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Starburst-AGN Connection: A Lesson from High- z Powerful Radio Galaxies Yoshi Taniguchi

POSSIBLE. Starburst-AGN Connection: A Lesson from High- z Powerful Radio Galaxies Yoshi Taniguchi. Never take any JANKY FOODS @ Kyoto, please !. High- z Powerful Radio Galaxies (HzPRGs). 3 CR, PKS, Bologna, Molonglo, LBDS, …  N > 10000. Quasars and HzPRGs are sign posts at high redshift

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Starburst-AGN Connection: A Lesson from High- z Powerful Radio Galaxies Yoshi Taniguchi

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

  2. High-z PowerfulRadio Galaxies (HzPRGs) 3CR, PKS, Bologna, Molonglo, LBDS, …  N > 10000 Quasars and HzPRGs are sign posts at high redshift Rest-frame UV/opt: Quasars: dominated by nonthermal continuum HzPRGs: dominated by stellar light Hostsof 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. The Most Distant Known HzPRGTN J0924-2201 @ z = 5.19(van Breugel et al. 1999, ApJ, 518, L61) High-z: mostly z ~ 2 - 4

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

  5. Obs. Properties of HzPRG Hosts High-z analogs of ULIRGs? [1] Gas-rich: Mcold gas ~ 1010Msun [2] Strong thermal FIR/submm: LFIR ~ 1012Lsun ~ LFIR(ULIRG) SFR ~ 100 Msun /yr (e.g., Archbald+01, MN, 323, 417;De Breuck+00, AA,362, 519) Mhalo > 1011Msun Some HzPRGs are HyLIRGs ! High-z analog of local ULIRGs ? Giant E formation is in progress in ULIRGs; “dissipative collapse” (Kormendy & Sanders 92, ApJ, 390, L53) HzPRG hosts, too ???

  6. Obs. Properties of HzPRG HostsSuperwind ? MRC 0406-244 @ z = 2.43 B3 0731+438 @ z = 2.43 “8” shape (Ruch+97, ApJ, 484, 163) (Taniguchi+01, ApJ, 559, L9) Bi-polar shape (Motohara+00, PASJ, 52, 33) 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 HzPRGsMagorrian Relation <<< If >>>> 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 ~ 10 ? z ~ 25 ?

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

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

  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) 2.3 Gyr 1.4 Gyr z ~ 8 (5 -10) 0.90 Gyr 0.6 Gyr z ~ 25 (20 – 30) 0.35 Gyr Ωm=0.3, Ωλ=0.7, & h = 0.7 Cosmic Age Interval (ΔT)

  14. Major epoch of SF in HzPRG hosts ? [1] N overabundance in high-zquasars NV/HeII & NV/CIV (Hamann & Ferland, 93, ApJ, 418, 1) [2] Fe overabundance in high-zquasars 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) BLR Extended z (SF) ~ 8 Chemical evolution models suggest ….

  15. Major Epoch of SF in HzPRG hosts ? 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 …. z (SF) ~ 8

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

  17. Merger-DrivenNuclear Starburst Supermassive BH binary [1] induces efficient fueling, [2] triggers intense nuclear (circumnuclear) starbursts for a long duration(~ 108yrs) [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● ~ 107Msun in each system @ z ~ 8 Question: How can we make such seed SMBHs @ z ~ 8

  19. What Happened in Pop. III Era? Sorry The Pop III World Very massive stars formed in mini halos @ z ~ 25 [1] Very massive stars M★ > 260Msun MIMBH ~ 100 Msun [2] Mini halos ・3.5σpeak (rare) : Mhalo ~ 106Msun ・3σpeak (popular):Mhalo ~ 105Msun (e.g., Madau+03, astro-ph/0310223) 1011 105 Pop. III subgalactic Pop. II (sub)galactic 25 10 Ostriker & Gnedin 96, ApJ, 472, L63

  20. What Happened in Pop. III Era? Pop III-origin IMBH M● ~ 100 Msun @ z ~ 25 How could an IMBH grow up ? FromM● ~ 100 Msun@ z ~ 25107Msun @ 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 ofIMBH to seed SMBHin Pop. III Era? Gas accretion (Eddington) timescale   ・ TEdd ~ 4 ×107 (η/0.1)(LEdd/L) yr   ・ΔT(z: 25  8) ~ 6 ×108 yr ~ 15 TEdd  M●(T=15TEdd)~ 105×M● (initial) IMBH could grow up to seed SMBH ! M● ~ 100 Msun@ z ~ 25 107Msun @ 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 Mhalo > 1011Msun could occur @ z ~ 8 [“nucleated”: M● ~ 107Msun] • 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 ~ 109 Msun because Tfric ~ 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 SMBHin the heart of HzPRGs @ z ~ 3 ● ● Pop III-driven IMBH M● ~ 100 Msun @ z ~ 25 ● ● ● ● τ(acc) ~ 0.6 Gyr ΔT ~ 0.6 Gyr (z: 25  8) ● ● Gas accretion-driven SMBH M● ~ 107 Msun @ z ~8 τ(fric) ~ 1 Gyr ΔT ~ 1.4 Gyr (z: 8  3) Major merger-driven SMBH M● ~ 109Msun @ z ~3 ●

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

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