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

まとめGRBは宇宙で最も明るい多色光源　有効利用しよう

特に z>10 first star epochは未開拓　 GRBで切り拓く

調べられる／られそうなこと：z 測定、星形成史、再電離史、金属組成、運動学、分子、ダスト、磁場…

多波長のシナジー：SKA, ALMA, SPICA, ASTRO-H, CTA…

JANUS and/or GUNDAMを上げよう

課題： Pop III GRB？　その兆候は？