peter laursen supervisor: anja c. andersen
DESCRIPTION
Dust in Young Galaxies. Peter Laursen Supervisor: Anja C. Andersen. www.dark-cosmology.dk DARK Cosmology Centre | Niels Bohr Institutet | Københavns Universitet. The code. Radiative transfer. Monte Carlo. Results. Surface brightness maps. Results. Surface brightness maps - PowerPoint PPT PresentationTRANSCRIPT
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www.dark-cosmology.dk DARK Cosmology Centre | Niels Bohr Institutet | Københavns Universitet
Peter Laursen
Supervisor: Anja C. Andersen
Dust in Young Galaxies
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The code
Radiative transfer
Monte Carlo
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ResultsSurface brightness maps
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ResultsSurface brightness maps
Surface brightnessprofiles
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ResultsSurface brightness maps
Surface brightnessprofiles
Spectra
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Dust in Young Galaxies
Star formationDust formationDust destructionRadiative transfer
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Dust in Young Galaxies
Dust Extinction in Starburst Galaxies at z = 3 – 6
Dust Creation in Supernova Explosions
Lyman Galaxies at z = 8.8
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Dust Extinction in Starburst
Galaxies at z = 3 - 6Lyman-Break Galaxies:
SFR = 10 – 1000 M☼ yr-1
Correcting for dust with Calzetti ext. curve: SFR increases a factor of 2 – 5
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Dust Extinction in Starburst
Galaxies at z = 3 - 6
Advance Monte Carlo code
Predict effect of dust as function of tsf, Z and z Very young starbursts: No AGBs, intense UV field
Analyze and model SED of LBGs from GOODS z = 2 – 6; X-rays to mid-IR
and Ultra-VISTA (COSMOS field)
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Dust Creation in Supernova Explosions
No AGB stars SNe?
Grain formation and growth in SN remnants
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Lyman Galaxies at z = 8.8
~no sky-lines in the near-IRe.g., = 1.2 m
Simulate morphology and SB of statistical sample
Compare with VISTA observations