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

2. 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. 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. 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. 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. 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. 7 VO Science – Some Examples Merging Galaxies (Allam et al.) – 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

8. 8 VO Science: Integration of Theory and Observations Theory Astrophysics – Basis for All Observations NVO Theory – Large Scale Theory Simulations: 10s of TB and Rising – Virtual Telescope/Instrument Projects

9. 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. 10 N Body Simulations of Globular Cluster Evolution

11. 11 N Body Simulations of Globular Cluster Evolution

12. 12 Collimated Outflows from AGN M 87

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

14. 14 AGN Outflows 3C 175 FR II

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

16. 16 AGN Outflows

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

18. 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. 19 MHD Simulations of Collimated Outflows from AGN – Virtual Telescope Observations Electrons Radio VLA Compare with Radio Archives

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

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

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

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

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

25. 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 -2-2 -4 -6 -3

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

27. 27 Mixing Layers Thickness Grows with Distance/Time Mixing Layer Can Permeate Entire Jet - RELHL )(v)/( CTan

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

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

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

31. 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. 32 Clusters of Galaxies and Cooling Flows A 1689

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

34. 34 Clusters of Galaxies and Cooling Flows Perseus Cluster

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

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

37. 37 Non-Linear R-T Instability t = 0 Beta = 1.3 MBeta = 1.3 KBeta = 130 1 kpc slices T = 10M K t = 15 Myr

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

39. 39 Three Dimensional MHD Calculations = 3000

40. 40 Consistency with Observations Consistency with Observations = 120 = 3000

41. 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?