End to End End to End SimulationsSimulations
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What’s this ?
This is the MUSE
datacube of NGC 1068 we just received
from ESOCan you
remind me how many
students we have left ?
p.3
End to End ModellingEnd to End Modelling
Data Reduction System
Atmos. & AO simulations
Astro. Scene Simulations
Instrument Numerical Model
Data Analysis Software Tools
Validation
Prototype OKWFM OKNFM Apr 09
Tools & format releasedStars & Galaxies Fields
First releasedDec 09 ?
AO PSF modelingWFM OKNFM Apr 09
Quick Simulation
QSIM OKStars & Galaxies Datacube
ANR DAHLIA 09-12
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Data FormatData Format
Raw data– Fits file– 0: header extension– 1..24: image extensions
Reduced data– Fits file– 0: header extension– 1: 3D data extension (3D image :x:y)– 2: 3D variance extension – 3: 3D bad pixel flag
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ProcessProcess
Semi-analytical model of galaxy formation (Jeremy)
Datacubes at MUSE spatial and spectral resolution
Noisy datacubesAnalysis
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Semi-analytical Semi-analytical model of galaxy model of galaxy
formation (1)formation (1)Millennium simulation (De Lucia & Blaizot, 2007; Springel et al., 2005)
SAM (dark matter halo -> galaxies)– Catalog selection
K < 31 & FOV=1.2x1.2 arcmin²
– Output X, Y, Rdisk, B/T ratio, Star formation history
Image creation– Exponential disk + Bulge (Hernquist) light
profile– Random orientation and PA of the disk
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Semi-analytical Semi-analytical model of galaxy model of galaxy
formation (2)formation (2) Spectra– Stellar population absorption lines– Lyman-alpha lines from HII regions ionized
by young stars Voigt template (absorption + emission) EW(z=0) 150 A Normalized to get the correct count at z~3 ?
– Other nebular emission lines from Charlot & Longhetti 2001 Input parameters: Z, effective ionization, dust-to-
heavy elements -> emission line template
– Dust attenuation
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Input datacubeInput datacube
Disk HR imageBulge HR imageFor each image
– LR Continnuum + absorption line images
– Emission line tables (lambda, flux, sigma)
– Lyman alfa profile (to be x by the continuum)
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MUSE datacube MUSE datacube creation (1)creation (1)
Process each objectConvolve by appropriate spectral PSF
– Function of x,y
Convolve by appropriate spatial PSF– No AO: MOFFAT seeing model f(lambda)– AO: MOFFAT AO model f(lambda, x, y)
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MUSE datacube MUSE datacube creation (2)creation (2)
Add atmosphere– Continuum + OH emission lines f(moon)
+ random variation OH– Absorption f(airmass)
Convert in count– Throughput
Add noise– Photon, dark current, readout
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ComputingComputing
SAM– Output: 1600 galaxies– CPU time ?– Disk size: 36 Mo
Data cube creation (1)– 80 exposures with different atmospheric conditions– CPU time: 80x8.5 = 28 days– Disk size: 80x1.3 = 104 Go
Data cube creation (2)– 80 exposures of 1 hour– CPU time: 80x1.5 hour = 5 days– Disk size: 80x2.6 Go = 208 Go
Analysis ?
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Deep-Field Deep-Field SimulationSimulation
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Spatially Resolved Spatially Resolved Galaxies FieldGalaxies Field
20 arcsec
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Dense Stellar FieldDense Stellar Field
1 arcmin
20 arcsec
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