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Science and the NVO – Overview and Discussion

The National Virtual Observatory (NVO) represents a significant endeavor to enhance astronomical research by developing a robust infrastructure. In its first five years, the NVO focused on creating an organizational framework, fostering collaborations, and building essential software tools for astronomers. Emphasizing user accessibility, the project aims to simplify data access and analysis across multiple wavelengths. By addressing the “Two Cultures” problem in science, the NVO strives to connect theoretical findings with observational data, enabling more meaningful research and discoveries in astronomy.

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Science and the NVO – Overview and Discussion

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  1. Science and the NVO – Overview and Discussion Dave De Young NVO Project Scientist NOAO NVOSS Aspen September 2006

  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

  3. NVO and The “Two Cultures” Problem

  4. NVO and The “Two Cultures” Problem • First Five Years – Infrastructure • Strong Emphasis on Software Development • Strong Emphasis on IT Approach • NVO as a “Software Sandbox” • Do It Because “It’s Cool” • But – The Goal of the NVO Is Enabling Science Not Developing Software • First Step: Acceptance by Community

  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

  6. Some Requirements for Community Acceptance • Ease of Access • No Jargon, No TLA’s • “What’s a ‘Registry’”? • Data • Ease of Access • Multi-Wavelength • Catalogs, Images, Spectra, Time Series • Ability to Combine and Analyse

  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

  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

  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

  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

  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-)

  12. NVO Science – Some Examples • Merging Galaxies • (Allam et al. 2006) • Galaxy Mergers: Create Starbursts, Form Central CD’s 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

  13. NVO Science: Integration of Theory and Observations • Why Theory • Basic to Scientific Inquiry • Why NVO Theory • Large Scale Theory Simulations: 10’s of TB and Rising • “Virtual Telescope/Instrument” Projects

  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

  15. N Body Simulations of Globular Cluster Evolution

  16. N Body Simulations of Globular Cluster Evolution

  17. Collimated Outflows from AGN • M 87

  18. Collimated Outflows from AGN • 3C 405 – Cyg A

  19. Collimated Outflows from AGN • 3C 175

  20. Collimated Outflows from AGN • 3C 31

  21. MHD Simulations of Collimated Outflows from AGN – Virtual Telescope Observations Radio Electrons Compare with Radio Archives VLA

  22. MHD Simulations of Collimated Outflows from AGN – Virtual Telescope Observations IC-CMB SSC Compare with Chandra Archives Chandra

  23. Clusters of Galaxies and “Cooling Flows” • A 1689

  24. Clusters of Galaxies and “Cooling Flows” • Perseus Cluster

  25. Clusters of Galaxies and the “Cooling Flow Problem” • N1275 Fabian et al. 2000

  26. Clusters of Galaxies and the “Cooling Flow Problem” • Can Reheating of the Intracluster Medium by AGN “Solve” the Cooling Flow Problem?

  27. Models of Buoyant Radio Source Bubbles Density • 2-D Hydrodynamic • Abundant Mixing! X-Y High Resolution Brueggen & Kaiser 2002

  28. Non-Linear R-T Instability t = 0 Beta = 1.3 M Beta = 1.3 K Beta = 130 1 kpc slices T = 10M K t = 15 Myr

  29. Evolution of Cluster Bubbles Including MHD Beta = 120

  30. Three Dimensional MHD Calculations •  = 3000

  31. Relic Radio Bubbles in Galaxy Clusters • N1275 Compare with Chandra Archives Fabian et al. 2000

  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?

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