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GRB多波長放射で切り開く暗黒の宇宙
SKA
CTA
井上進(京大理)
ALMA
SPICA ASTRO-H
TMT
GRBs for UNravelling the Dark Ages Mission
再電離(磁場)
金属ダスト
分子
high-z GRB afterglows: expectations
天文月報102, 248 (2009)
z measurementfrom Ly break:
Subaru z~<20TMT z~<40
JANUS z~<13GUNDAM z~<?
first star epoch
観測ほとんど皆無 (WMAPのみ )
Yoshida, Omukai & Hernquist 081st gen.はわかったとされている2nd gen.研究に移行
Pop 3 =metal/dust-free, H2+HD-coolingassume: no metal/dust, B field, CR, turbulence, DM heating
1st HII region -> IGM reionization1st SN -> 1st metal/dust (+CR+B)
Pop 2 =metal/dust-cooling1st sun -> 1st planet, life, human!
1st BH -> 1st QSO
z~100-10 未知との遭遇
cosmic star formation rate deduced from GRB rate
Kistler+ 09
from GRB rate
from HUDF
JANUS/GUNDAMでより high-zへ直接観測と相補的
cosmic reionization epoch
early? late? two-epoch?When?
mini-QSOs?What?
So what?suppression ofdwarf galaxyformation
How? topology?
Pop III? Pop II?
Madau 07
dark matter decay?
z>7 現在のフロンティア
reionization: IGM HI (+ HII) from Lyprofile
McQuinn+ 08
mean IGM HI + host galaxy HI + host HII
宇宙再電離すばる、 TMTで各成分を分離より high-zへ(WMAP, Planckと重なる時期)
z=6.295
Ly damping wing profile
UV background from gamma-ray absorption
+ → e+ + e-
E e.g. TeV + 1eV (IR) 100 GeV + 10 eV (UV)
cosmic star formation rategamma-ray opacity
high-z UV背景放射:ガンマ線吸収で識別CTA( Fermiの後継)で z~20 GRBまで観測可能
SI+ 10 MN 404, 1938Y. Inoue, SI+, in prep.
high-z UV backgroundbelow Ly edge above Ly edge
- does not ionize HI, weakly absorbed- reasonably uniform- important for absorption
- ionizes HI, strongly absorbed- highly non-uniform- negligible for absorption
<13.6 eV >13.6 eV
- direct measure of UV emissivity (indep. of escape fraction, IGM clumping factor)
metal abundancesGRB 050904 z=6.295Kawai+ 06, Totani+ 06
kinematics D’Elia+ 09
- multiple velocity components- variable line ratio (UV pumping)VLT/UVES res. ~4 km/s @4500A - 1.9km/s @9000A
GRB 080319B z=0.937
母銀河の金属組成、運動学より high-zへ
metal abundancesD’Elia+ arXiv:1007.5357
VLT/X-shooter 0.3-2.5um R=10000
GRB 090926A z=2.1071
X/H~3x10-3-10-2
FeII
SiII
ground
fine struc.
X-ray absorption lines/edges
EDGE/XENIA
Campana+ 06
E~0.2-2 keV E~3 eV Seff~1000 cm2
z=1 GRB
z=7 GRB
<-> 光赤外と相補的
Piro+ 07
-> more from D. Hartmann
星生成領域スケールの組成遠方まで観測可能?ダストの影響なしが H, Heの情報なし
ASTRO-H E=0.3-10 keV E=7 eV Seff=210 cm2
simulations by Bamba (see also Kawai, Yonetoku+, Kyoto conf.)
スザクとは違うのだよ、スザクとは!
log NH=22 (Zsolar)
log NH=23Fe
Si
z=1bright aft@t=10ks5e-10 erg/cm2/sinteg. 10ks
S
Si
ASTRO-H E=0.3-10 keV E=7 eV Seff=210 cm2
see also Kawai, Yonetoku+, Kyoto conf.
log NH=22 (Zsolar)
log NH=23
Fe
z=6bright aft@t=10ks4e-11 erg/cm2/sinteg. 10ks
z measurementfor dark bursts<- JANUS alert
XENIA
log NH=22 (Zsolar)
log NH=23
Siz=1early aft@t=1ks1e-9 erg/cm2/sinteg. 1ks
E~0.2-2 keV E~3 eV Seff~1000 cm2
S
O
Ne
Mg
O
Fe
XENIA
log NH=22 (Zsolar)
log NH=23
z=6early aft@t=1ks5e-10 erg/cm2/sinteg. 1ks
E~0.2-2 keV E~3 eV Seff~1000 cm2
Fe
Si
metal abundances at low metallicityKobayashi+ 06nucleosynthesis by low metal. SN/HN
CNO: mass loss-elements: pair-instability SNTi, Zn: entropy in SN core -> explosion physicsMn: SN Ia contribution…
moleculesGRB 080607 z=3.063 Prochaska+ 09
log NHI=22.70log NH2=21.2log NCO=16.5
分子=星形成の原材料より high-zへ?
electronic absorption bands
Keck/LRIS R=1000-4000
collapse of zero/low-metallicity star forming clouds Omukai+ 05 model
[Z/H]<-6: Mfrag~103M Pop 3-3<[Z/H]<-5: Mfrag~0.1-100M Pop 2 [Z/H]crit=-5+-1
H2
H2+HD
dust
T minimum -> fragmentationcollapsing zero/low-metal. protostellar clouds
HD molecules Ivanchik+ arXiv:1002.2107Q 1232+082 z=2.3377
N(HD)/N(H2)=7.1(+3.2 -2.2)x10-5
VLT/UVES R=45000
primordial molecules c.f. ambient H2 excited by GRB UVDraine 00, Draine & Hao 02
rdiss
GRB
excited H2
massivestar
foreground massive starUV pumped H2
probe individual Pop IIInewly-born massive stars?
N~1018-1020 cm-2
electronic absorption bandscold H2: 912-1110A (11.2-13.6 eV)vib. excited H2: 1110-1650 A (7.5-11.2 eV)
similar for HD?
atomic/molecular absorption lines
• HD• CO (high)• [OI]
probe Pop IIIPop III->II transition
probe physicalconditions (different J)
ALMA
SKA• CO (low)
SI, Omukai & Ciardi2007 MNRAS 380, 1715
チャレンジングだろうがやってみよう
回転順位線より高柱密度領域TMTと相補的
dust Perley+ 10GRB 071025 z~5
- extinction feature- best fit with high-z QSO extinc. curve (Maiolino+ 04)
ダスト:Pop II星形成への遷移に本質的?TMTでより high-zへPop III ダストの性質も?
absorption by first dust
based on first dust models of Schneider+ 06
(optical depth at fragmentation)
TMT (+SPICA)でPop 3 -> Pop 2 遷移を探れる?ダストの性質も?
pair instabilitySN zero-metal SN II
intergalactic/interstellar magnetic fields at high-z
Gnedin+ 00
BnHI
ngas T
IGM B generation at high-zcosmic reionization frontsB~10-20-10-16 G
also Langer+ 05
B fields in Pop III star forming regionsB~10-16-10-14 G on pc scales
B profile
mean B vs z
Xu+ 08
“pair echos” (delayed secondary emission) probe of intergalactic magnetic fields
Plaga 95 (original idea)
GRB
IR
~TeV
e+
e-
B
CMB
~GeV
sensitive to very weakintergalactic magnetic fields
CMB
MeV
MeV
delay
B~10-20-10-16 G
evolving echo flux
fix Eiso=1054 erg, z=10, Emax=10 TeV
observationally challenging, but marginally detectable by CTA
CTA sens. B=10-15G
assume low EBL(0.1x CF model)
Takahashi, SI, Ichiki & Nakamura arXiv:1007.5363
Pop 3 HII regions
Whalen+ 04
- large r~<100 pc- low density n~0.1 cm-3
Can be probed throughafterglow evolution?
- flat profile
also Kitayama+ 04
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