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Science and the VO – Overview and Discussion

Science and the VO – Overview and Discussion. Dave De Young NVO Project Scientist NOAO. NVOSS Santa Fe September 2008. NVO Enters its Operational Phase. First Six Years – Infrastructure

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Science and the VO – Overview and Discussion

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  1. Science and the VO – Overview and Discussion Dave De Young NVO Project Scientist NOAO NVOSS Santa Fe September 2008

  2. NVO Enters its Operational Phase • First Six Years – Infrastructure • Strong Emphasis on Software Development • Strong Emphasis on IT Approach • NVO as a “Software Sandbox” • But – The Goal of the NVO Is Enabling Science - Not Developing Software • First Step: Acceptance by Community

  3. VO 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

  4. VO Science – Some Examples • Radio-Loud AGN in the SDSS • Best et al. • Cross Match SDSS DR2, NVSS, FIRST • SDSS Spectral Data • 2712 Radio Galaxies • Radio Emission Due to AGN vs Star Bursts

  5. VO Science – Some Examples • Is There an AGN – Starburst Connection? • (Heckman et al.) • 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

  6. VO Science – Some Examples • Detecting Embedded Intermediate Mass Stars • (Kerton et al. ) • 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-)

  7. VO Science – Some Examples • Merging Galaxies • (Allam et al.) • 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

  8. VO Science: Integration of Theory and Observations • Theory <=> Astrophysics • Basis for All Observations • NVO Theory • Large Scale Theory Simulations: 10’s of TB and Rising • “Virtual Telescope/Instrument” Projects

  9. VO Science: Integration of Theory and Observations • Goal: Translate Theory Results to Observational Parameters • Cross Match Theory “Surveys” and Observational Surveys • Interaction: Guide New Observations Guide New Theory Work

  10. N Body Simulations of Globular Cluster Evolution

  11. N Body Simulations of Globular Cluster Evolution

  12. Collimated Outflows from AGN • M 87

  13. AGN Outflows • 3C 405/Cyg A – Not “typical” Radio Galaxy

  14. AGN Outflows • 3C 175 FR II

  15. AGN Outflows 3C 273 – The Power of Multi-wavelength Observations

  16. AGN Outflows

  17. Large Scale AGN Outflows Harris & Krawczynski 2006 Siemiginowska et al. 2007, 2008

  18. Large Scale X-Ray Jets • The IC/CMB Model • Tavecchio et al. 2000, Celotti et al. 2001 • PKS 0637-752: Γ ~ 10 • Reproduces SED • Has Three Basic Assumptions • Equipartition Conditions • Relativistic Motion on 10-100 Kpc Scales • Population of Low Energy electrons Schwartz et al. 2000

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

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

  21. Galaxy Formation and Evolution • Millennium Simulation 10 3 1 x 10 Particles; 500Mpc

  22. Galaxy Formation and Evolution – “Feedback” Bower et al. 2003

  23. Galaxy Formation and Evolution – Radio AGN “Feedback” • Effects of Radio AGN Croton et al. 2006

  24. AGN Outflows and Feedback • 3C 31 – FR I

  25. Extended Extragalactic Radio Sources - Demographics • Space Densities: (to z ~ 0.3) • Spiral Galaxies: ~ 3 x 10 Mpc • FR-I Sources: ~ 3 x 10 Mpc • FR-II Sources: ~ 1 x 10 Mpc • Thus FR-I Objects are > 100 Times More Common than FR-II Objects -2 -3 -4 -3 -6 -3

  26. Outflow Interaction with Ambient Medium – “Feedback” • Fully Non-Linear K-H Instability: • Development of Turbulent Mixing Layer

  27. a b f = r r - Tan C ( / ) (v ) L H REL Mixing Layers • Thickness Grows with Distance/Time • Mixing Layer Can Permeate Entire Jet

  28. Mixing Layers • K-H Instability and Mixing Layers in Supersonic Flows • And in Relativistic Flows

  29. Saturated Mixed Jet Models • Empirical – Symmetric, Decelerating, Adiabatic Laing & Bridle 2004

  30. Evolution of Turbulent Flows • Development of the Turbulent Cascade

  31. VO Science – Some Examples • Radio-Loud AGN in the SDSS • (Best et al. 2005) Mandelbaum et al. 2008 • Cross Match SDSS (DR2)DR4, NVSS, FIRST • SDSS Spectral Data • (2712)5712 Radio Galaxies • Radio Emission Due to AGN vs Star Bursts

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

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

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

  35. Clusters of Galaxies and the “Cooling Flow Problem” • z ~ 0.6 • pV ~ 10 erg! 62

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

  37. 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

  38. Evolution of Cluster Bubbles Including MHD Beta = 120, 3000; 2D

  39. Three Dimensional MHD Calculations •  = 3000

  40. Consistency with Observations  = 3000  = 120

  41. Summary • To Date: VO Establishes Infrastructure • Basically 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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