Siddhartha Gurung López
Estructura A Gran Escala Del Universo A Alto Desplazamiento Al
Rojo En La Era De Los Cartografiados Cosmológicos De Galaxias
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Alvaro Orsi, Silvia Bonoli
Supervisors
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Orsi
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Helmut Meusinger
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Some future surveys will use Lyα emitters to constrain cosmology
Lyα will be easily detected in many future surveys
Lyα Radiative Transfer in Galaxies
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Expanding homogenous thin shell
Lyα Radiative Transfer in Galaxies
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😀
Expanding homogenous thin shell
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Lyα Radiative Transfer in the IGM
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Intergalactic mediumGalaxy Observer
HI
LLy↵
0 ⇥ fgalaxy
esc
f IGMesc⇥ LLy↵
obs
=
8
Orsi
Semi - analytical model
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GALFORM
Cold Gas
Mstar
Mcold
SFRRdisk,bulge
Disk/bulge radius
Mvir
Virial mass
ZMetallicity
LLy↵0
⟶
⟶
⟶ ⟶⟶
⟶
Intrinsic luminosity
Monte Carlo Radiative Transfer Code
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GeometryColumn density
Expansion velocityDust content
Number of photons
Monte Carlo radiative transfer
code
Escape fraction Line profile
time = 1h/galaxy ⇥ 3 · 106galaxies = 3 · 106h
Input parameter grid MCMC Analytic expression time ⇠ 1s
GEOMETRIES
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Thin Shell
GEOMETRIES
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Wind
GEOMETRIES
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Biconical Wind
Lyα Radiative Transfer
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Escape fraction Line shape
Semi - analytical model
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GALFORMCold Gas
Mstar
Mcold
SFR Rdisk,bulge
Disk/bulge radius
MvirVirial mass
ZMetallicity
LLy↵0
⟶⟶
⟶ ⟶⟶
⟶
Intrinsic luminosity
Vexp
= V
Mstar
Mvir
Rvir
NHI = NMcold
R
2disk/bulge
Intergalactic medium
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Laursen et. al. 2011
Intergalactic medium
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Luminosity Function
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Correlation Function
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GRACIAS !! 😀
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Escape Fraction Uncertainties
Lyα Radiative Transfer
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Expanding homogenous sphere Expanding homogenous thin shell
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