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

=

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Orsi

Semi - analytical model

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GALFORM

Cold Gas

Mstar

Mcold

SFRRdisk,bulge

Disk/bulge radius

Mvir

Virial mass

ZMetallicity

LLy↵0

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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

⟶⟶

⟶ ⟶⟶

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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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