UK E-Science Initiative and its Application to SDO J.L. Culhane MSSL

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

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” GRID PC Mainframe Space Missions Network Laptop Phone / PDA Printer

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.

How does Astrogrid work? User Web Service Web Interface Data Archive Data Storage Data Transformation & Processing Distributed Network of Registries 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 RESOURCES

Astrogrid Registry Data Archive 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 Registry Database 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

Solar Interior to Outer Atmosphere 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

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

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

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

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 Network Issues

PPARC E-Science AO Proposals due by 31 st 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

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

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

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

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What is Astrogrid? 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 Resources Datasets Processors Storage Other virtual observatories Disciplines Astrophysics Solar Physics Solar Terrestrial Physics

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.

Example: Solar / Stellar Flares 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. Solar Flare Catalogue #1 Solar Flare Catalogue #2 Yohkoh Archive Solar-B Archive XMM Archive Chandra Archive User Web Interface Merged Solar Flare List NEW: Stellar Flare Catalogue

HMI Data Archive

HMI Data Flow

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

HMI Standard Data Products

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.

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