Mid- Infrared Spectroscopic Mid- Infrared Spectroscopic Properties Properties of IR QSOs of IR QSOs

XiaoYang, XiaXiaoYang, Xia Center for AstrophysicsCenter for Astrophysics Tianjin Normal UniversityTianjin Normal University

OutlineOutline

•Infrared Luminous QSOs (IR Infrared Luminous QSOs (IR QSO)QSO)

•Spitzer IRS Spectra of IR Spitzer IRS Spectra of IR QSOsQSOs

ULIRGs ULIRGs Optical selected QSOs Optical selected QSOs (sanders, (sanders, 1988)1988)

Merger of Merger of gas-rich gas-rich galaxiesgalaxies

gas-falling to gas-falling to center of galaxycenter of galaxyULIRGsULIRGs

QSOsQSOs

feedbacfeedbackk

图取自图取自 Hopkins Hopkins et al. (2008)et al. (2008)

气体耗尽气体耗尽 , , 尘 尘 埃被完全吹散埃被完全吹散

Mrk 231

Canalizo & Stockton (2001)

Mrk231Mrk231

IR QSOs are at Transition Stage IR QSOs are at Transition Stage from Merger to QSOs, then to from Merger to QSOs, then to EllipticalsEllipticals

The Coeval Growth of Black The Coeval Growth of Black Holes and their host Holes and their host

SpheriodsSpheriods

黑洞质量与星系核球质量有很好的相关

The statistical properties of IR The statistical properties of IR QSOs QSOs at optical and infrared bands at optical and infrared bands

•The optical spectoscopic The optical spectoscopic propertiesproperties

•The infrared propertiesThe infrared properties

IR QSO Sample IR QSO Sample

• QDOTQDOT IRAS galaxy sampleIRAS galaxy sample (Lawrence et al. (Lawrence et al. 1999)1999)

• 1 Jy1 Jy ULIRGs sampleULIRGs sample (Kim & Sanders 1998)(Kim & Sanders 1998)

• IRAS-ROSATIRAS-ROSAT cross-identification samplecross-identification sample (Moran et al. 1996)(Moran et al. 1996)

A sample ofA sample of 31 31 IR QSOs (IR QSOs (z<0.35z<0.35)) ，， takes a takes a

fraction fraction

of about of about 25% 25% in local universe. Based on the in local universe. Based on the sample, statistical results should be representativesample, statistical results should be representative..

29.0

118.588

yrM

M

yrM

SFR

sunsun

Z=6Z=6Z=6

Carilli et al. 2007

19 19 IR QSOsIR QSOs Hao et al. 2005, 15 have both low & high –res obs. Hao et al. 2005, 15 have both low & high –res obs.

3535 ULIRGsULIRGs

IRASIRAS 1-Jy sample and 1-Jy sample and SpitzerSpitzer GTO #105 + High- GTO #105 + High-resolution mid-IR data, Farrah et al. (2007)resolution mid-IR data, Farrah et al. (2007)

2020 PG QSOsPG QSOs Spitzer GTO & GO #14, 3187 & 20142, with enough Spitzer GTO & GO #14, 3187 & 20142, with enough

S/N, z<0.27 + PG QSOs from QUEST (Schweitzer et al. S/N, z<0.27 + PG QSOs from QUEST (Schweitzer et al. 2006)2006)

Sample

How to measure the SFR at How to measure the SFR at QSOsQSOs

• Torus of QSOs could give FIR Torus of QSOs could give FIR emissionemission

Haas et al. 2003Haas et al. 2003

• Lir/Lco, Lir/L(HCN) are higher for Lir/Lco, Lir/L(HCN) are higher for QSOs than those of ULIRGsQSOs than those of ULIRGs

Evens et al. 2007Evens et al. 2007

Spitzer IRS observations for IR Spitzer IRS observations for IR QSOQSO

Cao Chen et al. 2007Cao Chen et al. 2007

•19 IR QSOs have been 19 IR QSOs have been observedobserved

By Spitzer IRSBy Spitzer IRS

•ResultsResults

19 19 IR QSOsIR QSOs Hao et al. 2005, 15 have both low & high –res obs. Hao et al. 2005, 15 have both low & high –res obs.

3535 ULIRGsULIRGs

IRASIRAS 1-Jy sample and 1-Jy sample and SpitzerSpitzer GTO #105 + High- GTO #105 + High-resolution mid-IR data, Farrah et al. (2007)resolution mid-IR data, Farrah et al. (2007)

2020 PG QSOsPG QSOs Spitzer GTO & GO #14, 3187 & 20142, with enough Spitzer GTO & GO #14, 3187 & 20142, with enough

S/N, z<0.27 + PG QSOs from QUEST (Schweitzer et al. S/N, z<0.27 + PG QSOs from QUEST (Schweitzer et al. 2006)2006)

Sample

The Mid-IR Spectra of IR The Mid-IR Spectra of IR QSOsQSOs

•Mid-IR slopMid-IR slop

•PAH emissionsPAH emissions

•Fine-structure line emissionsFine-structure line emissions

The low resolution mid-infrared spectra The low resolution mid-infrared spectra of IR QSOs of IR QSOs

③③

③③

③③ ULIRGsULIRGs

IR QSOsIR QSOs

PG PG QSOsQSOs

SFRSFR

③③

Fine structure line Fine structure line [NeII] 12.81[NeII] 12.81mm SFR indicator in SFR indicator in QSOsQSOs

③③

log L(PAH 6.2log L(PAH 6.2m)∕Lm)∕L⊙⊙

SFRSFR

③③

③③

SFRSFR

MMBHBH

˙̇

HH blueshift blueshift

• Feedback may play role to suppress Feedback may play role to suppress both both

• star formation and AGNstar formation and AGN

Anti-correlatedAnti-correlated

SummarySummary

• Mid-IR to Far-IR slop reflects the relativeMid-IR to Far-IR slop reflects the relative

contribution from central AGN and SFcontribution from central AGN and SF

• NeII is a good indicator for SFRNeII is a good indicator for SFR

• Feedback plays role on suppressing Feedback plays role on suppressing both starburst and AGNboth starburst and AGN

Further worksFurther works

• Molecular gas content by IRAM 30mMolecular gas content by IRAM 30m

• Herschel observations on high-z Herschel observations on high-z QSOsQSOs

Thank youThank you

Silicate absorptionSilicate absorption

•The diverse properties of The diverse properties of Mid-IR spectra of ULIRGsMid-IR spectra of ULIRGs

•Molecular disk/ring at Molecular disk/ring at ULIRGsULIRGs

SampleSample

• 19 19 IR QSOsIR QSOs (Hao et al. 2005)(Hao et al. 2005)

• 20 20 PG QSOs PG QSOs 的中红外光谱数据的中红外光谱数据 ((Schweitzer et al. Schweitzer et al. 2006)2006)

• 35 35 ULIRGs ULIRGs (from (from IRASIRAS 1Jy sample, 1Jy sample, Kim & Sanders Kim & Sanders 1998)1998)

红外类星体 红外类星体 (IR (IR QSOs)QSOs)

—— 具有具有 I-I- 型活动星系核光学光谱型活动星系核光学光谱 特征的极亮红外星系特征的极亮红外星系 ;; — — 多呈现并合晚期的形态多呈现并合晚期的形态 ;;—— 拥有较高的恒星形成率与黑洞吸积率拥有较高的恒星形成率与黑洞吸积率 ;;—— 很可能是由 很可能是由 ULIRGs ULIRGs 到光学选类星体 到光学选类星体 (( 如如 PG QSOsPG QSOs)) 演化演化 过程中的过渡源。过程中的过渡源。

Mrk 231

Canalizo & Stockton (2001)

IRAS 中 -远红外双色图