1. Mid- Infrared Spectroscopic Properties of IR QSOs
XiaoYang, Xia
Center for Astrophysics
Tianjin Normal University

2. Outline
Infrared Luminous QSOs (IR QSO)
Spitzer IRS Spectra of IR QSOs

3. ULIRGs  Optical selected QSOs (sanders, 1988)
gas-falling to center of galaxy
Merger of gas-rich galaxies
ULIRGs
feedback
QSOs
气体耗尽, 尘 埃被完全吹散
图取自 Hopkins
et al. (2008)

5. Mrk 231
Canalizo &
Stockton (2001)
Mrk231

6. The Coeval Growth of Black Holes and their host Spheriods
IR QSOs are at Transition Stage from Merger to QSOs, then to Ellipticals
The Coeval Growth of Black Holes and their host Spheriods

8. The statistical properties of IR QSOs at optical and infrared bands
The optical spectoscopic properties
The infrared properties

9. IR QSO Sample QDOT IRAS galaxy sample (Lawrence et al. 1999)
1 Jy ULIRGs sample (Kim & Sanders 1998)
IRAS-ROSAT cross-identification sample (Moran et al. 1996)
A sample of 31 IR QSOs (z<0.35)，takes a fraction
of about 25% in local universe. Based on the sample, statistical results should be representative.

16. Z=6
Z=6
Z=6
Carilli et al. 2007

17. Sample
19 IR QSOs
Hao et al. 2005, 15 have both low & high –res obs.
35 ULIRGs
IRAS 1-Jy sample and Spitzer GTO #105 + High-resolution mid-IR data, Farrah et al. (2007)
20 PG QSOs
Spitzer GTO & GO #14, 3187 & 20142, with enough S/N, z< PG QSOs from QUEST (Schweitzer et al. 2006)

18. How to measure the SFR at QSOs
Torus of QSOs could give FIR emission
Haas et al. 2003
Lir/Lco, Lir/L(HCN) are higher for QSOs than those of ULIRGs
Evens et al. 2007

19. Spitzer IRS observations for IR QSO Cao Chen et al. 2007
19 IR QSOs have been observed
By Spitzer IRS
Results

20. Sample
19 IR QSOs
Hao et al. 2005, 15 have both low & high –res obs.
35 ULIRGs
IRAS 1-Jy sample and Spitzer GTO #105 + High-resolution mid-IR data, Farrah et al. (2007)
20 PG QSOs
Spitzer GTO & GO #14, 3187 & 20142, with enough S/N, z< PG QSOs from QUEST (Schweitzer et al. 2006)

21. The Mid-IR Spectra of IR QSOs
Mid-IR slop
PAH emissions
Fine-structure line emissions

22. ③
The low resolution mid-infrared spectra
of IR QSOs

23. ③

24. ULIRGs IR QSOs PG QSOs ③
SFR

25. ③

26. ③ Fine structure line [NeII] 12.81m  SFR indicator in QSOs SFR
log L(PAH 6.2m)∕L⊙

27. ③

28. ③ Feedback may play role to suppress both star formation and AGN ˙ SFR
Anti-correlated
SFR
MBH ˙
H blueshift

29. Summary Mid-IR to Far-IR slop reflects the relative
contribution from central AGN and SF
NeII is a good indicator for SFR
Feedback plays role on suppressing both starburst and AGN

30. Further works Molecular gas content by IRAM 30m
Herschel observations on high-z QSOs

31. Thank you

38. The diverse properties of Mid-IR spectra of ULIRGs
Silicate absorption
The diverse properties of Mid-IR spectra of ULIRGs
Molecular disk/ring at ULIRGs

63. Sample 19 IR QSOs (Hao et al. 2005)
20 PG QSOs 的中红外光谱数据 (Schweitzer et al. 2006)
35 ULIRGs (from IRAS 1Jy sample, Kim & Sanders 1998)

65. 红外类星体 (IR QSOs) — 具有I-型活动星系核光学光谱 特征的极亮红外星系; — 多呈现并合晚期的形态;
Mrk 231
红外类星体 (IR QSOs)
— 具有I-型活动星系核光学光谱
特征的极亮红外星系;
— 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;
— 很可能是由 ULIRGs 到光学选类星体
(如 PG QSOs) 演化
过程中的过渡源。
IRAS 中-远红外双色图
Canalizo &
Stockton (2001)