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lyman alpha and ionizing radiative transfer in simulations of high-z galaxies
model MW3 ceverino et al. (2010)
lyman alpha and ionizing radiative transfer in simulations of high-z - - PowerPoint PPT Presentation
lyman alpha and ionizing radiative transfer in simulations of high-z - - PowerPoint PPT Presentation
lyman alpha and ionizing radiative transfer in simulations of high-z galaxies daniel kasen (UCB/LBNL) daniel ceverino, avishai dekel, michele fumagalli, joel primack, x prochaska lyman alpha and ionizing radiative transfer in simulations of
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lyman alpha and ionizing radiative transfer in simulations of high-z galaxies
z = 2.3 Mv = 3.5 x 1011 Msun Rv = 72 kpc model MW3 ceverino et al. (2010)
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Lyman alpha blobs
LAB 2 (z = 3.09) wilman et al., 2005
75 kpc L = 1044 ergs s-1
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steidel et al., 2011 (<z> = 2.65 stacks)
c
- n
t i n u u m
lyman alpha
typical sensitivity
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- rigin of the lyman alpha blobs
- cooling emission from infall
e.g., haiman+ 2000, fadal+ 2001, dijkstra&loeb 2009, goerdt+ 2010, faucher-giguere+ 2010
- photoionization by stars
but c.f. matsuda+ 2004, nilsson+ 2006
- photoionization by AGN
e.g., geach+ 2009
- scattering in circumgalactic gas/outflows
e,g., zheng+ 2010, steidel+ 2011
what does theory predict when line scattering, photoionization and dust are taken into account?
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gas column
temperature stellar luminosity
gas density
dust optical depth
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transport of ionizing and L radiation
multi-wavelength monte carlo transport
no on the spot approximation
arbitrary distribution of ionizing sources
isotropic UVB plus ~5000 star particles
using an AMR grid
10 levels of refinement, x ~ 60 pc for 280 kpc box
dust absorption + scattering included
dust opacity constructed from metal distribution
transport done in post-processing
assumes ionization equilibrium, approximate heating
scattering/absorption on unresolved scales?
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- ptically thin approximation
e.g., goerdt et al. (2010) with line scattering and dust
l y m a n a l p h a e m i s s i
- n
( e r g s s-1 k p c-2 )
lyman alpha cooling emission
no stellar or AGN photoionization; L = 7 x 1042 ergs/s
L s u r f a c e b r i g h t n e s s ( e r g s s
- 1
c m
- 2
a r c s e c
- 2
)
fesc,l = 55%
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lyman alpha cooling emission
no stellar or AGN photoionization
velocity (km/s) normalized flux
lyman alpha
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- rientation dependence of L emission
MW3 z = 2.33 (cooling emission, no photoionization)
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- rientation dependence of L emission
MW3 z = 2.33 (cooling emission, no photoionization)
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Lyman alpha blobs
LAB 2 (z = 3.09) wilman et al., 2005
75 kpc L = 1044 ergs s-1
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neutral hydrogen column depth (cm
- 2
)
MW3
z = 2.33 fesc,uv = 6.8%
fesc,uv = 27% see fumagalli+2011
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lyman alpha emission (ergs s-1 kpc-2)
L s u r f a c e b r i g h t n e s s ( e r g s s
- 1
c m
- 2
a r c s e c
- 2
)
MW3
z = 2.33 SFR = 30 Msun/yr
fesc,L = 5%
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MW3
z = 2.33
LAGN = 1045 ergs/s lyman alpha emission (ergs s-1 kpc-2)
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emission (ergs s-1 kpc-2) surface brightness (ergs s-1 cm-2 arcsec-2)
H alpha from photoionization
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MW3
z = 2.3
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dependence on mass/redshift
z = 4.5 Rv = 39 kpc z = 3.5 Rv = 71 kpc z = 2.3 Rv = 114 kpc
gas column density
model SFG1
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dependence on mass/redshift
z = 4.5 Rv = 39 kpc z = 3.5 Rv = 71 kpc z = 2.3 Rv = 114 kpc
lyman alpha emission
UVB + stars UVB + stars UVB + stars
model SFG1
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