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Science and the VO – Science and the VO – Overview and DiscussionOverview and Discussion

Dave De Young NVO Project Scientist

NOAO

NVOSS Santa Fe

September 2008

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NVO Enters its Operational NVO Enters its Operational PhasePhase

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

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VO Science – New VO Science – New CapabilitiesCapabilities

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

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VO Science – Some VO Science – Some ExamplesExamples

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

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VO Science – Some VO Science – Some ExamplesExamples

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

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VO Science – Some VO Science – Some ExamplesExamples

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-)

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VO Science – Some VO Science – Some ExamplesExamples

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

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VO Science: Integration of VO Science: Integration of Theory and ObservationsTheory and Observations

Theory <=> Astrophysics– Basis for All Observations

NVO Theory– Large Scale Theory Simulations: 10’s of

TB and Rising– “Virtual Telescope/Instrument” Projects

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VO Science: Integration of VO Science: Integration of Theory and ObservationsTheory and Observations

Goal: Translate Theory Results to Observational Parameters

Cross Match Theory “Surveys” and Observational Surveys

Interaction: Guide New Observations

Guide New Theory Work

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N Body Simulations of N Body Simulations of Globular Cluster EvolutionGlobular Cluster Evolution

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N Body Simulations of N Body Simulations of Globular Cluster EvolutionGlobular Cluster Evolution

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Collimated Outflows from Collimated Outflows from AGNAGN

M 87

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AGN OutflowsAGN Outflows

3C 405/Cyg A – Not “typical”

Radio Galaxy

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AGN Outflows AGN Outflows

3C 175 FR II

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AGN OutflowsAGN Outflows

3C 273 – The Power of Multi-wavelength Observations

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AGN OutflowsAGN Outflows

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Large Scale AGN OutflowsLarge Scale AGN Outflows

Harris & Krawczynski 2006

Siemiginowska et al. 2007, 2008

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Large Scale X-Ray JetsLarge 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

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MHD Simulations of Collimated MHD Simulations of Collimated Outflows from AGN – Virtual Outflows from AGN – Virtual

Telescope ObservationsTelescope Observations

Electrons

Radio

VLACompare with Radio Archives

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MHD Simulations of Collimated MHD Simulations of Collimated Outflows from AGN – Virtual Outflows from AGN – Virtual

Telescope ObservationsTelescope Observations

IC-CMB

Chandra

SSC

Compare with Chandra Archives

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Galaxy Formation and Galaxy Formation and EvolutionEvolution

Millennium Simulation

1 x 10 Particles; 500 Mpc10 3

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Galaxy Formation and Galaxy Formation and Evolution – “Feedback”Evolution – “Feedback”

Bower et al. 2003

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Galaxy Formation and Galaxy Formation and Evolution – Radio AGN Evolution – Radio AGN

“Feedback”“Feedback”– Effects of Radio AGN

Croton et al. 2006

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AGN Outflows and FeedbackAGN Outflows and Feedback

3C 31 – FR I

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Extended Extragalactic Radio Extended Extragalactic Radio Sources - DemographicsSources - 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

-4

-6

-3

-3

-3

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Outflow Interaction with Outflow Interaction with Ambient Medium – “Feedback”Ambient Medium – “Feedback” Fully Non-Linear K-H Instability:

– Development of Turbulent Mixing Layer

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Mixing LayersMixing Layers Thickness Grows with Distance/Time

Mixing Layer Can Permeate Entire Jet

-RELHL )(v)/( CTan

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Mixing LayersMixing Layers

K-H Instability and Mixing Layers in Supersonic Flows

And in Relativistic Flows

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Saturated Mixed Jet ModelsSaturated Mixed Jet Models Empirical – Symmetric, Decelerating, Adiabatic

Laing & Bridle 2004

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Evolution of Turbulent FlowsEvolution of Turbulent Flows

Development of the Turbulent Cascade

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VO Science – Some VO Science – Some ExamplesExamples

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

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Clusters of Galaxies and Clusters of Galaxies and “Cooling Flows”“Cooling Flows”

A 1689

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Clusters of Galaxies and the Clusters of Galaxies and the “Cooling Flow Problem”“Cooling Flow Problem”

Can Reheating of the Intracluster Medium

by AGN “Solve” the

Cooling Flow

Problem?

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Clusters of Galaxies and Clusters of Galaxies and “Cooling Flows”“Cooling Flows”

Perseus Cluster

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Clusters of Galaxies and the Clusters of Galaxies and the “Cooling Flow Problem”“Cooling Flow Problem”

z ~ 0.6

pV ~ 10 erg!62

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Models of Buoyant Radio Models of Buoyant Radio Source BubblesSource Bubbles

2-D Hydrodynamic

Abundant

Mixing!

X-Y High Resolution

Brueggen & Kaiser 2002

Density

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Non-Linear R-T InstabilityNon-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

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Evolution of Cluster Bubbles Evolution of Cluster Bubbles Including MHDIncluding MHD

Beta = 120, 3000; 2D

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Three Dimensional MHD Three Dimensional MHD CalculationsCalculations

= 3000

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Consistency with Consistency with ObservationsObservations

= 120

= 3000

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SummarySummary 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?