From ULIRGs to QSOs XiaoYang, Xia Center for Astrophysics Tianjin Normal University Collaborators: H. Wu, Deng, Zou, Z. Zheng, Mao, X.Z. Zheng, Hao, Huo, Y. Gao, Wang,J.L, Tan

Infrared luminous QSOs may give hint on high-z submm loud QSOs Outline The morphology and environment of ULIRGs and LIRGs May give hint for high-z SMGs Infrared luminous QSOs may give hint on high-z submm loud QSOs Then the relation of ULIRGs with SMGs and IR QSOs with submm loud QSOs

The morphology of ULIRGs Based on 97 HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively The AGN fraction is 80%, 65% to 36% from single, double and multi-nucleus/nuclei QSOs and ellipticals appear at last stage of merger Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

Cui et al. 2002

The morphology of ULIRGs All ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively, based on 97 HST snapshot images. The AGN fractions are 80% 65% 36% single double multi nucleus/nuclei (total AGN fraction is about 65%, similar as z=1-3 ULIRGs, but little less than 80% for SMGs) QSOs and ellipticals appear at last stage of merger Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

Z. Zheng, et al. 1999

The morphology of ULIRGs Based on 97 HST snapshot images, we find that all ULIRGs are interacting/merging galaxies and the fractions of single, double and multi-nucleus/nuclei are 43%, 39% and 18%, respectively The AGN fraction is 36%, 65% to 80% from single, double and multi-nucleus/nuclei QSOs and ellipticals appear at last stage of merger Some ULIRGs have extended soft X-ray halo based on Chandra observations (e.g. NGC 6240, Mrk 273)

Huo et al. ApJ 2004

Mrk273 108x80 kpc Xia et al. 2002

NGC 6240 Huo et al. 2004

·· · Ellipticals Groups ULIRGs

Not all local ULIRGs will be sub-L* ellipticals Some ULIRGs may form from group and will be massive ellipticals Such case could be more at higher-z

This result is conflict with lower metallicity in center of ULIRGs based on optical analysis “we find that LIRGs and ULIRGs are underabundant by a factor of 2 on average” by Rupke et al.2008, ApJ, 674, 172

Le Floc'h et al., 2006

Morphology of LIRGs Based on SDSS DR2 159 images   Wang,  et al. 2006, ApJ, 649, 722 Based on SDSS DR2 159 images (R<15.9m and z<0.1)

Barred spiral

The morphology of LIRGs The fractions of interacting/merging and normal spirals are 50% and 40%, respectively 75% spirals are with strong bar

Lir<4x10^11 Lsun

Interacting/merging Spirals Wang et al. 2006, ApJ

Infrared luminous QSOs QSOs with Lir>10^12Msun

IR QSOs 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.

Zheng, X.Z., 2002

Zheng, 2002

● PG QSOs IR QSOs ○ Hao, et al. 2005

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

Samples by Spitzer IRS 19 IR QSOs 35 ULIRGs 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<0.27 + PG QSOs from QUEST (Schweitzer et al. 2006)

The low resolution mid-infrared spectra of IR QSOs ③ Cao, et al. 2008

③ Fine structure line [NeII] 12.81m  SFR indicator in QSOs

③

③

③ Feedback may play role to suppress both star formation and AGN SFR/Mdot SFR/Mdot Anti-correlated H blueshift

High-z SMGs are scaled up of ULIRGs Are high-z submm-loud QSOs are scaled up of IR QSOs? 30% high-z QSOs detected at submm

High-z (sub)mm loud QSOs 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)

Carilli et al. 2007 Z=6 Z=6 Z=6 Hao, et al. 2008

Molecular gas of IR QSOs (Xia, Gao, Hao, Omont, Leon, Ocana, Tan and Mao) Sample IR QSOs 20 observed at 2008 fall PG & HE QSOs 24 ULIRGs 36 SMG 12 submm-loud QSOs 15

15/20 IR QSOs detected by IRAM 30m

1.35 1.22

Molecular gas of ULIRGs and IR QSO is similar BH mass of ULIRGs and IR QSOs are 10^7 to 10^8 Msun and 10^7 to 10^9 BH mass of SMG and submm loud QSOs are <10^8 Msun and 10^9 Molecular gas of ULIRGs and IR QSO is similar Molecular gas for SMG and submm loud QSOs are similar

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

The Coeval Growth of Black Holes and their host Spheriods IR QSOs and high-z (sub)mm loud QSOs are at stage with high SFR and high accretion rate The Coeval Growth of Black Holes and their host Spheriods

Thank you

Summary ULIRGs are interacting/merging pair or group or galaxies From ULIRGs to elliptical galaxies, there is a transition stage (IR QSOs), during which both SFR and accration rate are high Feedback plays important role on suppressing both starburst and AGN

IR QSOs are in transition stage from starburst to QSOs Strong FeII emitters and Balmar emission line blueshift Infrared excess from starburst PAH, NeII and L60 could be good indicators of SFR for IR QSOs High L60/Lco’ for both IR QSOs and high-z sub-mm loud QSOs

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

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

Summary Mid-IR to Far-IR slop reflects the relative contribution from central AGN and SF NeII is a good indicator for SFR The inclination of molecular disk of ULIRGs and silicate absorption correlates well– need more sample

The morphology and environment of nearby ULIRGs and LIRGs ULIRGs are interacting/merging galaxies  “An HST surface photometric study of ultraluminous infrared galaxies”，1999,A&A,349,735，Zheng, Z. et all. “ IRAS 23532+2513: a compact group including a Seyfert 1 and a starburst galaxy”， 1995,A&A, 304,369，Zou, et al. “ Statistical Properties of Ultraluminous IRAS Galaxies from an HST Imaging Survey”， 2001, AJ, 122, 63， Cui, J. et al. “Chandra Observations of Markarian 273: Unveiling the Central Active Galactic Nucleus and the Extended Hot Gas Halo” 2002, ApJ, 564, 196，Xia, et al.

T=41K, ß=1.95

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

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 )

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

Infrared luminous QSOs (IR QSOs) “Spectroscopic Properties of QSOs Selected from Ultraluminous Infrared Galaxy Samples”， 2002, AJ, 124, 18，Zheng, X. Z. et al. “The Physical Connections among Infrared QSOs, Palomar-Green QSOs, and Narrow-Line Seyfert 1 Galaxies”， 2005, ApJ, 625, 78，Hao, C.N.  et al. “Growth of Black Holes and Their Host Spheroids in (Sub)mm-loud High-Redshift QSOs”， 2008, ChJAA, 8, 12，Hao, C.N. et al. “Mid-Infrared spectroscopic properties of ultra-luminous infrared quasars”，  2008, MNRAS, 390, 336, Cao, C. et al.

The relation of spectral type with morphology Single nucleus Double nuclei Multi-nuclei AGN fraction

· cluster · group 。 ULIRGs

Zheng, 2002

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)

ULIRGs IR QSOs PG QSOs ③

SFR

The morphology of ULIRGs “The proportion of ultraluminous IRAS galaxies in interacting systems” Zou, et al. ,1991,MNRAS,252,593， “A statistical study of the spectra of very luminous IRAS galaxies. II. Spectral and environmental analysis” Wu et al.1998,A&AS, 132,181, “An HST surface photometric study of ultraluminous infrared galaxies”， Zheng, Z. et al. 1999,A&A,349,735， “  Statistical Properties of Ultraluminous IRAS Galaxies from an HST Imaging Survey”，  Cui, J. et al. 2001, AJ, 122, 63，

The environment of ULIRGs “ IRAS 23532+2513: a compact group including a Seyfert 1 and a starburst galaxy”，  Zou, et al., 1995, A&A, 304,369 “Chandra Observations of Markarian 273: Unveiling the Central Active Galactic Nucleus and the Extended Hot Gas Halo” Xia, et al. ,2002, ApJ, 564, 19 “Chandra Observations of Ultraluminous Infrared Galaxies: Extended Hot Gaseous Halos in Merging Galaxies”， Huo, et al. , 2004, ApJ, 611, 208

barred spirals are the dominant population above LIR=5x1010L⊙

IR luminosity function “Infrared Galaxies in the nearby Universe” Wang, et al. 2008, ChJAA, in press 1137 IR galaxies from SDSS DR5 (z<0.08 and r<15.9) Normal spirals are the dominant population below LIR=8x1010L⊙

Infrared luminous QSOs (IR QSOs) “Spectroscopic Properties of QSOs Selected from Ultraluminous Infrared Galaxy Samples”， Zheng, X. Z. et al. 2002, AJ, 124, 18 “The Physical Connections among Infrared QSOs, Palomar-Green QSOs, and Narrow-Line Seyfert 1 Galaxies”， Hao, C.N.  et al. 2005, ApJ, 625, 78 “Mid-Infrared spectroscopic properties of ultra-luminous infrared quasars”，  Cao, C. et al. 2008, MNRAS, 390, 336 “The moleculor gas of IR QSOs”， Xia et al. in preparison “Growth of Black Holes and Their Host Spheroids in (Sub)mm-loud High-Redshift QSOs”， Hao, C.N. et al. 2008, ChJAA, 8, 12

IR QSOs are at transition state from mergers to classicals QSOs then to ellipticals IR QSOs are with high SFR and high accretion rate

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