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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?
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