StarFormation & AGN Activities in LIRGs@ z < 2 H. Hanami - - PowerPoint PPT Presentation

StarFormation & AGN Activities in LIRGs@z < 2

• H. Hanami & T. Ishigaki (Iwate Univ.),

+ AKARI ExtraGalactic Survey Team 2014/08/06@Charlottesville

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Why & How to study LIRGs up toz ∼ 2

• Why SF & AGN decline @z < 2

– LIRGs @z ∼ 1 − 2 near Main Seq. ∗ Consist of ⋆ + ISM(Dust) + AGN

• How: A Deep Survey with Subaru+AKARI

– Subaru/SC→ ⋆ & zphot – AKARI/IRC→ > 1, 000LIRGs up to z ∼ 2 →Distinction between SF/AGN-LIRGs →Co-Evolution of SF & AGN Hanami+, 2012, PASJ, 64, 4 Confirming with +Herschel/PACS &CXO in Ishigaki+2014 in prep.

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AKARI covers 2, 3, 4, 7,9, 11, 15, 18,24µm

3µm 4µm ← ⋆ ց 7µm րDust 5µm ;Window for AGN 9µm ← PAH8µm 11µm15µm 18µm 24µm @z < 2 →

• PAH@8µm → SFR @z < 2
• ⋆ ց before Dust ր @5µm→ Window for AGN

→ Distinction between SF/AGN-LIRGs

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z vs. νLν(8µm): νLν(8µm) ≃ 0.1LtIR ULIRGs LIRGs IRGs

MIR-all:SF MIR-all:s-BBG MIR-all:p(qp)-BBG

ULIRGs LIRGs IRGs 11 15

z≃1 1824 z≃2 MIR-B:SF

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z≃1 1824 z≃2 MIR-B:SF/AGN

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z≃1 1824 z≃2 MIR-B:AGN

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MIR Color-Color Diag.@z ≃0.6,1.0, > 1.2

z ≃ 0.6 [9] − [11] [11] − [15] z ≃ 1 [9] − [11] [11] − [15] z ≥ 1.2 [11] − [15] [15] − [18] AGN StarForming z ≃ 0.6 [9] − [11] [11] − [15] AGN StarForming z ≃ 1 [9] − [11] [11] − [15] AGN StarForming z ≥ 1.2 [11] − [15] [15] − [18] 7.7µm PAH @z ≃ 1(1.5) detected with L15(L18W)

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Rest Frame SEDs of AGN,SFw/AGN,SF

@z ≃0.6,1.0, > 1.2 magenta:BL AGN

Spectroscopic

AGN StarForming

SFw/AGN SF Dominated

Photometric

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zphot, M∗, SFRIR, f(AGN) for > 1000 LIRGs

Hanami+, 2012, PASJ, 64, 4

Fitting with BC03

↓

zphot, M∗, AV , SFRUV Star < 2µm Dust > 5µm

Fitting with Dusty SF (SK08) + Torus (QSO2) → νL8−1000µm ∼ L(IR; SF) ∼ SFRIR → νL8µm ∼ L(IR; AGN)

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M∗ − SFR @z ≃0.6,1.0, > 1.2

Thick;SFR(IR+obs.UV), Thin;SFR(Corr.UV)

SFR(IR + obs.UV ) ∝ SFR(Corr.UV ) SFRMS ≃ 25M⊙yr−1

(

M∗ 1011M⊙

)0.7 (1 + z)2

SFRIR > SFRMS@z > 0.4

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5µm between ⋆ and Dust→ Window for AGN AGN SF/AGN StarForming

@z ≃0.6,1.0, > 1.2 νLν(5µm) ≃ 2 × 109L⊙

(

M∗ 1011M⊙

)0.5 (1 + z)4

AGN activities are Weak mass depedence, More rapid evolution than SFR

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Synergy with Herschel/PACS

Ishigaki+14 in Preparation Confirming Hanami+, 2012, PASJ, 64, 4

Opt-NIR Fitting → zphot, M∗ Star < 2µm Dust > 5µm Subaru

Not CFHT

AKARI Herschel/PACS

→ Tdust, Mdust, ρdustwith Improving L(IR; SF), L(IR; AGN), f(AGN) =

L(IR;AGN) L(IR;AGN)+L(IR;SF) 10

Synergy with CXO

All MIR AGNs emit X-ray? @z< .4,∼ .6,∼ 1.0,> 1.2

L(5µm) L(2 − 7keV ) Krumpe,Miyaji,Ishigaki,HH+14 in prep. 0.5 − 2.0keV Stacking for ∼ 400 MIR AGN& AGN/SF w/o X-ray 2.0 − 8.0keV

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AGNs Co-Exist with SF @z∼ 0.6,∼ 1.0,> 1.2 MIR &X-ray AGNs with SF

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Catch AGNs with MIR, X-ray, & BPT f(AGN) =

LIR(AGN) LIR(AGN+SF) L(5µm;AGN) L(5µm;AGN+SF)

f < 0.1 SF←

SFw/AGN

f > 0.3 →AGN [NII]/Hα [OIII]/Hβ

L(5µm) is sensitive to detect AGN X-ray(square) ∼ AGNs in BPT ∼ f(AGN) > 0.3

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f(AGN) → AKARI+Herschel Colors

[7] − [11] [11] − [100] AGNւ րSF [7] − [11] [11] − [100] [9] − [15] [15] − [100] AGNւ րSF [9] − [15] [15] − [100] [11] − [18] [18] − [100] AGNւ րSF [11] − [18] [18] − [100]

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Rest Frame SEDs, Again @z ≃0.6,1.0, > 1.2

magenta:BL AGN

Spectroscopic

AGN StarForming +PACS

SFwAGN SF Dominated

Photometric

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M∗, SFR, sSFR @z< .4,∼ .6,∼ 1.0,> 1.2 M∗ SFR(IR + UV ) AGN M∗ SFR(IR + UV ) SFw/AGN M∗ SFR(IR + UV ) StarForming M∗ sSFR AGN M∗ sSFR SFw/AGN M∗ sSFR StarForming

· SFR ↓ as f(AGN) ↑ → AGN Quenches SF?

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M∗ vs. Mdust @z< .4,∼ .6,∼ 1.0,> 1.2 M∗ Mdust AGN M∗ Mdust SFw/AGN M∗ Mdust StarForming z ∼ 0.2

ւ

z ∼ 1.0 ∆Mdust րց as f(AGN) ↑

∆Mdust ∼ 107 ← 109M⊙@z ∼ 0.2 ← 1.0

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Mdust vs. SFR, LIR(AGN)

@z< .4,∼ .6,∼ 1.0,> 1.2

Mdust

SFR(IR + UV )

ւ ց Mdust

LIR(AGN)

ւ ց

Mdust is Essential for Tracing Evolution

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Mdust/M∗ vs. L(10µm)/L(8µm)

All

Mdust/M∗ L(10µm)/L(8µm)

• nly SF

Mdust/M∗ L(10µm)/L(8µm) Si Abs.@10µm ↔ Mdust ∼ MISM

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Mdust vs, L(8µm)/LIR(SF) sSFR(IR + UV ) L(8µm)/LIR(SF) Mdust L(8µm)/LIR(SF) Mdust Tracing PAH Defict? ↔

IRS+MIPS+PACS@z ∼ 2; Nordon+13

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Summary

• Studying LIRGs @z < 2

with Opt.+MIR+FIR+X-Ray – MIR diagnostics → Passfinder for JWST/MIRI ∗ SF ↔ 8µm ∗ AGN ↔ 5µm ∗ Mdust ↔ 10µm – Adding FIR ∗ Rapid Ev. of Mdust ց during z = 0.4 − 0.8 ∗ Mdust tracing CoEv. of ⋆, ISM(Dust), AGN

• Correct understanding for Radiation Transfer

– Do not extrapolate Screen model picture!

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