The Coeval Growth of Black Holes and their host Spheriods

1. The Coeval Growth of Black Holes and their host Spheriods X.Y.Xia Tianjin Normal University, China Collaborators: C.N.Hao, S.Mao, Z.G.Deng &H.Wu

2. Motivation • The tight correlation between Mbh and the mass of host spheriodKommendy&Gebhardt 2001, Merritt & Ferrarese 2001 • The Star Formation History and Distribution of QSOs Heckman et al. 2004; Springel et al. • How such correlation arise?Does it always exist? the growing process of Mbh and spheriod Different SFR/Mdot for different stages of galaxy assemply The SFR/Mdot about 1000 for local narrow emission line AGN Heckman & Kauffmann 2004 • The SFR/Mdot about several hundred for IR QSOsHao et al. 2005 • The SFR/Mdot >1000 for SMGs Alexander et al. 2005 • The SFR/Mdot less than 10 for typical QSOs

6. Motivation • The tight correlation between Mbh and the mass of host spheriodKommendy&Gebhardt 2001, Merritt & Ferrarese 2001 • The Star Formation History and Distribution of QSOs Heckman et al. 2004; Springel et al. • How such correlation arise?Does it always exist? the growing process of Mbh and spheriod Different SFR/Mdot for different stages of galaxy assemply The SFR/Mdot about 1000 for local narrow emission line AGN Heckman & Kauffmann 2004 • The SFR/Mdot about several hundred for IR QSOsHao et al. 2005 • The SFR/Mdot >1000 for SMGs Alexander et al. 2005 • The SFR/Mdot less than 10 for typical QSOs

7. 1 SFR >100 PG QSOs IR QSOs ULIRGs Mdot <1 Thansition phase tens >1000 SFR FIR super- Luminous QSOs High-z SMGs Typical QSOs Mdot 0.2 <1

8. Transition stage from merger to ellipticals

11. IR QSOs are in transitionary stage • Strong FeII emitters • High Eddington ratio • Steep x-ray slop at one extreme end of Eigenvecgtor 1 and they are young QSOs • Starburst

12. The starburst and central AGN give main contributions at different waveband • By comparing optical and IR QSOs sample, It is possible to separate the contributions • Determining SFR and Mdot

13. IR QSOs at Low redshift (Hao at al. 2005) • IR QSO sample Zheng et al. (2002) (2)The optically-selected QSO sample PG QSOs , BG92 (1992), Haas et al. (2003) • NLS1 sample Wang & Lu (2001)

14. Sample Selection • QDOTIRAS galaxy sample(Lawrence et al. 1999) • 1 JyULIRGs sample(Kim & Sanders 1998) • IRAS-ROSATcross-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.

21. High-z QSOs • Rest Frame Submillimeter Detected QSOs (57) • Typical QSOs (95)

22. Sample • Optically selected QSOs at redshift about 4 with 1.2mm observation, Omont et al. (2001) • Optically selected QSOs at redshift about 4 with 1.2mm observation, Carilli et al. (2001) • Optically selected QSOs at redshift about 2 with 1.2mm observation, Omont et al. (2003) • X-ray absorbed and submillimeter detected QSOs Stevens et al. (2005) • CO/HCN detected QSOs Carrilli et al. (2002, 2005)

23. T=41K, ß=1.95

25. Parameters estimates at high z SFR:Monochromatic luminosity at 60m the monochromatic luminosity at 60m from the flux density at 1.2mm by assuming the rest-frame FIR SED can be described by a greybody spectrum with the dust temperature of 41K and the dust emissivity of 1.95 Priddey & McMahon (2001). Mdot: Bolometric luminosity Vestergaard (2004 )

26. Accretion rate Star formation rate

30. 1 SFR >100 PG QSOs IR QSOs ULIRGs Mdot <1 Thansition phase 10 >1000 SFR FIR super- Luminous QSOs High-z SMGs Typical QSOs Mdot 0.2 <1

31. Summary • Typical QSOs at both low and high redshift) are satisfied the same Lfir and Lbol relation • The FIR excess of low and high redshift QSOs originates from starburst • The SFR/Mdot for low-z IR QSOs and high-z submillimeter detected QSOs is several hundred • The Mbh-M* relation could be built up during this short period (107to108 yr)

32. Thank You