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