Future Catalogs James Pizagno (UW)
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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
Priority and Goals
Provide images for Data Management Pipelines:
Realistic brightness and spatial distribution
Realistic galaxy morphology
Variable objects
Moving objects
Multiple populations of stars
Science Collaborations:
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?
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
Supernovae
SN Ia:
Rate: Dilday et al. 2008 ApJ:
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
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?