1 science and the nvo – overview and discussion dave de young nvo project scientist noao nvoss...

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Science and the NVO – Science and the NVO – Overview and DiscussionOverview and Discussion

Dave De Young NVO Project Scientist

NOAO

NVOSS Aspen September 2006

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NVO Enters Its Operational NVO Enters Its Operational PhasePhase

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

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NVO and The “Two Cultures” NVO and The “Two Cultures” ProblemProblem

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NVO and The “Two Cultures” NVO and The “Two Cultures” ProblemProblem

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

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Some Requirements for Some Requirements for Community AcceptanceCommunity 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

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Some Requirements for Some Requirements for Community AcceptanceCommunity 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

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Some Requirements for Some Requirements for Community AcceptanceCommunity 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

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NVO Science – New NVO 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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NVO Science – Some NVO Science – Some ExamplesExamples

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

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NVO Science – Some NVO Science – Some ExamplesExamples

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

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NVO Science – Some NVO Science – Some ExamplesExamples

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-)

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NVO Science – Some NVO Science – Some ExamplesExamples

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

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NVO Science: Integration of NVO Science: Integration of Theory and ObservationsTheory 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

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

Goal: Translate Theory Results to Observational Parameters

Cross Match Theory “Surveys” and Observational Surveys

Interaction: Direct New Observations

Direct 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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Collimated Outflows from Collimated Outflows from AGNAGN

3C 405 – Cyg A

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Collimated Outflows from Collimated Outflows from AGNAGN

3C 175

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Collimated Outflows from Collimated Outflows from AGNAGN

3C 31

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

A 1689

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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”

N1275

Fabian et al. 2000

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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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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

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Three Dimensional MHD Three Dimensional MHD CalculationsCalculations

= 3000

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Relic Radio Bubbles in Galaxy Relic Radio Bubbles in Galaxy ClustersClusters

N1275

Fabian et al. 2000

Compare with Chandra Archives

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SummarySummary 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?