1 science and the nvo – overview and discussion dave de young nvo project scientist noao nvoss...
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1 Science and the NVO Overview and Discussion Dave De Young NVO Project Scientist NOAO NVOSS Aspen September 2006 Slide 2 2 NVO Enters Its Operational Phase The First Five Years: Develop Infrastructure Basic Organizational Structure Establish Collaborations Develop Software Infrastructure (A Very Large Task) Expose Astronomers to the Concept Develop Some Astronomical Tools Goal: Simple, Readily Used Slide 3 3 NVO and The Two Cultures Problem Slide 4 4 First Five Years Infrastructure Strong Emphasis on Software Development Strong Emphasis on IT Approach NVO as a Software Sandbox Do It Because Its Cool But The Goal of the NVO Is Enabling Science Not Developing Software First Step: Acceptance by Community Slide 5 5 Some Requirements for Community Acceptance Most Astronomers DO NOT: Understand Java Understand HTML/XML Care About Elegant Code Often Use SQL Most Astronomers DO Want the Fastest, Easiest Way to Do Their Science Slide 6 6 Some Requirements for Community Acceptance Ease of Access No Jargon, No TLAs Whats a Registry? Data Ease of Access Multi-Wavelength Catalogs, Images, Spectra, Time Series Ability to Combine and Analyse Slide 7 7 Some Requirements for Community Acceptance Tools Simple, Useful 90-10 Rule Majority of Astronomers: Observers, Optical, Stellar Astronomy Role of Power Users Small Numbers, Big Projects, High Visibility Services Easy to Use, Relevant, Reliable Slide 8 8 NVO Science New Capabilities Large Scale Surveys: 1 10 Tb New Facilities: ~ 10 Tb/day High Bandwidth Data Transmission All Imply a New Paradigm for Research Cross Match of 1 10 Million Objects New Patterns in Statistics New Relations; Unseen Physical Processes Serendipity Slide 9 9 NVO Science Some Examples Radio-Loud AGN in the SDSS Best et al. 2005 Cross Match SDSS DR2, NVSS, FIRST SDSS Spectral Data 2712 Radio Galaxies Radio Emission Due to AGN vs Star Bursts Slide 10 10 NVO Science Some Examples Is There an AGN Starburst Connection? (Heckman et al.2006) Does a Common Accretion Torus Produce Both? Both Phenomena Produce X-rays Cross Correlate 80,000 X-ray Sources with > 500,000 Galaxies (with z) From SDSS DR4 Look for Common Hosts Look for Evolution with Redshift Slide 11 11 NVO Science Some Examples Detecting Embedded Intermediate Mass Stars (Kerton et al. 2006) Star of 5-10 Mo At Boundary Between Solar Type and Very Massive Stars Hence Crossover of Different Physical Processes Young B Stars Buried in Molecular Clouds Radio + mm Spectral Line Surveys + 2MASS, IRAS Data Cube Analysis (x-y- ) Slide 12 12 NVO Science Some Examples Merging Galaxies (Allam et al. 2006) Galaxy Mergers: Create Starbursts, Form Central CDs in Clusters, Feed AGN, Produce ULIRGS. Optical (SDSS) Surveys Bias toward High SFR IR Traces Mass Distribution (Red Stars) Search 2MASS XSC (1.6M Galaxies) Expect ~ 30,000 Merging Pairs Do Multi Wavelength Followup Slide 13 13 NVO Science: Integration of Theory and Observations Why Theory Basic to Scientific Inquiry Why NVO Theory Large Scale Theory Simulations: 10s of TB and Rising Virtual Telescope/Instrument Projects Slide 14 14 NVO Science: Integration of Theory and Observations Goal: Translate Theory Results to Observational Parameters Cross Match Theory Surveys and Observational Surveys Interaction: Direct New Observations Direct New Theory Work Slide 15 15 N Body Simulations of Globular Cluster Evolution Slide 16 16 N Body Simulations of Globular Cluster Evolution Slide 17 17 Collimated Outflows from AGN M 87 Slide 18 18 Collimated Outflows from AGN 3C 405 Cyg A Slide 19 19 Collimated Outflows from AGN 3C 175 Slide 20 20 Collimated Outflows from AGN 3C 31 Slide 21 21 MHD Simulations of Collimated Outflows from AGN Virtual Telescope Observations Electrons Radio VLA Compare with Radio Archives Slide 22 22 MHD Simulations of Collimated Outflows from AGN Virtual Telescope Observations IC-CMB Chandra SSC Compare with Chandra Archives Slide 23 23 Clusters of Galaxies and Cooling Flows A 1689 Slide 24 24 Clusters of Galaxies and Cooling Flows Perseus Cluster Slide 25 25 Clusters of Galaxies and the Cooling Flow Problem N1275 Fabian et al. 2000 Slide 26 26 Clusters of Galaxies and the Cooling Flow Problem Can Reheating of the Intracluster Medium by AGN Solve the Cooling Flow Problem? Slide 27 27 Models of Buoyant Radio Source Bubbles 2-D Hydrodynamic Abundant Mixing! X-Y High Resolution Brueggen & Kaiser 2002 Density Slide 28 28 Non-Linear R-T Instability t = 0 Beta = 1.3 MBeta = 1.3 KBeta = 130 1 kpc slices T = 10M K t = 15 Myr Slide 29 29 Evolution of Cluster Bubbles Including MHD Beta = 120 Slide 30 30 Three Dimensional MHD Calculations = 3000 Slide 31 31 Relic Radio Bubbles in Galaxy Clusters N1275 Fabian et al. 2000 Compare with Chandra Archives Slide 32 32 Summary To Date: VO Establishes Infrastructure Almost Done Tomorrow: VO Enables New Science The Transition is Now Carry Forward Infrastructure Development Change Culture to Science Implementation Engage Astronomical Community What Science do YOU Want to Do?