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.
Effects of early reionization on the formation of galaxies
Hajime SusaRikkyo University
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.
Substructure in Galactic Halo
Moore et al. 1999Cluster Halo
Galactic Halo
M 145 10 8
M 122 10 820 times smaller than expected
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.
Early reionization (WMAP)
( ) 0.17 0.04recz
Spergel et al. 2003
Instantaneous reionization:
17 3reionz
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.
Smaller scale sub-clumps
xIn hierarchical clustering scenario, small clumps evolve faster thanthe parent system.
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
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
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
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 ]
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
Convergence of c*=1 model
172N 152N
132N
142N
172N 152N
132N
142N
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).
Detection of Reneutralization ?
Susa Rikkyo University
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
Top Heavy IMF ?
Sokasian et al 2003
Volume fractionof HII region
τe
POPII 、Salpeter IMF
+First StarsTOP Heavy
Cen(2003)
High-z Lyα emitter
low-z
high-z
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 ?
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
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
Flux of Lyα 、 Hα
Detectable by next generation facilities ………….
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.