GRB多波長放射で切り開く暗黒の宇宙 SKA GRBs for UNravelling the Dark Ages Mission 井上進（京大理） ALMA 分子 ダスト SPICA TMT 再電離 （磁場） 金属 CTA ASTRO-H high-z GRB afterglows: expectations z measurement from Ly break: JANUS z~<13 GUNDAM z~<? Subaru z~<20 TMT z~<40 天文月報 102, 248 (2009) first star epoch z~100-10 未知との遭遇 Pop 3 =metal/dust-free, H2+HD-cooling assume: no metal/dust, B field, CR, turbulence, DM heating 1st HII region -> IGM reionization 1st SN -> 1st metal/dust (+CR+B) 1st BH -> 1st QSO Pop 2 =metal/dust-cooling 1st sun -> 1st planet, life, human! 観測ほとんど皆無 (WMAPのみ) 1st gen.はわかったとされている 2nd gen.研究に移行 Yoshida, Omukai & Hernquist 08 cosmic star formation rate deduced from GRB rate from GRB rate Kistler+ 09 from HUDF JANUS/GUNDAMでよりhigh-zへ 直接観測と相補的 cosmic reionization epoch z>7 現在のフロンティア When? early? late? two-epoch? How? topology? What? Pop III? Pop II? mini-QSOs? dark matter decay? So what? suppression of dwarf galaxy formation Madau 07 reionization: IGM HI (+ HII) from Lyprofile z=6.295 McQuinn+ 08 Ly damping wing profile 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） UV background from gamma-ray absorption g + g → e+ + eE e e.g. TeV + 1eV (IR) 100 GeV + 10 eV (UV) high-z UV背景放射：ガンマ線吸収で識別 SI+ 10 MN 404, 1938 CTA（Fermiの後継）でz~20 GRBまで観測可能 Y. Inoue, SI+, in prep. gamma-ray opacity cosmic star formation rate high-z UV background below Ly edge e<13.6 eV - does not ionize HI, weakly absorbed - reasonably uniform - important for gg absorption - direct measure of UV emissivity (indep. of escape fraction, IGM clumping factor) above Ly edge e>13.6 eV - ionizes HI, strongly absorbed - highly non-uniform - negligible for gg absorption metal abundances GRB 050904 z=6.295 Kawai+ 06, Totani+ 06 母銀河の金属組成、運動学 よりhigh-zへ kinematics D’Elia+ 09 GRB 080319B z=0.937 - multiple velocity components - variable line ratio (UV pumping) VLT/UVES res. ~4 km/s @4500A - 1.9km/s @9000A metal abundances GRB 090926A z=2.1071 ground D’Elia+ arXiv:1007.5357 VLT/X-shooter 0.3-2.5um R=10000 FeII fine struc. X/H~3x10-3-10-2 SiII X-ray absorption lines/edges Campana+ 06 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 <-> 光赤外と相補的 EDGE/XENIA E~0.2-2 keV E~3 eV Seff~1000 cm2 z=1 GRB Piro+ 07 -> more from D. Hartmann z=7 GRB E=0.3-10 keV E=7 eV Seff=210 cm2 simulations by Bamba (see also Kawai, Yonetoku+, Kyoto conf.) ASTRO-H log NH=22 (Zsolar) Si log NH=23 Si S Fe z=1 bright aft@t=10ks 5e-10 erg/cm2/s integ. 10ks スザクとは違うのだよ、スザクとは！ ASTRO-H E=0.3-10 keV E=7 eV Seff=210 cm2 see also Kawai, Yonetoku+, Kyoto conf. log NH=22 (Zsolar) z=6 bright aft@t=10ks 4e-11 erg/cm2/s integ. 10ks Fe log NH=23 z measurement for dark bursts <- JANUS alert E~0.2-2 keV E~3 eV Seff~1000 cm2 XENIA z=1 early aft@t=1ks 1e-9 erg/cm2/s integ. 1ks Ne Fe Mg Si log NH=22 (Zsolar) S O log NH=23 O E~0.2-2 keV E~3 eV Seff~1000 cm2 XENIA log NH=22 (Zsolar) Si z=6 early aft@t=1ks 5e-10 erg/cm2/s integ. 1ks log NH=23 Fe metal abundances at low metallicity nucleosynthesis by low metal. SN/HN Kobayashi+ 06 CNO: mass loss -elements: pair-instability SN Ti, Zn: entropy in SN core -> explosion physics Mn: SN Ia contribution molecules electronic absorption bands GRB 080607 z=3.063 Prochaska+ 09 Keck/LRIS R=1000-4000 log NHI=22.70 log NH2=21.2 log NCO=16.5 分子＝星形成の原材料 よりhigh-zへ？ collapse of zero/low-metallicity star forming clouds collapsing zero/low-metal. protostellar clouds T minimum -> fragmentation H2 Omukai+ 05 model dust H2+HD [Z/H]<-6: Mfrag~103MQ Pop 3 -3<[Z/H]<-5: Mfrag~0.1-100MQ Pop 2 [Z/H]crit=-5+-1 HD molecules Q 1232+082 z=2.3377 Ivanchik+ arXiv:1002.2107 VLT/UVES R=45000 N(HD)/N(H2) =7.1(+3.2 -2.2)x10-5 primordial molecules electronic absorption bands cold H2: 912-1110A (11.2-13.6 eV) vib. excited H2: 1110-1650 A (7.5-11.2 eV) c.f. ambient H2 excited by GRB UV Draine 00, Draine & Hao 02 similar for HD? N~1018-1020 cm-2 foreground massive star UV pumped H2 excited H2 massive star GRB rdiss probe individual Pop III newly-born massive stars? atomic/molecular absorption lines SI, Omukai & Ciardi 2007 MNRAS 380, 1715 • CO (low) SKA probe physical conditions (different J) • HD • CO (high) • [OI] ALMA probe Pop III Pop III->II transition 回転順位線 より高柱密度領域 TMTと相補的 チャレンジングだろうが やってみよう dust GRB 071025 z~5 Perley+ 10 - 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 (optical depth at fragmentation) pair instability SN based on first dust models of Schneider+ 06 TMT (+SPICA)で Pop 3 -> Pop 2 遷移を探れる？ ダストの性質も？ zero-metal SN II intergalactic/interstellar magnetic fields at high-z B fields in Pop III star forming regions B~10-16-10-14 G on pc scales IGM B generation at high-z cosmic reionization fronts B~10-20-10-16 G B profile nHI B ngas T Xu+ 08 mean B vs z Gnedin+ 00 also Langer+ 05 “pair echos” (delayed secondary emission) probe of intergalactic magnetic fields Plaga 95 (original idea) sensitive to very weak intergalactic magnetic fields GRB MeV g ~TeV B~10-20-10-16 G e- IR e+ CMB B g ~GeV CMB g delay MeV evolving echo flux CTA sens. fix Eiso=1054 erg, z=10, Emax=10 TeV B=10-15G assume low EBL (0.1x CF model) observationally challenging, but marginally detectable by CTA Takahashi, SI, Ichiki & Nakamura arXiv:1007.5363 Pop 3 HII regions - large r~<100 pc - low density n~0.1 cm-3 - flat profile Can be probed through afterglow evolution? Whalen+ 04 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… 課題：Pop III GRB？ その兆候は？ 多波長のシナジー： SKA, ALMA, SPICA, ASTRO-H, CTA… JANUS and/or GUNDAMを上げよう
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