1. 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

2. 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

3. 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)

4. Cui et al. 2002

6. 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% % %
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)

7. Z. Zheng, et al. 1999

8. 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)

9. Huo et al. ApJ
2004

10. Mrk273
108x80 kpc
Xia et al. 2002

11. NGC 6240
Huo et al. 2004

12. ··
Ellipticals
Groups
ULIRGs

13. 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

16. 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

17. Le Floc'h et al., 2006

18. 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)

20. Barred spiral

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

22. Lir<4x10^11 Lsun

23. Interacting/merging
Spirals
Wang et al. 2006, ApJ

24. Infrared luminous QSOs
QSOs with Lir>10^12Msun

25. 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.

26. Zheng, X.Z., 2002

27. Zheng, 2002

29. ●
PG QSOs
IR QSOs ○
Hao, et al. 2005

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

33. 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< PG QSOs from QUEST (Schweitzer et al. 2006)

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

36. ③
Fine structure line [NeII] 12.81m
 SFR indicator in QSOs

37. ③

38. ③

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

40. 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

41. 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)

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

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

45. 15/20 IR QSOs detected by IRAM 30m

51. 1.35
1.22

57. 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

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

59. 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

60. Thank you

61. 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

62. 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

68. 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

69. 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

80. 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

81. 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 : 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.

84. T=41K, ß=1.95

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

86. 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 )

87. cluster
group 。
ULIRGs
Xue &Wu 2001

88. Ellipticals
O’Sullivan et al. 2003

89. Lx-T 关系（星系群，椭球星系和ULIRGs）

90. cluster
group 。
ULIRGs
Xue &Wu 2001

92. 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

93. 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.

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

99. cluster
group 。
ULIRGs

101. Zheng, 2002

104. 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)

105. ULIRGs IR QSOs PG QSOs ③

106. SFR

112. 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，

113. The environment of ULIRGs
“ IRAS : 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

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

115. 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⊙

116. 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

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

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