1 / 24

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

remedy
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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）

More Related