Transcript Future Catalogs James Pizagno (UW)‏

Future Catalogs
James Pizagno (UW)
How can existing catalogs be updated?
What we have..
Why?
Outline
Priority for Data Management, Science Collaborations
What Data Exist?
Areas to Update:
 Different Semi-Analytic Models of Galaxies
 Supernovae Ia
 Low Surface Brightness Galaxies
 Galactic Streams
 Dwarf Galaxies
 AGNs
 QSOs
 Lensing (weak, strong, micro)
 Planet Occultations
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Priority and Goals
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Provide images for Data Management Pipelines:
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Realistic brightness and spatial distribution
Realistic galaxy morphology
Variable objects
Moving objects
Multiple populations of stars
Science Collaborations:
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Address key science questions
Quality Assurance
Input into Image Simulation base catalog
Galaxy Models
What we need:
 Colors (SEDs), redshifts, sizes, morphology, lensing
Bower et al. 2006:
 Uses GALFORM
 Recent gas simulations
 Has morphology, high redshifts, color information
Models with varying Cosmology?
 ADDGALS (Wechsler et al.)
Durham Simulations (extension of Bower/Millennium)
Morphology
 Use HDF images and/or SDSS images?
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Faint or Extended Objects
Galactic streams:
 Input Willman-like dwarfs (Willman et al. 2005)
Low Surface Brightness galaxies:
 Analytic Size-Magnitude-Luminosity relations (Woo,
Dekel, & Courteau 2008, Schechter lum. Func.)
FITS maps
 Galaxy Interaction Tidal-Tails
 SDSS images
SPH simulations
Globular Clusters, Nebulae
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Supernovae
SN Ia:
 Rate: Dilday et al. 2008 ApJ:
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SN rate = A*mass_density(time) +B*mass_density_rate(time)
Place SN at characteristic radius
SED: Hsiao et al. 2007, ApJ, 663, 1187
 -20 to 85 days past B maximum
 0.1 o 2.5 micron coverage
Other types?
QSO and AGN and Lensing
QSO
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Add, correlation functions
AGN
 Need SED as a function of time
 Place in the center of a galaxy as a point source
Lensing
 Weak Lensing:
 Lensing software in current framework
 Strong Lensing:
 Include HST images of Lenses
 Generate multiple images using different
“views” through the Millennium Simulation
 Time Delays of variable lenses?
Planet Occultations
Well known light curves?
Statistically associate planets and stars
Will light curves drive photometric requirements?
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