1. Starburst-AGN Connection: A Lesson from High-z Powerful Radio Galaxies Yoshi Taniguchi POSSIBLE Never take any JANKY FOODS @ Kyoto, please !

2. High-z Powerful Radio Galaxies (HzPRGs) Quasars and HzPRGs are sign posts at high redshift Rest-frame UV/opt: Quasars: dominated by nonthermal continuum HzPRGs: dominated by stellar light Hosts of HzPRGs provide us a nice tool to study formation & evolution of galaxies @ high z (see for a review, McCarthy 93, ARA&A, 31, 639) ３ CR, PKS, Bologna, Molonglo, LBDS, …  N > 10000

3. The Most Distant Known HzPRG TN J0924-2201 @ z = 5.19 (van Breugel et al. 1999, ApJ, 518, L61) High-z: mostly z ~ 2 - 4

4. Obs. Properties of HzPRG Hosts Passive Evolution ? Rest-frame opt/NIR SED Evolution from z = 4 to 0.1 (Yoshii, Renzini, Arimoto, & YT) L(850μm) Evolution from z = 4 to 0.5 (Archibald+01, MN, 323, 417) HzPRG hosts  Passive Evolution  (giant) Ellipticals

5. [1] Gas-rich: M cold gas ~ 10 10 M sun [2] Strong thermal FIR/submm: L FIR ~ 10 12 L sun ~ L FIR (ULIRG) SFR ~ 100 M sun /yr (e.g., Archbald+01, MN, 323, 417; De Breuck+00, AA, 362, 519) Obs. Properties of HzPRG Hosts High-z analogs of ULIRGs? HzPRG hosts, too ??? Some HzPRGs are HyLIRGs ! Giant E formation is in progress in ULIRGs; “dissipative collapse” (Kormendy & Sanders 92, ApJ, 390, L53) M halo > 10 11 M sun High-z analog of local ULIRGs ?

6. Obs. Properties of HzPRG Hosts Superwind ? “8” shape (Ruch+97, ApJ, 484, 163) (Taniguchi+01, ApJ, 559, L9) Bi-polar shape (Motohara+00, PASJ, 52, 33) MRC 0406-244 @ z = 2.43 B3 0731+438 @ z = 2.43 Extended ionized gas: AGN photoionization + shock heating (e.g., De Breuck+00, AA, 362, 519)

7. A summary of Hosts properties [1] Passive evolution: From HzPRGs to giant Es in the local universe. [2] Gas-rich nature with very high SFR @ z ~ 3: High-z analog of local ULIRGs ? [3] Superwind: Also, consistent with the prediction of monolithic collapse models for elliptical galaxies. All these suggest that some HzPRGs experienced “semi-monolithic” collapse although mass assembly could be made hierarchically ! OK, go ahead, anyway …

8. Hosts of HzPRGs Magorrian Relation >>> HzPRGs are a progenitor of (giant) Es. Es follow the Magorrian relation. (M ● /M ○ ~0.001) It is interesting to study ・ star formation history ・ SMBH formation history in the hosts of HzPRGs !  When was Magorrian relation established ?  How was Magorrian relation established ?

9. When did major SF occur in HzPRG hosts ? z ~ 3 ? z ~ 5 ? z ~ 25 ? z ~ 10 ? ?????????????????? ！！！！！！

10. Subaru Deep Field (SDF) Two Lyα emitters beyond z = 6 z = 6.54 z = 6.58 Most distant ? (Kodaira+03, PASJ, 55, L17 )

11. z=6.50 z=6.55 z=6.54 z=6.58 z=6.60

12. Most Distant Galaxies （ 2003 October 30 ） No. Name z Tel. Ref. 1 SDF132522 6.60 Subaru SDF 2 SDF132432 6.58 Subaru SDF 3 SDF132528 6.58 Subaru SDF 4 SDF132418 6.58 Subaru Kodaira+03 5 HCM-6A 6.56 Keck/Subaru Hu+02 6 SDF132408 6.55 Subaru SDF 7 SDF132415 6.54 Subaru Kodaira+03 8 SDF132353 6.54 Subaru SDF 9 SDF132552 6.54 Subaru SDF 10 SDF132418 6.50 Subaru SDF 11 SDF132440 6.33 Subaru SDF 12 0226-04LAE 6.17 CFHT/VLT Cuby+03 But, tomorrow is another day … I don’t care.

13. Important Redshifts (convention in my talk) z ~ 3 (2 - 4 ) z ~ 25 (20 – 30) z ~ 8 (5 -10) 2.3 Gyr 0.90 Gyr 0.35 Gyr 0.6 Gyr 1.4 Gyr Cosmic Age Interval (ΔT) Ω m =0.3, Ω λ =0.7, & h = 0.7

14. Major epoch of SF in HzPRG hosts ? z (SF) ~ 8 [1] N overabundance in high-z quasars N V /HeII & NV/C IV (Hamann & Ferland, 93, ApJ, 418, 1) [2] Fe overabundance in high-z quasars FeII/MgII (Kawara+96, ApJ, 470, L85) (Yoshii+98, ApJ, 507, L113) (Dietrich+03, ApJ, 569, 817) [3] N overabundance in HzPRGs (Vernet+01, AA, 366, 7) Chemical evolution models suggest …. BLR Extended

15. Major Epoch of SF in HzPRG hosts ? z (SF) ~ 8 Superwind could develop ~ 1 Gyr after the onset of initial starburst. (e.g., Arimoto & Yoshii 87, AA, 173, 23) Note that early star formation timescale of Es ~ 1 Gyr. (Bower+92, MN 254, 589 & 681) SW @ z ~ 3 suggests ….

16. What Happened in Pop. II Era ? Back to ULIRGs (e.g., Arp 220) Origin of local ULIRGs: Merger between/among gas-rich, nucleated galaxies RHα

17. Merger-Driven Nuclear Starburst Supermassive BH binary [1] induces efficient fueling, [2] triggers intense nuclear (circumnuclear) starbursts for a long duration(~ 10 8 yrs) [strong spiral shocks] (Taniguchi & Wada96, ApJ, 469, 581) Different SF mode from normal SF in GMCs. Major merger between/among nucleated, massive systems could occur @ high z (z ~ 8) ?

18. What Happened in Pop. III Era ? What we need [1]: Major merger between/among nucleated systems could occur @ z ~ 8 What we need [2]: Nucleus (seed SMBH) with M ● ~ 10 7 M sun in each system @ z ~ 8 Question: How can we make such seed SMBHs @ z ~ 8

19. What Happened in Pop. III Era? Ostriker & Gnedin 96, ApJ, 472, L63 Pop. III subgalactic Pop. II (sub)galactic The Pop III World Very massive stars formed in mini halos @ z ~ 25 [1] Very massive stars M ★ > 260 M sun  M IMBH ~ 100 M sun [2] Mini halos ・ 3.5σpeak (rare) : M halo ~ 10 6 M sun ・ 3σpeak (popular): M halo ~ 10 5 M sun (e.g., Madau+03, astro-ph/0310223) 25 10 10 11 10 5 Sorry

20. What Happened in Pop. III Era? Pop III-origin IMBH M ● ~ 100 M sun ＠ z ~ 25 How could an IMBH grow up ? From M ● ~ 100 M sun ＠ z ~ 25  10 7 M sun @ z ~ 8 If Pop III formation efficiency is low, [1] Pop III-star clusters might be rare in each halo.  dynamical friction could not work. [2] Runaway merger-driven grow up could not work.  Grow up by gas accretion is much more likely.

21. Gas-accretion grow up of IMBH to seed SMBH in Pop. III Era? Gas accretion (Eddington) timescale ・ T Edd ~ 4 ×10 7 (η/0.1)(L Edd /L) yr ・ ΔT(z: 25  8) ~ 6 ×10 8 yr ~ 15 T Edd  M ● (T=15T Edd ) ~ 10 5 ×M ● (initial) IMBH could grow up to seed SMBH ! M ● ~ 100 M sun ＠ z ~ 25  10 7 M sun @ z ~8 [Mergers among mini halos are necessary]

22. What Happened in Pop. II Era?: Revisited Major-merger like, semi-monolithic collapse between/among nucleated galactic systems with M halo > 10 11 M sun could occur @ z ~ 8 [“nucleated”: M ● ~ 10 7 M sun ] Dynamical disturbance by “double (or multiple)” nuclei leads to formation of many super-star clusters in the merger center.  Dynamical friction (Ebisuzaki+01)  formation of a SMBH with M ~ 10 9 M sun because T fric ~ 1 Gyr < ΔT(z: 8  3) ~ 1.4 Gyr M ● /M ○ ~ 0.003 (Bekki & Couch 01, ApJ, 557, L19)

23. Kyoto Model for the formation of SMBH in the heart of HzPRGs @ z ~ 3 Pop III-driven IMBH M ● ~ 100 M sun @ z ~ 25 ● ● ● ● ● ● ● ● ● Gas accretion-driven SMBH M ● ~ 10 7 M sun @ z ~8 Major merger-driven SMBH M ● ~ 10 9 M sun @ z ~3 τ(acc) ~ 0.6 Gyr τ(fric) ~ 1 Gyr ΔT ~ 0.6 Gyr (z: 25  8 ) ΔT ~ 1.4 Gyr (z: 8  3 )

24. z ~ 8 z ~ 25 Pre-Maggorian Phase Not related to ○ formation Maggorian Phase ○ formation began Kyoto ( 京都） Tokyo ( 東京） Thank you （おおきに）