Starburst-AGN Connection:Starburst-AGN Connection:A Lesson from High-A Lesson from High-zz

Powerful Radio GalaxiesPowerful Radio GalaxiesYoshi TaniguchiYoshi Taniguchi

POSSIBLENever take any JANKY FOODS @ Kyoto, please !

High-High-zz Powerful PowerfulRadio Galaxies (HzPRGs)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

The Most Distant Known HzPRGTN J0924-2201 @ z = 5.19

(van Breugel et al. 1999, ApJ, 518, L61)

High-z: mostly z ~ 2 - 4

Obs. Properties of HzPRG HostsObs. Properties of HzPRG HostsPassive Evolution ?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 hostsPassive Evolution (giant) Ellipticals

[1] Gas-rich:

Mcold gas ~ 1010 Msun

[2] Strong thermal FIR/submm:

LFIR ~ 1012 Lsun ~ LFIR(ULIRG)

SFR ~ 100 Msun /yr(e.g., Archbald+01, MN, 323, 417; De Breuck+00, AA, 362, 519)

Obs. Properties of HzPRG Hosts Obs. Properties of HzPRG Hosts High-z analogs of ULIRGs?High-z analogs of ULIRGs?

HzPRG hosts, too ???

Some HzPRGs areHyLIRGs !

Giant E formation is in progress in ULIRGs; “dissipative collapse” (Kormendy & Sanders 92, ApJ, 390, L53)

Mhalo > 1011 Msun

High-z analog of local ULIRGs ?

Obs. Properties of HzPRG HostsObs. Properties of HzPRG Hosts Superwind ?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)

A summary of Hosts propertiesA 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 assemblycould be made hierarchically ! OK, go ahead, anyway …

Hosts of HzPRGsHosts of HzPRGsMagorrian RelationMagorrian 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 historyin the hosts of HzPRGs !

When was Magorrian relation established ? How was Magorrian relation established ?

When did major SF occurWhen did major SF occur in HzPRG hosts ? in HzPRG hosts ?

z ~ 3 ?

z ~ 5 ?

z ~ 25 ?

z ~ 10 ?

?????????

！！！

Subaru Deep Field (SDF) Two Lyα emitters beyond z = 6

z = 6.54

z = 6.58

Most distant ?

(Kodaira+03, PASJ, 55, L17)

z=6.50

z=6.55

z=6.54 z=6.54

z=6.54 z=6.58

z=6.58 z=6.58z=6.60

Most Distant GalaxiesMost Distant Galaxies（（ 2003 October 302003 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 SDF10 SDF132418 6.50 Subaru SDF11 SDF132440 6.33 Subaru SDF12 0226-04LAE 6.17 CFHT/VLT Cuby+03

But, tomorrow is another day … I don’t care.

Important RedshiftsImportant Redshifts(convention in my talk)(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

CosmicAge

Interval(ΔT)

Ωm=0.3, Ωλ=0.7, & h = 0.7

Major epoch of SF Major epoch of SF in HzPRG hosts ? in HzPRG hosts ?

z (SF) ~ 8

[1] N overabundance in high-z quasars NV/HeII & NV/CIV (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 evolutionmodels suggest ….

BLR

Extended

Major Epoch of SFMajor Epoch of SF in HzPRG hosts ? 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 ….

What Happened in Pop. What Happened in Pop. IIII Era ? Era ?Back to Back to ULIRGs ULIRGs (e.g.,(e.g., Arp 220 Arp 220))

Origin of local ULIRGs:Merger between/among gas-rich, nucleated galaxies

R Hα

Merger-DrivenMerger-DrivenNuclear StarburstNuclear 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 modefrom normal SF in GMCs.

Major merger between/among nucleated, massive systems could occur @ high z (z ~ 8) ?

What Happened in Pop. What Happened in Pop. IIIIII Era ? Era ?

What we need [1]:Major merger between/among

nucleated systems could occur @ z ~ 8

What we need [2]:Nucleus (seed SMBH) with M● ~ 107 Msun

in each system @ z ~ 8

Question:How can we make such seed SMBHs

@ z ~ 8

What Happened What Happened in Pop. in Pop. IIIIII Era? Era?

Ostriker & Gnedin96, ApJ, 472, L63

Pop. IIIsubgalactic

Pop. II(sub)galactic

The Pop III WorldVery massive stars formed in mini halos @ z ~ 25

[1] Very massive stars M ★ > 260 Msun

MIMBH ~ 100 Msun

[2] Mini halos

・ 3.5σpeak (rare) : Mhalo ~ 106 Msun

・ 3σpeak (popular): Mhalo ~ 105 Msun

(e.g., Madau+03, astro-ph/0310223)

25 10

1011

105

Sorry

What Happened What Happened in Pop. in Pop. IIIIII Era? Era?

Pop III-origin IMBH

M● ~ 100 Msun ＠ z ~ 25

How could an IMBH grow up ? From M● ~ 100 Msun ＠ z ~ 25 　 107 Msun @ 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.

Gas-accretion grow up ofGas-accretion grow up of IMBHIMBH to to seed SMBHseed SMBH

in Pop. in Pop. IIIIII Era? 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 　 107 Msun @ z ~8 [Mergers among mini halos are necessary]

What Happened What Happened in Pop. in Pop. IIII Era?: Revisited Era?: Revisited

Major-merger like, semi-monolithic collapsebetween/among nucleated galactic systems

with Mhalo > 1011 Msun could occur @ z ~ 8

[“nucleated”: M● ~ 107 Msun ]

Dynamical disturbance by “double (or multiple)” nucleileads 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)

KyotoKyoto Model for the formation of SMBH Model for the formation of SMBHin the heart of HzPRGs @ in the heart of HzPRGs @ zz ~ 3 ~ 3

Pop III-driven IMBHM● ~ 100 Msun @ z ~ 25

●

●

●

●

●●

● ●

●

Gas accretion-driven SMBHM● ~ 107 Msun @ z ~8

Major merger-driven SMBHM● ~ 109 Msun @ 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 )

z ~ 8

z ~ 25

Pre-Maggorian PhaseNot related to ○ formation

Maggorian Phase○ formation began

Kyoto( 京都）

Tokyo( 東京）

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