)  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformLiteratureSearch" PerformLiteratureSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue Object Identification in Deep Field Surveys Introduction An astronomer wants to correlate deep field surveys taken in different wavelengths. Images taken in two wavelengths (for instance, optical and radio), are aligned so that matching objects can be identified and correlated in both images. Flow of Events 1. First, the astronomer searches the resource catalogue for optical and radio deep field surveys with wavelength, instrument, sensitivity, dynamic range, epoch, and resolution metadata. A list of surveys is returned and one or more are selected. ( HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch) 2. The second wavelength (radio) survey is queried on the same position and radius, and another list of images is returned.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch,  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults) 3. The first wavelength (optical) survey is queried by coordinates and radius, and a list of images is returned.( HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch,  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults) 4. Matching images from both wavelengths' surveys are uploaded to a compute resource. ( HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource,  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/TransferDataToResource" TransferDataToResource ???) 5. Three algorithms are identified to the compute resource and run on both images: an astrometric alignment algorithm, a flux scale calibration algorithm, and finally a least squares fit alignment algorithm. ( HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram) 6. The aligned images are returned to  HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/MySpace" MySpace. ( HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData) Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\AgWiki _ Astrogrid _ DeepFieldSurveysSD_files\\deep_field.gif" \* MERGEFORMATINET   HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ComplexQuery" ComplexQuery  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/TransferDataToResource" TransferDataToResource Localizing Galaxy Clusters Introduction An astronomer wishes to calculate the density of galaxies over a particular location and then determine the redshift of those galaxies' spectra. Flow of Events First, the physicist searches the resource catalogue for galactic catalogues. An appropriate catalogue is identified and searched with a complex query on colour inequality. A list of target locations is returned, and target galaxy datasets are uploaded to a compute resource. The astronomer then uploads and runs a density map creation algorithm on the compute resource. Next, a redshift estimation algorithm is uploaded and run on the galaxy target datasets. The compute resource returns the coordinates of peaks on the density map. The astronomer can then search the resource catalogue for a spectrographic catalogue to query by coordinates. Matching spectral data is uploaded to the compute resource along with an algorithm to compute redshift. The compute resource returns the redshift of target galaxies. Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\AgWiki _ Astrogrid _ GalaxyClusteringSD_files\\galactic_cluster.gif" \* MERGEFORMATINET   HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ComplexQuery" ComplexQuery  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineModel" DetermineModel  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineProgram" DetermineProgram  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessLibraryFunction" AccessLibraryFunction  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AccessWebService" AccessWebService  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/UploadUserCode" UploadUserCode  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/SelectCatalogue" SelectCatalogue  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob Discovering High-redshift Quasars Introduction An astronomer wishes to investigate the epoch of ionisation in the universe. As a pragmatic first step, this intrepid researcher wants to discover new high redshift quasars with 5 < z < 10. Flow of Events First, the physicist searches the resource catalogue for all catalogues optical, near IR, or x-ray data with area information. A list of catalogues is returned, and the physicist selects two or more catalogues in different wavelengths to join on some inequality. The smaller catalogue(s) is joined with the larger catalogue and a result list is returned to the astronomer. Sequence Diagram  INCLUDEPICTURE \d "C:\\Documents and Settings\\gtr\\Desktop\\" \* MERGEFORMATINET   HYPERLINK "http://wiki.astrogrid.org/bin/view/Astrogrid/UseCases" UseCases: These use cases are the ones that will be needed to deliver this case.  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformRegistrySearch" PerformRegistrySearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/PerformCatalogueSearch" PerformCatalogueSearch  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToResource" NegotiateAccessToResource  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/AuthenticateIdentity" AuthenticateIdentity  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/DetermineAuthority" DetermineAuthority  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ComplexQuery" ComplexQuery  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/NegotiateAccessToJob" NegotiateAccessToJob  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpacePublishDerivedData" MySpacePublishDerivedData  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/ResultMerge" ResultMerge  HYPERLINK "http://wiki.astrogrid.org/bin/view/VO/MySpaceStoreResults" MySpaceStoreResults  Sextractor is a programme that finds and measures objects stars, galaxies, etc. in an image of the sky and writes out the details of those objects as a catalogue. It is a flexible programme with over 200 free parameters in its input configuration. This is towards the high end of the complexity scale. AVOs demonstration includes making Sextractor available as a web service and therefore translating all the input parameters from XML to Sextractors native format.  At the time of writing, the Java CoG doesnt work well with the most-recent Globus Toolkit. This situation is expected to improve by the beginning of 2003.  Commonly called a postage stamp in astronomical circles. Performance tests for grid components. Performance tests for Grid Components in AVO. Astrophysical Virtual Observatory, 2002 -  PAGE 2 - -  PAGE 2 - LC  CDwy  PQ]^!)JL+++++, ,(,),5,6,A,B,U,W,Z,\,m,o,~,,,,,,,,ľľľj0JCJU 5CJ\0JCJCJaJ0JB*CJphjCJUCJ jCJU6]y(jCJUmHnHsH uB.DLC  ? 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