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 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

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 TLAs – Whats 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 – 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 – 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 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

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

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 Electrons Radio VLA Compare with Radio Archives

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

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 2-D Hydrodynamic Abundant Mixing! X-Y High Resolution Brueggen & Kaiser 2002 Density

28 Non-Linear R-T Instability t = 0 Beta = 1.3 MBeta = 1.3 KBeta = 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 Fabian et al Compare with Chandra Archives

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?