SLIDE 1
OU-LE3 simulation needs
- Returns from
- Clusters of galaxies - implementation
- A. Biviano, S. Maurogordato, C. Benoist, S. Borgani, G.
De Lucia.
- Time domain
- I. Hook
- Weak lensing – validation
- R. Nakajima
OU-LE3 Simulation needs Carlton Baugh Institute for Computational - - PowerPoint PPT Presentation
OU-LE3 Simulation needs Carlton Baugh Institute for Computational - - PowerPoint PPT Presentation
OU-LE3 Simulation needs Carlton Baugh Institute for Computational Cosmology Durham University OU-LE3 simulation needs Returns from Clusters of galaxies - implementation A. Biviano, S. Maurogordato, C. Benoist, S. Borgani, G. De Lucia.
SLIDE 2
SLIDE 3
Generic needs
- Emission line properties
Line flux, equivalent width
- Broad photometry to AB~24-24.5
Euclid NIR Euclid VIS Pan-STARRS griz DES grizy CFHTLS ugriyz WFCAM ZYJHK SDSS ugriz VISTA-VHS-VIDEO ZYJHKs
SLIDE 4
Generic needs
- Simulated photo-z catalogue
SLIDE 5
Specific needs – clusters of galaxies
- DM haloes M>1.e+13Msun, r(D), D=2500,
500,200; velocity dispersion along axes from DM particles
- For each galaxy host halo ID, central or sat?
- Simulated images for cluster detection and
mass determination through weak/strong lensing
- Do need require full instrumental response at
this stage
SLIDE 6
Specific needs: weak lensing
- Galaxies and DM to generate kappa map
- Galaxy shapes with noise (no IA)
- Galaxy shapes with IA
- Shear at each galaxy position
- Image properties:
mask, bright stars, chip boundaries, CCD defects, ghosts, variations in depth & background
SLIDE 7
Specific needs: Time Domain
- Science areas: SNe, exo-planets, solar system
- Time series of VIS and NISP Y, J, H images
- Add fake transients with realistic properties
(lightcurves, colours, positions) – properties to be supplied by Time Domain scientists
- Images should be pre-processed (bias corrected,
flat fielded and sky subtracted). Individual dithered frames should be available so that an
- versampled reference image can be constructed.
SLIDE 8
Specific needs: time domain
Images should tile the following areas
- a few arcmin in a crowded stellar field
(exoplanets case)
- ~1 sq deg in a high galactic latitude field (for
the SN case).
- ~100 sq deg covering the range of stellar
densities and galaxy cluster backgrounds that are expected (for the solar system case)
SLIDE 9
Specific needs: time domain
- Simulated NISP spectroscopy of a subset of
the areas above
- both time-resolved and stacked images.