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End to End Simulations

End to End Simulations. What’s this ?. This is the MUSE datacube of NGC 1068 we just received from ESO. Can you remind me how many students we have left ?. Instrument Numerical Model. Astro. Scene Simulations. Validation. Data Analysis Software Tools. Data Reduction System.

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End to End Simulations

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  1. End to End Simulations

  2. What’s this ? This is the MUSE datacube of NGC 1068 we just received from ESO Can you remind me how many students we have left ?

  3. Instrument Numerical Model Astro. Scene Simulations Validation Data Analysis Software Tools Data Reduction System End to End Modelling Prototype OK WFM OK NFM Apr 09 AO PSF modeling WFM OK NFM Apr 09 Tools & format released Stars & Galaxies Fields Atmos. & AO simulations QSIM OK Stars & Galaxies Datacube Quick Simulation First released Dec 09 ? ANR DAHLIA 09-12

  4. Data 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 l:x:y) • 2: 3D variance extension • 3: 3D bad pixel flag

  5. Process • Semi-analytical model of galaxy formation (Jeremy) • Datacubes at MUSE spatial and spectral resolution • Noisy datacubes • Analysis

  6. Semi-analytical model of galaxy formation (1) • Millennium simulation (De Lucia & Blaizot, 2007; Springel et al., 2005) • SAM (darkmatter 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

  7. Semi-analytical model of galaxy 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-heavyelements -> emission line template • Dust attenuation

  8. Input datacube • Disk HR image • Bulge HR image • For each image • LR Continnuum + absorption line images • Emission line tables (lambda, flux, sigma) • Lyman alfa profile (to be x by the continuum)

  9. MUSE datacubecreation (1) • Process each object • Convolve 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)

  10. MUSE datacubecreation (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

  11. Computing • SAM • Output: 1600 galaxies • CPU time ? • Disk size: 36 Mo • Data cube creation (1) • 80 exposureswithdifferentatmospheric 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 ?

  12. Deep-Field Simulation

  13. SpatiallyResolved Galaxies Field 20 arcsec

  14. Dense Stellar Field 20 arcsec 1 arcmin

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