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)
Thank you (おおきに)