from ulirgs to qsos from ulirgs to qsos xiaoyang, xia xiaoyang, xia center for astrophysics center...
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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)
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)
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)
•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
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)
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
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.
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
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)
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
• 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
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
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.
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
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
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
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