很可能是由ULIRGs到光學(xué)選類星體如PGQSOsICRANet課件

1、 Mid- Infrared Spectroscopic Properties of IR QSOs XiaoYang, Xia Center for Astrophysics Tianjin Normal University OutlineInfrared Luminous QSOs (IR QSO) Spitzer IRS Spectra of IR QSOsULIRGs Optical selected QSOs (sanders, 1988)Merger of gas-rich galaxies gas-falling to center of galaxyULIRGs QSOs f

2、eedback圖取自 Hopkins et al. (2008)氣體耗盡, 塵 埃被完全吹散 Mrk 231 Canalizo & Stockton (2001) Mrk231IR QSOs are at Transition Stage from Merger to QSOs, then to EllipticalsThe Coeval Growth of Black Holes and their host SpheriodsThe statistical properties of IR QSOs at optical and infrared bandsThe optical spec

3、toscopic propertiesThe infrared properties 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 (z0.35)，takes a fraction of about 25% in local universe. Based on the sample

4、, statistical results should be representative. Z=6Z=6Z=6Carilli et al. 2007 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

5、, z0.27 + PG QSOs from QUEST (Schweitzer et al. 2006) SampleHow to measure the SFR at QSOsTorus of QSOs could give FIR emission Haas et al. 2003Lir/Lco, Lir/L(HCN) are higher for QSOs than those of ULIRGs Evens et al. 2007Spitzer IRS observations for IR QSO Cao Chen et al. 200719 IR QSOs have been o

6、bserved By Spitzer IRSResults 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, z0.27 + PG QSOs from QUEST (Schweitzer et al.

7、 2006) SampleThe Mid-IR Spectra of IR QSOsMid-IR slopPAH emissionsFine-structure line emissions The low resolution mid-infrared spectra of IR QSOs ULIRGs IR QSOs PG QSOsSFR Fine structure line NeII 12.81m SFR indicator in QSOs log L(PAH 6.2m)LSFRSFR MBH H blueshift Feedback may play role to suppress

8、 both star formation and AGNAnti-correlated SummaryMid-IR to Far-IR slop reflects the relative contribution from central AGN and SFNeII is a good indicator for SFRFeedback plays role on suppressing both starburst and AGN Further worksMolecular gas content by IRAM 30mHerschel observations on high-z QSOs Thank you Silicate absorptionThe diverse properties of Mid-IR spectra of ULIRGsMolecular disk/ring at ULIRGs Sample19 IR QSOs (Hao et al. 2005)20 PG QSOs 的中紅外光譜數(shù)據(jù) (Schweitzer et al. 2006)35 ULIRGs (from IRAS 1Jy sample, Kim & Sanders 1998) 紅外類星體 (IR QSOs) 具有I-型活動星