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 ?

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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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