From ULIRGs to QSOsFrom ULIRGs to QSOs

XiaoYang, XiaXiaoYang, Xia

Center for AstrophysicsCenter for Astrophysics

Tianjin Normal UniversityTianjin Normal University

Collaborators: H. Wu, Deng, Zou, Z. Zheng, Collaborators: H. Wu, Deng, Zou, Z. Zheng, Mao, X.Z. Zheng, Hao, Huo, Y. Gao, Mao, X.Z. Zheng, Hao, Huo, Y. Gao, Wang,J.L, TanWang,J.L, Tan

OutlineOutline•The morphology and The morphology and

environment of ULIRGs and environment of ULIRGs and LIRGsLIRGs

May give hint for high-z SMGsMay give hint for high-z SMGs

•Infrared luminous QSOs Infrared luminous QSOs may give hint on high-z submm loud QSOsmay give hint on high-z submm loud QSOs

Then the relation of ULIRGs with SMGs and IR Then the relation of ULIRGs with SMGs and IR QSOs with submm loud QSOsQSOs with submm loud QSOs

The morphology of ULIRGs The morphology of ULIRGs

• Based on Based on 9797 HST snapshot images, we find that all HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei fractions of single, double and multi-nucleus/nuclei are are 43%, 39% and 18%,43%, 39% and 18%, respectively respectively

• The AGN fraction is 80%, 65% to 36% from single, The AGN fraction is 80%, 65% to 36% from single, double and multi-nucleus/nuclei double and multi-nucleus/nuclei

• QSOs and ellipticals appear at last stage of mergerQSOs and ellipticals appear at last stage of merger

• Some ULIRGs have extended soft X-ray halo based Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)on Chandra observations (e.g. NGC 6240, Mrk 273)

Cui et al. 2002

The morphology of ULIRGs The morphology of ULIRGs • All ULIRGs are interacting/merging galaxies and the All ULIRGs are interacting/merging galaxies and the

fractions of single, double and multi-nucleus/nuclei fractions of single, double and multi-nucleus/nuclei are are 43%, 39% and 18%,43%, 39% and 18%, respectively, based on 97 respectively, based on 97 HST snapshot images. HST snapshot images.

• The AGN fractions areThe AGN fractions are 80% 65% 36% 80% 65% 36% single double multi nucleus/nuclei single double multi nucleus/nuclei (total AGN fraction is about 65%, similar as (total AGN fraction is about 65%, similar as

z=1-3 ULIRGs, but little less than 80% for z=1-3 ULIRGs, but little less than 80% for SMGs)SMGs)

• QSOs and ellipticals appear at last stage of mergerQSOs and ellipticals appear at last stage of merger

• Some ULIRGs have extended soft X-ray halo based Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)on Chandra observations (e.g. NGC 6240, Mrk 273)

Z. Zheng, et al. 1999

The morphology of ULIRGs The morphology of ULIRGs

• Based on 97 HST snapshot images, we find that all Based on 97 HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectivelyare 43%, 39% and 18%, respectively

• The AGN fraction is 36%, 65% to 80% from single, The AGN fraction is 36%, 65% to 80% from single, double and multi-nucleus/nuclei double and multi-nucleus/nuclei

• QSOs and ellipticals appear at last stage of mergerQSOs and ellipticals appear at last stage of merger

• Some ULIRGs have extended soft X-ray halo based Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)on Chandra observations (e.g. NGC 6240, Mrk 273)

Huo et al. ApJ2004

Xia et al. 2002

Mrk273

108x80 kpc

NGC 6240 Huo et al. 2004

···

Ellipticals

Groups

ULIRGs

•Not all local ULIRGs will be sub-L* Not all local ULIRGs will be sub-L* ellipticalsellipticals

•Some ULIRGs may form from groupSome ULIRGs may form from group and will be massive ellipticalsand will be massive ellipticals

•Such case could be more at higher-zSuch case could be more at higher-z

This result is conflict with lower This result is conflict with lower metallicity in center of ULIRGs metallicity in center of ULIRGs based on optical analysisbased on optical analysis

“ “we find that LIRGs and ULIRGs are we find that LIRGs and ULIRGs are

underabundant by a factor of 2 on underabundant by a factor of 2 on average” by average” by Rupke et al.2008, ApJ, 674, 172 Rupke et al.2008, ApJ, 674, 172

Le Floc'h et al., 2006 Le Floc'h et al., 2006

Morphology of LIRGsMorphology of LIRGs

   Wang,  et al. 2006, ApJ, 649, 722Wang,  et al. 2006, ApJ, 649, 722

Based on SDSS DR2 Based on SDSS DR2 159159 images images

(R<15.9m and z<0.1)(R<15.9m and z<0.1)

Barred spiral

The morphology of LIRGsThe morphology of LIRGs

•The fractions of interacting/merging The fractions of interacting/merging and normal spirals are and normal spirals are 50% and 50% and 40%40%, respectively, respectively

•75%75% spirals are with strong bar spirals are with strong bar

Lir<4x10^11 Lsun

Wang et al. 2006, ApJ

Spirals

Interacting/merging

Infrared luminous QSOsInfrared luminous QSOs

QSOs with Lir>10^12MsunQSOs with Lir>10^12Msun

IR QSOs sampleIR QSOs sample

• QDOT IRAS galaxy sampleQDOT IRAS galaxy sample (Lawrence (Lawrence et al. 1999)et al. 1999)

• 1 Jy ULIRGs sample1 Jy ULIRGs sample (Kim & Sanders (Kim & Sanders 1998)1998)

• IRAS-ROSAT cross-identification IRAS-ROSAT cross-identification samplesample (Moran et al. 1996)(Moran et al. 1996)

A sample ofA sample of 31 31 IR QSOs IR QSOs

(z<0.35)(z<0.35) ，， takes a fraction of takes a fraction of about about 25%25% in local universe. in local universe.

Zheng, X.Z., 2002

Zheng, 2002

Hao, et al. 2005

●●○

PG QSOsIR QSOs

BH mass of ULIRGs is 10^7-10^8Msun

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)

Samples by Spitzer IRS

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

③③

Cao, et al. 2008

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

③③

③③

③③

SFR/MdotSFR/Mdot

③③

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

SFR/Mdot

•High-z SMGs are scaled up of High-z SMGs are scaled up of ULIRGsULIRGs

•Are high-z submm-loud QSOs Are high-z submm-loud QSOs are scaled up of IR QSOs?are scaled up of IR QSOs?

30% high-z QSOs detected at submm30% high-z QSOs detected at submm

High-z (sub)mm loud High-z (sub)mm loud QSOs QSOs 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)

Z=6Z=6Z=6

Carilli et al. 2007

Hao, et al. 2008

04.052.0

11)7.530.389(

yrM

MyrMSFR

sunsun

Molecular gas of IR QSOsMolecular gas of IR QSOs (Xia, Gao, Hao, Omont, Leon, Ocana, Tan and Tan and Mao)Mao)

Sample Sample

IR QSOs 20 IR QSOs 20 observed at 2008 fallobserved at 2008 fall

PG & HE QSOs 24PG & HE QSOs 24 ULIRGs 36ULIRGs 36 SMG 12SMG 12 submm-loud QSOs 15submm-loud QSOs 15

15/20 IR QSOs detected by IRAM 15/20 IR QSOs detected by IRAM 30m30m

1.35

1.22

• BH mass of ULIRGs and IR QSOs are 10^7 BH mass of ULIRGs and IR QSOs are 10^7

to 10^8 Msun and 10^7 to 10^9to 10^8 Msun and 10^7 to 10^9

• BH mass of SMG and submm loud QSOs BH mass of SMG and submm loud QSOs are <10^8 Msun and 10^9are <10^8 Msun and 10^9

• Molecular gas of ULIRGs and IR QSO Molecular gas of ULIRGs and IR QSO is similaris similar

• Molecular gas for SMG and submm Molecular gas for SMG and submm loud QSOs are similarloud QSOs are similar

BH mass of ULIRGs is 10^7-10^8Msun

IR QSOs and high-z (sub)mm loud IR QSOs and high-z (sub)mm loud QSOs are at stage with high SFR QSOs are at stage with high SFR and high accretion rateand high accretion rate

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

SpheriodsSpheriods

Thank you Thank you

SummarySummary• ULIRGs are interacting/merging pair or ULIRGs are interacting/merging pair or

group or galaxiesgroup or galaxies

• From ULIRGs to elliptical galaxies, there From ULIRGs to elliptical galaxies, there isis

a transition stage (IR QSOs), during which a transition stage (IR QSOs), during which both SFR and accration rate are highboth SFR and accration rate are high

• Feedback plays important role on Feedback plays important role on suppressing both starburst and AGNsuppressing both starburst and AGN

IR QSOs are in transition stage IR QSOs are in transition stage from starburst to QSOs from starburst to QSOs

• Strong FeII emitters and Balmar emission Strong FeII emitters and Balmar emission line blueshiftline blueshift

• Infrared excess from starburstInfrared excess from starburst

• PAH, NeII and L60 could be good indicators PAH, NeII and L60 could be good indicators of SFR for IR QSOsof SFR for IR QSOs

• High L60/Lco’ for both IR QSOs and high-z High L60/Lco’ for both IR QSOs and high-z sub-mm loud QSOs sub-mm loud QSOs

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

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

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

• The inclination of molecular disk of The inclination of molecular disk of ULIRGs and silicate absorption ULIRGs and silicate absorption correlates well– need more samplecorrelates well– need more sample

The morphology and environment The morphology and environment

of nearby ULIRGs and LIRGs of nearby ULIRGs and LIRGs• ULIRGs are interacting/merging galaxies ULIRGs are interacting/merging galaxies 

• ““An HST surface photometric study of An HST surface photometric study of ultraluminous infrared ultraluminous infrared galaxies”galaxies” ，， 1999,A&A,349,7351999,A&A,349,735 ，， Zheng, Z. et all.Zheng, Z. et all.

• “ “ IRAS 23532+2513: a compact group including a IRAS 23532+2513: a compact group including a Seyfert 1 and a starburst galaxy”Seyfert 1 and a starburst galaxy” ， ，  1995,A&A, 1995,A&A, 304,369304,369 ，， Zou, et al.Zou, et al.

• “ “ Statistical Properties of Ultraluminous IRAS Statistical Properties of Ultraluminous IRAS Galaxies from an HST Imaging Survey”Galaxies from an HST Imaging Survey” ， ，  2001, AJ, 2001, AJ, 122, 63122, 63 ，， Cui, J. et al.Cui, J. et al.

• ““Chandra Observations of Markarian 273: Chandra Observations of Markarian 273: Unveiling the Central Active Galactic Nucleus and Unveiling the Central Active Galactic Nucleus and the Extended Hot Gas Halo” the Extended Hot Gas Halo” 2002, ApJ, 564, 2002, ApJ, 564, 196196 ，， Xia, et al.Xia, et al.

黑洞质量与星系核球质量有很好的相关

T=41K, ß=1.95

Z=6Z=6Z=6

Carilli et al. 2007

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

· cluster

· group。ULIRGs

Xue &Wu 2001

· Ellipticals

O’Sullivan et al. 2003

Lx-T 关系（星系群，椭球星系和 ULIRGs）

· cluster

· group。ULIRGs

Xue &Wu 2001

IR QSOs are at IR QSOs are at transition statetransition state from ULIRGs to QSOs, then to from ULIRGs to QSOs, then to ellipticals, during which the SFR ellipticals, during which the SFR and accretion rate are higher and and accretion rate are higher and the relation of BH mass with the relation of BH mass with budge mass could be establishedbudge mass could be established

Infrared luminous QSOs (IR Infrared luminous QSOs (IR QSOs)QSOs)

• ““Spectroscopic Properties of QSOs Selected from Spectroscopic Properties of QSOs Selected from Ultraluminous Infrared Galaxy Samples”Ultraluminous Infrared Galaxy Samples” ，，

2002, AJ, 124, 182002, AJ, 124, 18 ，， Zheng, X. Z. et al.Zheng, X. Z. et al.

• ““The Physical Connections among Infrared QSOs, Palomar-The Physical Connections among Infrared QSOs, Palomar-Green QSOs, and Narrow-Line Seyfert 1 Galaxies”Green QSOs, and Narrow-Line Seyfert 1 Galaxies” ， ， 

2005, ApJ, 625, 782005, ApJ, 625, 78 ，， Hao, C.N.  et al.Hao, C.N.  et al.

• ““Growth of Black Holes and Their Host Spheroids in Growth of Black Holes and Their Host Spheroids in (Sub)mm-loud High-Redshift QSOs”(Sub)mm-loud High-Redshift QSOs” ，，

2008, ChJAA, 8, 122008, ChJAA, 8, 12 ，， Hao, C.N. et al.Hao, C.N. et al.

• ““Mid-Infrared spectroscopic properties of ultra-luminous Mid-Infrared spectroscopic properties of ultra-luminous infrared quasars”infrared quasars” ，，  

2008, MNRAS, 390, 336, Cao, C. et al.2008, MNRAS, 390, 336, Cao, C. et al.

The relation of spectral typeThe relation of spectral type with morphology with morphology

• Single nucleusSingle nucleus

• Double nucleiDouble nuclei

• Multi-nuclei AGN fractionMulti-nuclei AGN fraction

·cluster

·group。ULIRGs

Zheng, 2002

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

③③ ULIRGsULIRGs

IR QSOsIR QSOs

PG PG QSOsQSOs

29.0

118.588

yrM

M

yrM

SFR

sunsun

SFR

The morphology of ULIRGs The morphology of ULIRGs • ““The proportion of ultraluminous IRAS The proportion of ultraluminous IRAS

galaxies in interacting systems”galaxies in interacting systems” Zou, et al. ,1991,MNRAS,252,593Zou, et al. ,1991,MNRAS,252,593，，• ““A statistical study of the spectra of very A statistical study of the spectra of very

luminous IRAS galaxies. II. Spectral and luminous IRAS galaxies. II. Spectral and environmental analysis”environmental analysis”

Wu et al.1998,A&AS, 132,181, Wu et al.1998,A&AS, 132,181, • ““An HST surface photometric study of An HST surface photometric study of

ultraluminous infrared galaxies”ultraluminous infrared galaxies” ，， Zheng, Z. et al. 1999,A&A,349,735Zheng, Z. et al. 1999,A&A,349,735，，• “  “  Statistical Properties of Ultraluminous Statistical Properties of Ultraluminous

IRAS Galaxies from an HST Imaging IRAS Galaxies from an HST Imaging Survey”Survey”， ，             Cui, J. et al.Cui, J. et al. 2001, AJ, 122, 632001, AJ, 122, 63，，

The environment of ULIRGs The environment of ULIRGs

• “ “ IRAS 23532+2513: a compact group IRAS 23532+2513: a compact group including a Seyfert 1 and a starburst including a Seyfert 1 and a starburst galaxy”galaxy”，，              Zou, et al., 1995, A&A, 304,369Zou, et al., 1995, A&A, 304,369

• ““Chandra Observations of Markarian 273: Chandra Observations of Markarian 273: Unveiling the Central Active Galactic Unveiling the Central Active Galactic Nucleus and the Extended Hot Gas Halo” Nucleus and the Extended Hot Gas Halo”

Xia, et alXia, et al.. ,2002, ApJ, 564, 19 ,2002, ApJ, 564, 19

• ““Chandra Observations of Ultraluminous Chandra Observations of Ultraluminous Infrared Galaxies: Extended Hot Gaseous Infrared Galaxies: Extended Hot Gaseous Halos in Merging Galaxies”Halos in Merging Galaxies” ，，            Huo, et alHuo, et al. , . , 2004, ApJ, 611, 2082004, ApJ, 611, 208

barred barred spirals are the dominant spirals are the dominant population population above above LLIRIR=5x10=5x101010LL⊙⊙

IR luminosity functionIR luminosity function

“ “Infrared Galaxies in the nearby Universe” Infrared Galaxies in the nearby Universe” Wang, et al. 2008, ChJAA, in pressWang, et al. 2008, ChJAA, in press

1137 IR galaxies from SDSS DR5 1137 IR galaxies from SDSS DR5 (z<0.08 and r<15.9)(z<0.08 and r<15.9)

NormalNormal spirals are the dominant spirals are the dominant population below population below LLIRIR=8x10=8x101010LL⊙⊙

Infrared luminous QSOs (IR Infrared luminous QSOs (IR QSOs)QSOs)

• ““Spectroscopic Properties of QSOs Selected Spectroscopic Properties of QSOs Selected from Ultraluminous Infrared Galaxy Samples”from Ultraluminous Infrared Galaxy Samples”，，                          Zheng, X. Z. et al. 2002, AJ, 124, 18Zheng, X. Z. et al. 2002, AJ, 124, 18• ““The Physical Connections among Infrared The Physical Connections among Infrared

QSOs, Palomar-Green QSOs, and Narrow-Line QSOs, Palomar-Green QSOs, and Narrow-Line Seyfert 1 Galaxies”Seyfert 1 Galaxies”， ， 

Hao, C.N.  et al. 2005, ApJ, 625, 78Hao, C.N.  et al. 2005, ApJ, 625, 78• ““Mid-Infrared spectroscopic properties of ultra-Mid-Infrared spectroscopic properties of ultra-

luminous infrared quasars”luminous infrared quasars” ，，   Cao, C. et al. 2008, MNRAS, 390, 336Cao, C. et al. 2008, MNRAS, 390, 336• ““The moleculor gas of IR QSOs”The moleculor gas of IR QSOs” ，， Xia et al. in Xia et al. in

preparisonpreparison• “ “Growth of Black Holes and Their Host Growth of Black Holes and Their Host

Spheroids in (Sub)mm-loud High-Redshift QSOs”Spheroids in (Sub)mm-loud High-Redshift QSOs”，， Hao, C.N. et al. 2008, ChJAA, 8, 12Hao, C.N. et al. 2008, ChJAA, 8, 12

•IR QSOs are at IR QSOs are at transition statetransition state from mergers to classicals from mergers to classicals QSOs then to ellipticalsQSOs then to ellipticals

•IR QSOs are with high SFR and IR QSOs are with high SFR and high accretion ratehigh accretion rate

BH mass of ULIRGs is 10^7-10^8Msun