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 1

Why & How to study LIRGs up to z ∼ 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 → ⋆ & z phot – 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. 2

AKARI covers 2 , 3 , 4 , 7 , 9 , 11 , 15 , 18 , 24 µ m ← ⋆ ց ր Dust 5 µ m ;Window for AGN 3 µ m 4 µ m 7 µ m ← PAH8 µ m @ z < 2 → 9 µ m 11 µ m15 µ m 24 µ m 18 µ m • PAH@8 µ m → SFR @ z < 2 • ⋆ ց before Dust ր @5 µ m → Window for AGN → Distinction between SF/AGN-LIRGs 3

z vs. νL ν (8 µm ) : νL ν (8 µm ) ≃ 0 . 1 L tIR MIR-all:SF MIR-all:s-BBG MIR-all:p(qp)-BBG ULIRGs LIRGs IRGs MIR-B:SF MIR-B:SF/AGN MIR-B:AGN ULIRGs LIRGs IRGs 11 15 18 24 11 15 18 24 11 15 18 24 z ≃ 1 z ≃ 2 z ≃ 1 z ≃ 2 z ≃ 1 z ≃ 2 4

MIR Color-Color Diag. @ z ≃ 0.6,1.0, > 1 . 2 z ≥ 1 . 2 z ≃ 0 . 6 z ≃ 1 [15] − [18] [11] − [15] [11] − [15] [11] − [15] [9] − [11] [9] − [11] z ≥ 1 . 2 z ≃ 0 . 6 z ≃ 1 [15] − [18] [11] − [15] [11] − [15] StarForming StarForming StarForming AGN AGN AGN [11] − [15] [9] − [11] [9] − [11] 7 . 7 µ m PAH @ z ≃ 1(1 . 5) detected with L15(L18W) 5

Rest Frame SEDs of AGN,SFw/AGN,SF @ z ≃ 0 . 6,1 . 0, > 1 . 2 Spectroscopic magenta:BL AGN SFw/AGN SF Dominated Photometric AGN StarForming 6

z phot , M ∗ , SFR IR , f(AGN) for > 1000 LIRGs Hanami+, 2012, PASJ, 64, 4 Star < 2 µ m Dust > 5 µ m Fitting with BC03 Fitting with ↓ Dusty SF (SK08) + Torus (QSO2) → νL 8 − 1000 µm ∼ L ( IR ; SF ) ∼ SFR IR z phot , M ∗ , A V , SFR UV → νL 8 µm ∼ L ( IR ; AGN ) 7

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 ) ) 0 . 7 (1 + z ) 2 ( M ∗ SFR MS ≃ 25 M ⊙ yr − 1 10 11 M ⊙ � SFR IR � > SFR MS @ z > 0 . 4 8

5 µ m between ⋆ and Dust → Window for AGN AGN SF/AGN StarForming @ z ≃ 0 . 6,1 . 0, > 1 . 2 ) 0 . 5 (1 + z ) 4 ( νL ν (5 µm ) ≃ 2 × 10 9 L ⊙ M ∗ 10 11 M ⊙ AGN activities are Weak mass depedence, More rapid evolution than SFR 9

Synergy with Herschel/PACS Ishigaki+14 in Preparation Confirming Hanami+, 2012, PASJ, 64, 4 Star < 2 µ m Dust > 5 µ m Subaru AKARI Herschel/PACS Not CFHT → T dust , M dust , ρ dust with Improving L ( IR ; SF ), L ( IR ; AGN ), Opt-NIR Fitting L ( IR ; AGN ) → z phot , M ∗ f ( AGN ) = L ( IR ; AGN )+ L ( IR ; SF ) 10

Synergy with CXO All MIR AGNs emit X-ray? @ z< . 4, ∼ . 6, ∼ 1 . 0, > 1 . 2 Krumpe,Miyaji,Ishigaki,HH+14 in prep. L (2 − 7 keV ) 0 . 5 − 2 . 0keV 2 . 0 − 8 . 0keV L (5 µm ) Stacking for ∼ 400 MIR AGN& AGN/SF w/o X-ray 11

AGNs Co-Exist with SF @ z ∼ 0 . 6 , ∼ 1 . 0 , > 1 . 2 MIR &X-ray AGNs with SF 12

Catch AGNs with MIR, X-ray, & BPT L (5 µm ; AGN + SF ) L (5 µm ; AGN ) [OIII]/H β f > 0 . 3 f < 0 . 1 → AGN SF ← SFw/AGN L IR ( AGN ) [NII]/H α f ( AGN ) = L IR ( AGN + SF ) L (5 µm ) is sensitive to detect AGN X-ray(square) ∼ AGNs in BPT ∼ f ( AGN ) > 0 . 3 13

f(AGN) → AKARI+Herschel Colors [15] − [100] [18] − [100] [11] − [100] ր SF ր SF ր SF AGN ւ AGN ւ AGN ւ [9] − [15] [11] − [18] [7] − [11] [15] − [100] [18] − [100] [11] − [100] [9] − [15] [11] − [18] [7] − [11] 14

Rest Frame SEDs, Again @ z ≃ 0 . 6,1 . 0, > 1 . 2 +PACS Spectroscopic magenta:BL AGN SFwAGN SF Dominated Photometric AGN StarForming 15

M ∗ , SFR, sSFR @ z< . 4 , ∼ . 6 , ∼ 1 . 0 , > 1 . 2 AGN SF w/ AGN StarForming SFR ( IR + UV ) SFR ( IR + UV ) SFR ( IR + UV ) M ∗ M ∗ M ∗ AGN SF w/ AGN StarForming sSFR sSFR sSFR M ∗ M ∗ M ∗ · SFR ↓ as f(AGN) ↑ → AGN Quenches SF? 16

M ∗ vs. M dust @ z< . 4 , ∼ . 6 , ∼ 1 . 0 , > 1 . 2 AGN SF w/ AGN StarForming z ∼ 1 . 0 ւ M dust M dust M dust z ∼ 0 . 2 M ∗ M ∗ M ∗ ∆ M dust րց as f(AGN) ↑ ∆ M dust ∼ 10 7 ← 10 9 M ⊙ @ z ∼ 0 . 2 ← 1 . 0 17

M dust vs. SFR, LIR(AGN) @ z< . 4, ∼ . 6, ∼ 1 . 0, > 1 . 2 SFR ( IR + UV ) LIR ( AGN ) ց ց ւ ւ M dust M dust M dust is Essential for Tracing Evolution 18

M dust /M ∗ vs. L (10 µm ) /L (8 µm ) L (10 µm ) /L (8 µm ) L (10 µm ) /L (8 µm ) All only SF M dust /M ∗ M dust /M ∗ Si Abs. @10 µ m ↔ M dust ∼ M ISM 19

M dust vs, L (8 µm ) /LIR ( SF ) L (8 µm ) /LIR ( SF ) L (8 µm ) /LIR ( SF ) sSFR ( IR + UV ) M dust M dust Tracing PAH Defict? ↔ IRS+MIPS+PACS@ z ∼ 2; Nordon+13 20

Summary • Studying LIRGs @ z < 2 with Opt.+MIR+FIR+X-Ray – MIR diagnostics → Passfinder for JWST/MIRI ∗ SF ↔ 8 µm ∗ AGN ↔ 5 µm ∗ M dust ↔ 10 µm – Adding FIR ∗ Rapid Ev. of M dust ց during z = 0 . 4 − 0 . 8 ∗ M dust tracing CoEv. of ⋆ , ISM(Dust), AGN • Correct understanding for Radiation Transfer – Do not extrapolate Screen model picture! 21