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

X.Y.XiaX.Y.XiaTianjin Normal University, ChinaTianjin Normal University, China

Collaborators: C.N.Hao, S.Mao, Z.G.Deng &H.WuCollaborators: C.N.Hao, S.Mao, Z.G.Deng &H.Wu

MotivationMotivation • The tight correlation between Mbh and the mass of The tight correlation between Mbh and the mass of

host spheriodhost spheriod Kommendy&Gebhardt 2001, Merritt & Ferrarese Kommendy&Gebhardt 2001, Merritt & Ferrarese 20012001

• The Star Formation History and Distribution of QSOsThe Star Formation History and Distribution of QSOs Heckman et al. 2004; Springel et alHeckman et al. 2004; Springel et al..

• How such correlation arise?How such correlation arise? Does it always exist?Does it always exist? the growing process of Mbh and spheriodthe growing process of Mbh and spheriod

Different SFR/Mdot for different stages of galaxy Different SFR/Mdot for different stages of galaxy assemplyassemply

The SFR/Mdot about 1000 for local narrow emission line AGNThe SFR/Mdot about 1000 for local narrow emission line AGN Heckman & Kauffmann 2004Heckman & Kauffmann 2004• The SFR/Mdot about several hundred for IR QSOsThe SFR/Mdot about several hundred for IR QSOs Hao et al. Hao et al.

20052005• The SFR/Mdot >1000 for SMGs The SFR/Mdot >1000 for SMGs Alexander et al. 2005Alexander et al. 2005• The SFR/Mdot less than 10 for typical QSOsThe SFR/Mdot less than 10 for typical QSOs

黑洞质量与星系核球质量有很好的相关

MotivationMotivation • The tight correlation between Mbh and the mass of The tight correlation between Mbh and the mass of

host spheriodhost spheriod Kommendy&Gebhardt 2001, Merritt & Ferrarese Kommendy&Gebhardt 2001, Merritt & Ferrarese 20012001

• The Star Formation History and Distribution of QSOsThe Star Formation History and Distribution of QSOs Heckman et al. 2004; Springel et alHeckman et al. 2004; Springel et al..

• How such correlation arise?How such correlation arise? Does it always exist?Does it always exist? the growing process of Mbh and spheriodthe growing process of Mbh and spheriod

Different SFR/Mdot for different stages of galaxy Different SFR/Mdot for different stages of galaxy assemplyassemply

The SFR/Mdot about 1000 for local narrow emission line AGNThe SFR/Mdot about 1000 for local narrow emission line AGN Heckman & Kauffmann 2004Heckman & Kauffmann 2004• The SFR/Mdot about several hundred for IR QSOsThe SFR/Mdot about several hundred for IR QSOs Hao et al. Hao et al.

20052005• The SFR/Mdot >1000 for SMGs The SFR/Mdot >1000 for SMGs Alexander et al. 2005Alexander et al. 2005• The SFR/Mdot less than 10 for typical QSOsThe SFR/Mdot less than 10 for typical QSOs

SMGsTypical QSOs

ULIRGs PG QSOs

SFR

Mdot

SFR

Mdot

>1000

<10.2

tens

IR QSOs

FIR super-LuminousQSOs

Thansition phase

High-z

>100 1

<1

Transition stage from merger to ellipticals

IR QSOs are in transitionary IR QSOs are in transitionary stagestage

• Strong FeII emittersStrong FeII emitters

• High Eddington ratioHigh Eddington ratio

• Steep x-ray slopSteep x-ray slop

at one extreme end of Eigenvecgtor 1 and at one extreme end of Eigenvecgtor 1 and they are young QSOsthey are young QSOs

• StarburstStarburst

• The starburst and central AGN give main The starburst and central AGN give main contributions at different wavebandcontributions at different waveband

• By comparing optical and IR QSOs sample,By comparing optical and IR QSOs sample,

It is possible to separate the contributionsIt is possible to separate the contributions

• Determining SFR and MdotDetermining SFR and Mdot

IR QSOs at Low redshiftIR QSOs at Low redshift(Hao at al. 2005)(Hao at al. 2005)

(1)(1) IR QSO sampleIR QSO sample

Zheng et al. (2002)Zheng et al. (2002)

(2)(2) The optically-selected QSO sampleThe optically-selected QSO sample

PG QSOs , BG92 (1992), Haas et al. (2003)PG QSOs , BG92 (1992), Haas et al. (2003)

(3)(3) NLS1 sampleNLS1 sample Wang & Lu (2001)Wang & Lu (2001)

Sample SelectionSample Selection

• 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

High-z QSOsHigh-z QSOs

•Rest Frame Submillimeter Rest Frame Submillimeter Detected QSOs (57)Detected QSOs (57)

•Typical QSOs (95) Typical QSOs (95)

Optically selected QSOs at redshift about 4 with Optically selected QSOs at redshift about 4 with 1.2mm observation, 1.2mm observation, Omont et al. (2001)Omont et al. (2001)

Optically selected QSOs at redshift about 4 with Optically selected QSOs at redshift about 4 with 1.2mm observation, 1.2mm observation, Carilli et al. (2001)Carilli et al. (2001)

Optically selected QSOs at redshift about 2 with Optically selected QSOs at redshift about 2 with 1.2mm observation, 1.2mm observation, Omont et al. (2003)Omont et al. (2003)

X-ray absorbed and submillimeter detectedX-ray absorbed and submillimeter detected QSOs QSOs Stevens et al. (Stevens et al. (2005)2005) CO/HCN detected QSOs CO/HCN detected QSOs Carrilli et al. (2002, Carrilli et al. (2002,

2005)2005)

SampleSample

T=41K, ß=1.95

Parameters estimates at Parameters estimates at high zhigh zSFRSFR:: Monochromatic luminosity at 60Monochromatic luminosity at 60mm the monochromatic luminosity at 60the monochromatic luminosity at 60m from the m from the

flux density at 1.2mm by assuming the rest-flux density at 1.2mm by assuming the rest-frame FIR SED can be described by frame FIR SED can be described by

a greybody spectrum with the dust temperature a greybody spectrum with the dust temperature of 41K and the dust emissivity of 1.95 of 41K and the dust emissivity of 1.95

Priddey & McMahon (2001).Priddey & McMahon (2001).

MdotMdot:: Bolometric luminosity Bolometric luminosity Vestergaard Vestergaard (2004 )(2004 )

Bbol LL 74.9

sun

bolsun L

LyrMM

131

1074.6

sun

msun L

LyrMSFR

10

601

1026.3

Accretion rate

Star formation rate

04.052.0

11)7.530.389(

yrM

MyrMSFR

sunsun

SMGsTypical QSOs

ULIRGs PG QSOs

SFR

Mdot

SFR

Mdot

>1000

<10.2

10

IR QSOs

FIR super-LuminousQSOs

Thansition phase

High-z

>100 1

<1

SummarySummary

• Typical QSOs at both low and high Typical QSOs at both low and high redshift) are satisfied the same Lfir redshift) are satisfied the same Lfir and Lbol relationand Lbol relation

• The FIR excess of low and high The FIR excess of low and high redshift QSOs originates from redshift QSOs originates from starburst starburst

• The SFR/Mdot for low-z IR QSOs and The SFR/Mdot for low-z IR QSOs and high-z submillimeter detected QSOs high-z submillimeter detected QSOs is several hundredis several hundred

• The Mbh-MThe Mbh-M* * relation could be built up relation could be built up during this short period (10during this short period (1077 toto 10108 8 yr)yr)

Thank You