Effects of early reionization on the formation of galaxies Hajime Susa Rikkyo University.
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Transcript of Effects of early reionization on the formation of galaxies Hajime Susa Rikkyo University.
![Page 1: Effects of early reionization on the formation of galaxies Hajime Susa Rikkyo University.](https://reader036.fdocuments.net/reader036/viewer/2022062412/5a4d1af47f8b9ab0599809fe/html5/thumbnails/1.jpg)
Effects of early reionization on the formation of galaxies
Hajime SusaRikkyo University
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Impacts of UVB on GFPHOTO IONIZATION
Production of electrons : catalysts of H2 formation → enhance the fraction of H2
Momentum Transfer
PHOTO DISSOCOATIONDissociation of H2 → No coolant
PHOTO HEATINGKeep the gas temperature 104-105 KPhoto-evaporationSuppression of SF in gals.
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Substructure in Galactic Halo
Moore et al. 1999Cluster Halo
Galactic Halo
M 145 10 8
M 122 10 820 times smaller than expected
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Late Reionization, CDM density perturbation, and Radiative cooling.....
Blown away by photo-evaporation
7 20
If Z_reion=7, 1σ density perturbations are not prevented from forming stars.
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Early reionization (WMAP)
( ) 0.17 0.04recz
Spergel et al. 2003
Instantaneous reionization:
17 3reionz
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Early Reionization, CDM density perturbation, and Radiative cooling.....
Shaded Blown away ≒by photo-evaporation
7 20
If Z_reion=20, >2σ density perturbations are prevented from forming stars.
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Smaller scale sub-clumps
xIn hierarchical clustering scenario, small clumps evolve faster thanthe parent system.
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Method (RSPH)SPH
Steinmetz & Muller 1993Umemura 1993
GravityHMCS in University of Tsukuba (CCP)GRAPE6, direct-sum
Radiation transfer of ionizing photonsKessel-Dynet & Burkurt 2000 Nakamoto, Umemura & Susa 2001
Primordial chemistry & CoolingSusa & Kitayama 2000Galli & Palla 1998
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Model of SF
2
4
1 5000 K
3 20
2. 5 10
0
4 0
1ga
f
H
s
f
y
T
cd cdt t
***
.
.
.
,
v
In order to evaluate the case of maximal star formation rate, we assume
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Model of UVB
3
21 1 / 3 I z
1
21 exp 12 3 I z
1 z
21I
3 5Put a source outside the simulation box so that the mean intensity is equal to above value at the center.
21 0.01 I
21 exp 3(17 ) I z
Early Reionization model
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0t 86.5 10 yeart 91.1 10 yeart
91.5 10 yeart 93.5 10 yeart 93.7 10 yeart
93.9 10 yeart 94.9 10 yeart 97.0 10 yeart
2410
2910
2610
2510
2710
2810
-3[g cm ]
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Maximally Star-forming model (c*=1)
100ML
“ Evaporated ”
810 or20km/srot
M Mv
¤d d
>95% halos are photo-evaporated.
3
456
106
2
3
456
107
2
3
456
108
2
3
6 7 8 910
2
Vc=20 km/s
Vc=10 km/ s
Vc=5 km/ s
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Convergence of c*=1 model
172N 152N
132N
142N
172N 152N
132N
142N
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Summary 1Formation of low mass galaxies are investigated by 3D RHD simulations with early reionization model.CDM substructure problem is resolved solely by the early reionization model at dSph scale (<10^8 Msun or Vrot < 20 km/s).
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Detection of Reneutralization ?
Susa Rikkyo University
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GP trough of High-z QSOs
Fan et al. 2002
221 120.67 0.013 10HII y
d t
@ z=6Z=5.80
Z=5.82
Z=5.99
Z=6.28
Becker et al., 2001
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Top Heavy IMF ?
Sokasian et al 2003
Volume fractionof HII region
τe
POPII 、Salpeter IMF
+First StarsTOP Heavy
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Cen(2003)
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High-z Lyα emitter
low-z
high-z
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High-z Lyαemitter 2
Haiman 2002Broad line emission + high SFR ⇒ large self HII region ⇒Still detectable even at neutral universe.
How they look like in double reionization universe ?
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A double reionization history
Z<6 yh1=0.00016<z<9 yh1=0.39<z<19 yh1=0.0001Z>19 yh1=1
Cen like
Effects of self-HII region is also taken into account.
Haiman like
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Emission profile Δv=10km/s, SFR=1Msun/yr
1.0
0.8
0.6
0.4
0.2
0.0100500-50
x10- 6
1.0
0.8
0.6
0.4
0.2
0.0100500-50
x10- 6 1.0
0.8
0.6
0.4
0.2
0.0100500-50
x10- 6
1.0
0.8
0.6
0.4
0.2
0.0100500-50
x10-6
Z=4
Z=23
Z=15
Z=9
revival
ionized
neutral
ionized
neutral
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Flux of Lyα 、 Hα
Detectable by next generation facilities ………….
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Summary 2
It is possible to use F(Lyα)/F(Hα) ratio to probe the reionization history at z > 7.If double reionization history is assumed, the ratio has characteristic behavior.