UK E-Science Initiative and its Application to SDO

1. UK E-Science Initiativeand itsApplication to SDO J.L. Culhane MSSL

2. SUMMARY • The UK Astrogrid • Dealing with SDO Data Volumes • The PPARC E-Science AO • HMI Data Products and Pipeline

3. What is the Grid? • Ian Foster, Argonne National Lab & University of Chicago • “A Grid is a system that: • Coordinates resources that are not subject to centralized control. • Uses standard, open, general-purpose protocols and interfaces. • Delivers nontrivial qualities of service.” • - Ian Foster, “What is the Grid? A Three Point Checklist” Network PC Laptop Mainframe Phone / PDA Space Missions GRID Printer

4. UK Astrogrid • Astrogrid is one of three major world-wide projects (along with European AVO and US-VO projects) which aim to create an astronomical Virtual Observatory • Astrogrid has a significant Solar Physics component • The Virtual Observatory will be a set of co-operating and interoperable software systems that: • allow users to interrogate multiple data centres in a seamless and transparent way; • provide powerful new analysis and visualisation tools; • give data centres a standard framework for publishing and delivering services using their data.

5. How does Astrogrid work? Web Service: “A web service is any piece of software that makes itself available over the Internet and uses a standardized XML messaging system.” - Ethan Cerami, “Top Ten FAQs for Web Services”, The O’Reilly Network Web Service Data Archive User Web Interface RESOURCES Web Service Web Service Data Storage Web Service Distributed Network of Registries Data Transformation & Processing

6. Astrogrid Registry Data Archive Registry Database Data Storage Data Transformation Distributed Network of Registries Registry: “Dynamic database of metadata describing a set of Internet-available resources. A registry is used to identify and locate resources satisfying user-specified criteria, and to direct more detailed information requests to the relevant services. Robert Hanisch, STSCI • METADATA: • Basic: ID, title, service type • Curation: Location, contact, publisher, creator, etc. • Metadata: Allowed methods, input / output variables, etc. • Metadata Format: Wavelength, coordinates, instrument coverage… Registries contain information about resources

7. Solar Interior to Outer Atmosphere • Science goal: Connect observations of the interior to fluctuations in the solar atmosphere • Data Required: Helioseismology observations connected with solar atmosphere observations • Current difficulties: Being able to search efficiently for solar atmospheric events that may be responding to an excitation source in the interior • Grid future: Ability to: • Search easily for events e.g. flux emergence, AR evolution, flares, coronal mass ejections, over specific time periods • Extract parameters over the cycle from the atmosphere and interior in order to compare their evolution • Crucial for SDO to relate convection zone observations to magnetic field data for Photosphere and above

8. SDO HMI Archiving and Processing • SDO instruments generate raw data (~ 2 Tbyte/day) along with derived products • Derived products result from pipeline processing that must keep up with the flow of incoming data • GRID or Virtual Observatory approach could allow: • Distributed data holding • Distributed processing capability • Network bandwidths and processing power at single sites set limits: • Available network bandwidths for users could limit data transfer from/between multiple archives • All data at one site implies considerable processing power accessible by many distributed users

9. Distributed Archive Approach • Multiple copies of the data desirable • Needs a minimum of two geographically separated sources with the advantages: • Greater resilience in ability to supply users • Load sharing between different providers (network and processing) • Avoids need for single site to provide excessive processing power

10. Single Archive Approach • Solar data normally stored in a raw form and need to be processed before use • Processing involves extraction and calibration of selected observations. • For data (e.g. helioseismology data) involving extended time intervals, processing data at source is desirable • Advantages that result: • Reduced amount of information to be returned to user • Affords the instrument teams more control over the processing and quality of their data products but • Heavy loading of processors at single archive site unless requests are for high-level lower-volume data products

11. Network Issues • UK has “SuperJanet” backbone currently at 10 Gbps • Local access points operate at 2.5 Gbps (e.g. UCL interconnect rate to backbone) • Europe has “Geant” backbone at 10 Gbps covering UK, France, Germany,Sweden, Switzerland with 2.5 Gbps local interconnects • Transatlanic connection to Geant currently 2.5 Gbps with upgrade to 10 Gbps planned for 2004 • Discussion of “Global” 1 Tbps network by 2006?? • Geant driven in part by needs of HEP community for LHC – hence SDO may not have a problem in moving data between sites

12. PPARC E-Science AO • Proposals due by 31st May, 2003 • Existence of first level Astrogrid infrastructure assumed • Proposals should: • Be for the application of infrastructure and related techniques to “real” data sets • Underpin science but close connection between projects and the science programme is essential • Demonstrate an enabling role for eventual science exploitation • Ensure development of standards and deployment of Grid infrastructure • SDO bid is now anticipated by PPARC

13. HMI Data Analysis Pipeline Processing HMI Data Internal rotation Ω(r,Θ) (0<r<R) Spherical Harmonic Time series To l=1000 Heliographic Doppler velocity maps Filtergrams Mode frequencies And splitting Internal sound speed, cs(r,Θ) (0<r<R) Full-disk velocity, v(r,Θ,Φ), And sound speed, cs(r,Θ,Φ), Maps (0-30Mm) Local wave frequency shifts Ring diagrams Doppler Velocity Carrington synoptic v and cs maps (0-30Mm) Time-distance Cross-covariance function Tracked Tiles Of Dopplergrams Wave travel times High-resolution v and cs maps (0-30Mm) Egression and Ingression maps Wave phase shift maps Deep-focus v and cs maps (0-200Mm) Far-side activity index Stokes I,V Line-of-sight Magnetograms Line-of-Sight Magnetic Field Maps Stokes I,Q,U,V Full-disk 10-min Averaged maps Vector Magnetograms Fast algorithm Vector Magnetic Field Maps Vector Magnetograms Inversion algorithm Coronal magnetic Field Extrapolations Tracked Tiles Coronal and Solar wind models Tracked full-disk 1-hour averaged Continuum maps Continuum Brightness Solar limb parameters Brightness feature maps Brightness Images Version 1.2w Net Access/ Mirror Enabling Code/ Algorithms Data Product HMI SRR/SCR Presentation April 8-10

14. HMI Science Data Analysis Plan Science Exploitation HMI SRR/SCR Presentation April 8-10

15. HMI Data Volumes Net Access HMI SRR/SCR Presentation April 8-10

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17. What is Astrogrid? • Resources • Datasets • Processors • Storage • Other virtual observatories • Disciplines • Astrophysics • Solar Physics • Solar Terrestrial Physics Astrogrid is a £5 M data grid project that will link data archives, resources, and disciplines from UK space institutions into a virtual observatory. • Data Archives • Mullard Space Science Laboratory • Rutherford Appleton Laboratory • University of Cambridge • University of Leicester • Royal Observatory Edinburgh • Queens University Belfast • Jodrell Bank Observatory

18. GRID/Virtual Observatory Within a virtual observatory: • Not required for all datasets to be stored at a single site • Metadata and registries allow system to handle a distributed archive. • Different organisations or countries could host the different datasets or different parts of the datasets (e.g. split by time). • Complete catalogues relating to particular datasets should be held wherever the data are held. • Distributed data holding reduces the pressure on: • Network connection to an archive • Processing capabilities needed at the archive site • Most accessed data could be selectively copied to distributed archives e.g. EGSO, Astrogrid • Derived data products should be held at distributed sites • Material needed for more detailed searches should be described by metadata in appropriate registries.

19. Example: Solar / Stellar Flares Solar Flare Catalogue #1 Solar Flare Catalogue #2 Yohkoh Archive Solar-B Archive XMM Archive Chandra Archive Science Problem: A solar physicist studying the flare mechanism would like to gather data on both solar and stellar flares. Data Required:X-ray datasets: lightcurves, spectra, and redshift / blueshift information from SOHO, Yokhoh, EXOSAT, ROSAT, XMM, Chandra, etc. Current Issues: No stellar flare catalogue (at time of science problem writing), datasets provided by several different archives with no common interface. NEW: Stellar Flare Catalogue Merged Solar Flare List User Web Interface

20. HMI Data Archive

21. HMI Data Flow

22. HMI Dataflow Concept HMI SRR/SCR Presentation April 8-10

23. HMI Standard Data Products

24. UK Astrogrid Scientific Aims • Improve the quality, efficiency, ease, speed, and cost-effectiveness of on-line astronomical research • Make comparison and integration of data from diverse sources seamless and transparent • Remove data analysis barriers to interdisciplinary research • Make science involving manipulation of large datasets as easy and as powerful as possible.

25. UK Astrogrid Practical Goals • Develop, with our IVOA partners (including European Grid of Solar Observations/EGSO), internationally agreed standards for data, metadata, data exchange and provenance • Develop a software infrastructure for data services • Establish a physical grid of resources shared by AstroGrid and key data centres • Construct and maintain an AstroGrid Service and Resource Registry • Implement a working Virtual Observatory system based around key UK databases and of real scientific use to astronomers • Provide a user interface to that VO system • Provide, either by construction or by adaptation, a set of science user tools to work with that VO system • Establish a leading position for the UK in VO work